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%% C.T V2.1 8 Juin 1992                                                         
%% F.A V2.2 9 Juin 1992                                                         
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\message{           Hipparcos Input Catalogue (ESA SP-1136) }                   
\message{          Copyright (C) 1992, European Space Agency}                   
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\begin{document}                                                                
\pagenumbering{roman}                                                           
                                                                                
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% Front pages                                                                   
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\vspace*{-2 cm}                                                                 
                                                                                
                                                                                
\vspace{3.0 cm}                                                                 
\CENTER{\LARGE\it THE HIPPARCOS INPUT CATALOGUE}                                
\vspace{1 cm}                                                                   
\CENTER{\it A publication of the INCA Consortium}                               
\vspace{2 cm}                                                                   
\CENTER{\large C. Turon\UPNOTE{1},\\                                            
M. Cr\'ez\'e\UPNOTE{2}, D. Egret\UPNOTE{2}, A. G\'omez\UPNOTE{2},               
M. Grenon\UPNOTE{2}, H. Jahrei\ss\UPNOTE{2}, Y. R\'equi\`eme\UPNOTE{2},\\       
A.N. Argue\UPNOTE{3}, A. Bec-Borsenberger\UPNOTE{3}, J. Dommanget\UPNOTE{3},    
M.O. Mennessier\UPNOTE{3},\\                                                    
F. Arenou, M. Chareton, F. Crifo, J.C. Mermilliod\UPNOTE{4},\\                  
D. Morin, B. Nicolet, O. Nys, L. Pr\'evot\UPNOTE{4}, M. Rousseau,\\             
M.A.C. Perryman\UPNOTE{5}\\}                                                    
                                                                                
\medskip                                                                        
\CENTER{\normalsize\it and}                                                     
                                                                                
\CENTER{\normalsize J.E. Arlot, A. Baglin, D. Barth\`es, M.O. Baylac,           
P. Brosche, M. Burnet,\\                                                        
J. Delhaye, C. Dettbarn, M. Erbach, F. Figueras, W. Fricke\dag,                 
L. Helmer, P. Hemenway,\\                                                       
C. Jordi, P. Lampens, T. Lederle, J. Lub, J. Manfroid, J.A.                     
Mattei, J.M. Mazurier,\\                                                        
M. Mermilliod, L.V. Morrison, C.A. Murray, E. Oblak, J.P. P\'eri\'e, B.         
Pernier,  R.S. Le Poole,\\                                                      
L. Quijano, M. Rapaport, A. Sellier, J. Torra, H.-J. Tucholke, C. de Vegt}      
                                                                                
\medskip                                                                        
\CENTER{\footnotesize\it with contributions from}                               
                                                                                
\CENTER{\footnotesize R.W. Argyle, P. Bacchus, N. Baron, J. Calaf, J.P          
Cordoni, C. Fabricius, J.C. Feaugas, H.J. Fehlberg,\\                           
D.R. Florkowski, E. de Geus, P. Gibbs, L. Hartman, D.L. Jauncey, K.J.           
Johnston, M. Marouard, A. Mekkas,\\                                             
J.L. Mui\~nos, J. N\'u\~nez, F. Ochsenbein, J.J. de Or\'us, J.M. Paredes,       
M.J. Penston, C. Petersen, Y. Peyrin,\\                                         
A. Robin, V. Roman, G. Rossell\'o, H. Schwan, D. Sinachopoulos,                 
G.L. White, N. Zacharias\\}                                                     
                                                                                
\medskip                                                                        
\CENTER{\normalsize\it and\\                                                    
(interfaces with the data reduction and satellite activities)}                  
                                                                                
\CENTER{\normalsize E. H{\o}g, J. Kovalevsky, F. van Leeuwen, L. Lindegren, A.  
Sch\"utz, H. Schrijver}                                                         
                                                                                
\bigskip                                                                        
{\small\noindent                                                                
\UPNOTE{1}~Leader of the INCA Consortium\\                                      
\UPNOTE{2}~Responsible for specific activities within the INCA Consortium\\     
\UPNOTE{3}~Coordinators of `Working Groups' within the INCA Consortium\\        
\UPNOTE{4}~Responsible for the selection of stars in special areas\\            
\UPNOTE{5}~Hipparcos Project Scientist}                                         
                                                                                
\vfill                                                                          
                                                                                
\bigskip                                                                        
\CENTER{\LARGE\bf The INCA Consortium}                                          
\eject                                                                          
                                                                                
\noindent                                                                       
The production of the Hipparcos Input Catalogue has also                        
benefited from the participation of:                                            
                                                                                
\medskip\noindent                                                               
J.P. Anosova, M. Auvergne, R. Barbier, P. Bartholdi, U. Bastian,                
C.J.~Benn, J.F.~Bopp, F. Bosq,\\                                                
H. Boughaleb, J. Bourgeois, M.T. Bridgeland, J.W. de~Bruyn, P.S. Bunclark, G.   
Burki,\\                                                                        
J.P.~Busset, O.~Caceres\dag, J.E.~Le~Campion, M.P. Candy, M.A.~Catal\`a,        
R.~Coll, N.~Cramer, \\                                                          
J. Cuypers, J.~Doyle, R.L.~Duncombe, R.~Estalella, P.                           
Figon, O.~Franz, M.T. Gachard,\\                                                
M.~Geffert, S. Grenier, J. Guibert, R.T. Harmon, H.~Hensberge, M.J. Irwin,      
P.~Jenniskens,\\                                                                
A. Jorissen, S.M. Kazeza, C.~Kint, A.R.~Klemola, J.P. Koninx,                   
H.J. van Langevelde, A. L\`ebre,\\                                              
G.~Leonis, J.F.~Lestrade, L. Louys, C. Ma, M.~Mayor, H.~McAlister,              
B.~McLean, G.~Montignac,\\                                                      
B. Morgan, W.~Nicholson, D.S. Nithakorn, V.V.~Orlov,                            
R.~Pannunzio, T.~Pauwels, L. Perdomo,\\                                         
C. Petersen, N.~Ralite, E. Rebeirot,                                            
S.~Rousseau, C. Ruatti, G. Ruben, F. Rufener,\\                                 
F.~Sala, M.~Saltel, D.~Scales,                                                  
M.~Scardia, L. Schmadel, E. Schmeidler, H.~Scholl, C.~Smith,\\                  
G. Souli\'e, M.~Tellechea, H.G. Walter, M. Wenger, R.~Wielen, C.E.~Worley       
                                                                                
\bigskip                                                                        
\bigskip\noindent                                                               
the permanent and constructive support of the Hipparcos Science                 
Team:                                                                           
                                                                                
\medskip\noindent                                                               
P.L. Bernacca, M.~Cr\'ez\'e, F.~Donati, M. Grenon, M. Grewing, E. H{\o}g, \\    
J. Kovalevsky, F. van Leeuwen, L. Lindegren, H. van der Marel, C.A. Murray, \\  
M.A.C. Perryman ({\it Chairman}), R.S. Le Poole, H. Schrijver, C. Turon         
                                                                                
\bigskip                                                                        
\bigskip\noindent                                                               
and of the ESOC team dealing with all catalogue and                             
observation monitoring aspects:                                                 
                                                                                
\medskip\noindent                                                               
P.E. Davies, A.J.C. McDonald, A. Sch\"utz                                       
                                                                                
\bigskip                                                                        
\bigskip\noindent                                                               
and the advice of the Programme Selection Committee:                            
                                                                                
\medskip\noindent                                                               
A. Blaauw ({\it Chairman}), J. Dommanget, W. Gliese, M. Hack, E.P.J.            
van den Heuvel, \\                                                              
C. Jaschek, J.~Lequeux, P.O. Lindblad, A. Maeder,                               
P.E. Nissen, B.E.J. Pagel, \\                                                   
A. Renzini, C. de Vegt, P.A. Wayman, R.~Wielen                                  
                                                                                
\vfill                                                                          
                                                                                
                                                                                
\noindent                                                                       
\copyright 1992 ~European Space Agency                                          
                                                                                
\bigskip                                                                        
\bigskip                                                                        
\noindent                                                                       
Questions or comments should be sent to                                         
                                                                                
\medskip\noindent                                                               
Catherine Turon, \\                                                             
Observatoire de Paris-Meudon, \\                                                
92195 Meudon Cedex, France.                                                     
\eject                                                                          
                                                                                
\CENTER{\Large\bf Support of the INCA Consortium}                               
                                                                                
\medskip                                                                        
\CENTER{The work of the INCA Consortium has been supported by                   
the funding authorities of each of the main participating                       
institutes in its respective country:}                                          
                                                                                
                                                                                
\bigskip                                                                        
{\bf Australia}                                                                 
\begin{itemize}\itemsep=-4pt                                                    
 \item Commonwealth Scientific and Industrial Research Organisation (CSIRO),    
 \item Australian National Research Fellowship Scheme.                          
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf Belgium}                                                                   
\begin{itemize}\itemsep=-4pt                                                    
 \item Minist\`ere de l'Education Nationale/Ministerie                          
 van Nationale Opvoeding,                                                       
 \item Fonds de la Recherche Fondamentale Collective (Bruxelles),               
 \item Fonds National de la Recherche Scientifique,                             
 \item Commission des Communaut\'es Europ\'eennes.                              
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf Denmark}                                                                   
\begin{itemize}\itemsep=-4pt                                                    
 \item Danish Space Board,                                                      
 \item Danish Natural Science Research Council,                                 
 \item Carlsberg Foundation.                                                    
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf France}                                                                    
\begin{itemize}\itemsep=-4pt                                                    
 \item Centre National de la Recherche Scientifique - Institut                  
       National des Sciences de l'Univers,                                      
 \item Centre National d'Etudes Spatiales,                                      
 \item Minist\`ere de l'Education Nationale, de la Jeunesse et des Sports,      
 \item Minist\`ere de la Recherche et de la Technologie,                        
 \item Minist\`ere des Affaires Etrang\`eres,                                   
 \item R\'egion Languedoc-Roussillon,                                           
 \item D\'el\'egation G\'en\'erale \`a l'Espace.                                
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf Germany}                                                                   
\begin{itemize}\itemsep=-4pt                                                    
 \item Ministerium f\"ur Wissenschaft und Kunst, Baden-W\"urttemberg,           
 \item Bundesministerium f\"ur Forschung und Technologie.                       
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf The Netherlands}                                                           
\begin{itemize}\itemsep=-4pt                                                    
 \item Sterrewacht Leiden, Leiden University.                                   
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf Spain}                                                                     
\begin{itemize}\itemsep=-4pt                                                    
 \item Comisi\'on Interministerial de Ciencia y Tecnolog\'{\i}a,                
 \item Comissi\'o Interdepartamental de Recerca i Innovaci\'o Tecnol\`ogica,    
 \item Estado Mayor de la Armada. Ministerio de Defensa,                        
 \item Direcci\'on General de Investigaci\'on Cient\'{\i}fica y T\'ecnica.      
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf Switzerland}                                                               
\begin{itemize}\itemsep=-4pt                                                    
 \item Universit\'e de Gen\`eve,                                                
 \item Universit\'e de Lausanne,                                                
 \item Fonds National Suisse de la Recherche Scientifique.                      
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf United Kingdom}                                                            
\begin{itemize}\itemsep=-4pt                                                    
 \item Science and Engineering Research Council,                                
 \item University of Cambridge.                                                 
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf USA}                                                                       
\begin{itemize}\itemsep=-4pt                                                    
 \item University of Texas,                                                     
 \item NASA.                                                                    
\end{itemize}                                                                   
                                                                                
%                                                                               
\vfill\eject                                                                    
%                                                                               
                                                                                
\CENTER{\Large\bf Main Institutes Participating in the INCA Consortium}         
                                                                                
\medskip                                                                        
\par {\bf Australia}                                                            
\begin{itemize}\itemsep=-4pt                                                    
 \item Australia Telescope National Facility, CSIRO, Epping,                    
 \item Perth Observatory.                                                       
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf Belgium}                                                                   
\begin{itemize}\itemsep=-4pt                                                    
 \item Observatoire Royal de Belgique,                                          
       Bruxelles/Koninklijke Sterrenwacht van Belgi\"e,                         
 \item Institut d'Astrophysique de l'Universit\'e de Li\`ege. \par              
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf Denmark}                                                                   
\begin{itemize}\itemsep=-4pt                                                    
 \item Astronomisk Observatorium, Brorfelde,                                    
 \item Astronomisk Observatorium, K{\o}benhavn.                                 
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf France}                                                                    
\begin{itemize}\itemsep=-4pt                                                    
 \item Bureau des Longitudes,                                                   
 \item Observatoire de Besan\c{c}on,                                            
 \item Observatoire de Bordeaux,                                                
 \item Observatoire de Paris-Meudon,                                            
 \item Centre de Donn\'ees astronomiques de Strasbourg,                         
       Observatoire de Strasbourg,                                              
 \item Equipe d'Astrophysique, Universit\'e des Sciences et Techniques du       
       Languedoc, Montpellier,                                                  
 \item Centre National d'Etudes Spatiales, Toulouse.                            
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf Germany}                                                                   
\begin{itemize}\itemsep=-4pt                                                    
 \item Astronomisches Rechen-Institut, Heidelberg,                              
 \item Astronomisches Institut, Universit\"at M\"unster,                        
 \item Hamburger Sternwarte, Hamburg,                                           
 \item Institut f\"ur Astronomie, Universit\"at M\"unchen,                      
 \item Universit\"ats-Sternwarte Bonn, Daun.                                    
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf The Netherlands}                                                           
\begin{itemize}\itemsep=-4pt                                                    
 \item Sterrewacht Leiden.                                                      
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf Spain}                                                                     
\begin{itemize}\itemsep=-4pt                                                    
 \item Real Instituto y Observatorio de la Armada, San Fernando,                
 \item Universitat de Barcelona.                                                
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf Switzerland}                                                               
\begin{itemize}\itemsep=-4pt                                                    
 \item Observatoire de Gen\`eve,                                                
 \item Institut d'Astronomie de Lausanne.                                       
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf United Kingdom}                                                            
\begin{itemize}\itemsep=-4pt                                                    
 \item Royal Greenwich Observatory, Cambridge,                                  
 \item Institute of Astronomy, Cambridge.                                       
\end{itemize}                                                                   
                                                                                
                                                                                
{\bf USA}                                                                       
\begin{itemize}\itemsep=-4pt                                                    
 \item AAVSO,                                                                   
 \item Jet Propulsion Laboratory, Pasadena California,                          
 \item Naval Research Laboratory, Washington D.C.,                              
 \item University of Texas, Austin, Texas,                                      
 \item U.S. Naval Observatory, Washington D.C.                                  
\end{itemize}                                                                   
                                                                                
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%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\huge\bf Contents}                                                      
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
                                                                                
                                                                                
{\bf Introduction} \dotfill\ 1                                                  
\begin{itemize}\itemsep=-4pt                                                    
 \item The Hipparcos Input Catalogue \dotfill\ 1                                
 \item The Hipparcos mission \dotfill\ 1                                        
 \item The INCA Consortium (Input Catalogue Consortium) \dotfill\ 2             
 \item The Hipparcos observing programme \dotfill\ 2                            
 \item Contents of this publication \dotfill\ 3                                 
 \item References \dotfill\ 3                                                   
\end{itemize}                                                                   
                                                                                
{\bf Star Selection} \dotfill\ 5                                                
                                                                                
\bigskip                                                                        
{\bf Main Catalogue} \dotfill\ 7                                                
\begin{itemize}\itemsep=-4pt                                                    
 \item Fields \makebox[2cm][l]{~\,1-3} Hipparcos Input Catalogue (HIC)          
                                   Identification \dotfill\ 8                   
 \item Fields \makebox[2cm][l]{~\,4-11} Position (Equinox J2000.0) \dotfill\ 11 
 \item Fields \makebox[2cm][l]{12-15} Other coordinates \dotfill\ 14            
 \item Fields \makebox[2cm][l]{16-19} Position (Equinox B1950.0) \dotfill\ 15   
 \item Fields \makebox[2cm][l]{20-24} Proper Motion \dotfill\ 15                
 \item Fields \makebox[2cm][l]{25-31} Photometry \dotfill\ 16                   
 \item Fields \makebox[2cm][l]{32-33} Spectral Type \dotfill\ 19                
 \item Fields \makebox[2cm][l]{34-36} Parallax \dotfill\ 21                     
 \item Fields \makebox[2cm][l]{37-38} Radial Velocity \dotfill\ 21              
 \item Fields \makebox[2cm][l]{39-44} Variability \dotfill\ 22                  
 \item Fields \makebox[2cm][l]{45-50} Multiplicity \dotfill\ 25                 
 \item Fields \makebox[2cm][l]{51-60} Identifications \dotfill\ 26              
 \item Field~ \makebox[2cm][l]{61} Miscellaneous Information \dotfill\ 29       
 \item Catalogue Abbreviations \dotfill\ 32                                     
 \item References \dotfill\ 33                                                  
 \item Notes \dotfill\ 37                                                       
                                                                                
\end{itemize}                                                                   
                                                                                
                                                                                
\bigskip                                                                        
{\bf Annex 1: Components of Double and Multiple Systems} \dotfill\ 44           
                                                                                
\begin{itemize}\itemsep=-4pt                                                    
 \item Annex 1 \dotfill\ 45                                                     
 \item Catalogue of Components of Double and Multiple Stars \dotfill\ 45        
 \item Fields \makebox[2cm][l]{~\,1-3} Component Identification \dotfill\ 46    
 \item Fields \makebox[2cm][l]{~\,4-5} Position (Equinox J2000.0) \dotfill\ 46  
 \item Field~ \makebox[2cm][l]{~~\,\,6} Photometry \dotfill\ 47                 
 \item Fields \makebox[2cm][l]{~\,7-10} System Geometry \dotfill\ 47            
 \item Fields \makebox[2cm][l]{11-12} Proper Motion \dotfill\ 48                
 \item Fields \makebox[2cm][l]{13-19} Cross-Identifications \dotfill\ 48        
 \item Acknowledgements \dotfill\ 49                                            
 \item References \dotfill\ 49                                                  
\end{itemize}                                                                   
                                                                                
\bigskip                                                                        
{\bf The INCA Consortium} \dotfill\ 50                                          
\begin{itemize}\itemsep=-4pt                                                    
 \item Executive and Steering Committees of the INCA Consortium \dotfill\ 50    
 \item Members of the INCA Consortium \dotfill\ 51                              
\end{itemize}                                                                   
                                                                                
{\bf The Proposals} \dotfill\ 59                                                
\begin{itemize}\itemsep=-4pt                                                    
 \item The ESA Hipparcos Scientific Selection Committee \dotfill\ 59            
 \item Scientific Proposals received by ESA \dotfill\ 60                        
\end{itemize}                                                                   
                                                                                
{\bf Acknowledgements} \dotfill\ 65                                             
                                                                                
                                                                                
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%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\huge\bf List of Tables}                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
\bigskip                                                                        
\bigskip                                                                        
\bigskip                                                                        
                                                                                
\makebox[3cm][l]{Table A1} HIC numbers of objects suppressed from the Input     
                                 Catalogue \dotfill\ 9                          
                                                                                
\makebox[3cm][l]{Table A2/1} Supplementary HIC numbers - ordered by running     
                                  number  \dotfill\ 10                          
                                                                                
\makebox[3cm][l]{Table A2/2} Supplementary HIC numbers - ordered by right       
                                  ascension  \dotfill\ 10                       
                                                                                
\makebox[3cm][l]{Table A3} Solar system objects observed by Hipparcos           
                                  \dotfill\ 31                                  
                                                                                
                                                                                
\bigskip                                                                        
                                                                                
\makebox[3cm][l]{Table B1} Source of positions and proper motions  \dotfill\ 13 
                                                                                
\makebox[3cm][l]{Table B2} Source of photometry  \dotfill\ 18                   
                                                                                
\makebox[3cm][l]{Table B3} Source of spectral types  \dotfill\ 20               
                                                                                
\makebox[3cm][l]{Table B4} Source of radial velocities  \dotfill\ 22            
                                                                                
\makebox[3cm][l]{Table B5} Galactic open clusters: names and abbreviations      
                                          \dotfill\ 30                          
                                                                                
\bigskip                                                                        
                                                                                
\makebox[3cm][l]{Table V1} Variability code  \dotfill\ 17                       
                                                                                
\makebox[3cm][l]{Table V2} Types of variability  \dotfill\ 23                   
                                                                                
\makebox[3cm][l]{Table V3} Coded error of the $V$ magnitudes  \dotfill\ 24      
                                                                                
\makebox[3cm][l]{Table V4} Magnitudes and colours given in fields 25, 27, 29    
                                   \dotfill\ 25                                 
                                                                                
\bigskip                                                                        
                                                                                
\makebox[3cm][l]{Table I1} FK4-FK5, IRS catalogues  \dotfill\ 27                
                                                                                
\makebox[3cm][l]{Table I2} AGK3-CPC catalogues  \dotfill\ 27                    
                                                                                
\makebox[3cm][l]{Table I3} Abbreviations and format of catalogues used in       
                        fields 58 and 59  \dotfill\  28                         
                                                                                
\makebox[3cm][l]{Table I4} Identifiers in the Magellanic                        
                      Clouds  \dotfill\  28                                     
                                                                                
\makebox[3cm][l]{Table I5} Other identifiers  \dotfill\ 29                      
                                                                                
\bigskip                                                                        
                                                                                
\makebox[3cm][l]{Table Annex} Ephemerides for three orbital pairs               
                      \dotfill\ 47                                              
                                                                                
                                                                                
                                                                                
\bigskip                                                                        
\bigskip                                                                        
                                                                                
                                                                                
\CENTER{Tables A1-A3 and B1-B5 are as referenced in the printed version         
 (ESA SP-1136)}                                                                 
                                                                                
                                                                                
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%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\huge\bf Introduction}                                                  
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\pagenumbering{arabic}                                                          
                                                                                
\bigskip                                                                        
\bigskip                                                                        
\bigskip                                                                        
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{The Hipparcos Input Catalogue}                                        
%-------------------------------------------------                              
                                                                                
The Hipparcos Input Catalogue was constructed as the                            
observing programme for the European Space Agency's Hipparcos                   
astrometry mission. The requirements of the project in terms of                 
completeness, sky coverage, astrometric and photometric accuracy, as            
well as the necessary optimisation of the scientific impact, resulted           
in an extended effort to compile and homogenize existing data, to               
clarify sources and identifications and, where needed, to collect new           
data matching the required accuracy.                                            
                                                                                
\medskip                                                                        
This has resulted in an unprecedented catalogue of stellar data                 
including up-to-date information on positions, proper motions,                  
magnitudes and colours, and (whenever available) spectral types, radial         
velocities, multiplicity and variability information.  The catalogue is         
complete to well-defined magnitude limits, and includes a substantial           
sampling of the most important stellar categories present in the solar          
neighbourhood beyond these limits. As explained below, the magnitude            
limits vary from 7.3 to 9 mag as a function of galactic latitude and            
spectral type, and there are no stars fainter than about $V=13$ mag.            
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{The Hipparcos mission}                                                
%-------------------------------------------------                              
                                                                                
Overviews of the European Space Agency's Hipparcos                              
astrometry mission, its history, scientific objectives and observing            
programme, the payload design, and plans for the satellite operations           
and data reductions, have been given frequently before the satellite            
launch. The most comprehensive description of the satellite, observing          
programme, and methods foreseen for the data reduction are contained in         
a 3-volume ESA publication, ESA SP-1111 (Perryman \ETAL\ 1989). The             
project was accepted within ESA's mandatory scientific programme in             
1980, with a planned operational lifetime of 2.5 years. The goal of the         
Hipparcos project was to measure the astrometric parameters of about            
100\,000 stars with an accuracy of some 2-4 milli-arcsec (depending on          
magnitude) for the main mission and, as subsequently incorporated               
during the design phase, the astrometric and two-colour photometric             
properties of a further minimum of some 400\,000 or more stars with             
somewhat lower accuracy for the Tycho experiment. By placing the                
observing platform above the perturbing atmosphere, and exploiting the          
all-sky visibility and freedom from gravitational flexure and thermal           
fluctuations, differential angular measurements are built up over large         
angles, at many different orientations and at many different epochs.            
>From these measurements, relative positions, annual proper motions and         
absolute parallaxes, free from regional or systematic errors at the             
milli-arcsec level, can be derived.                                             
                                                                                
\medskip                                                                        
The Hipparcos satellite was launched by Ariane 4, flight 33, on 8               
August 1989. At the time of publication of this `Hipparcos Input                
Catalogue', the satellite is more than two years into its measurement           
programme, the on-board instrumentation is functioning according to             
specification and, despite the necessary revisions to the mode of               
operation brought about by the non-nominal orbit, the target accuracies         
of the original mission should be attained.                                     
                                                                                
                                                                                
%                                                                               
\vfill                                                                          
\eject                                                                          
%                                                                               
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{The INCA Consortium (Input Catalogue Consortium)}                     
%-------------------------------------------------                              
                                                                                
The observing programme, by the nature of the mission                           
concept and the data reduction procedures outlined below, had to be             
pre-selected and finalised before launch. The INCA Consortium was               
established in 1981, and was assigned the responsibility, by the                
European Space Agency, of dealing with the definition of, and                   
preparation of, all aspects of the Hipparcos observing programme. The           
final observing programme consists of more than 118\,000 stars, mostly          
within our Galaxy but some within the Magellanic Clouds, one quasar             
(3C273) and, within our solar system, 48 minor planets and three                
satellites of major planets (Europa, Iapetus and Titan). These selected         
objects were based upon 214 scientific proposals submitted to ESA in            
1982, by the world-wide astronomical community, in response to an               
Invitation for Proposals. The selection of objects to be retained for           
observation according to their scientific interest was made by an {\it          
ad hoc} `Hipparcos Scientific Selection Committee'. Their                       
recommendations, constrained by the satellite observing capabilities,           
were implemented by the INCA Consortium, in consultation with the               
original proposers and representatives of the data reduction and                
satellite project teams.  During this work and with the agreement of            
the Hipparcos Scientific Selection Committee, additional proposals were         
defined by the INCA Consortium in order to optimise the scientific              
return expected for some specific topics, notably the introduction of           
the magnitude-limited survey, the selection of stars in the Magellanic          
Clouds and in galactic open clusters, and the introduction of stars             
associated with the improvement of the link to an extragalactic                 
reference system.                                                               
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{The Hipparcos observing programme}                                    
%-------------------------------------------------                              
                                                                                
The final observing programme was selected from some                            
214\,000 proposed candidates following a series of comprehensive                
numerical simulations of the satellite observations. Each iterative             
step of these simulations was followed by an in-depth analysis of the           
resulting provisional selection, its qualities and drawbacks with               
respect to the selection of stars from high-priority proposed                   
programmes, to their observability by the satellite, and to the optimum         
use of the satellite's specific observing capabilities. The 48 minor            
planets and the three other solar system objects finally retained for           
observation were selected purely on the basis of their magnitudes and           
their observability by the satellite.                                           
                                                                                
\medskip                                                                        
A variety of constraints on the contents of the Input Catalogue arise           
from the measurement principle of the Hipparcos satellite, which is             
designed to scan the celestial sphere systematically at a constant              
rate. With a field of view of about $0.9\times 0.9$ degrees, a modulating       
grid of period 1.2 arcsec, and observations conducted by switching the          
`instantaneous field of view' of the detector to those programme stars          
visible within the total field of view, the following broad conditions          
influence the global observing programme: (i)~the number of stars               
per square degree contained in the observing programme is limited;              
(ii)~there is, at the same time, a requirement on the minimum density of        
bright stars and their uniformity across the sky required for satellite         
attitude determination and the subsequent data reductions; (iii)~the            
magnitude distribution of the retained stars must be consistent with            
the available observing time (the minimum acceptable, and target,               
observing times increase with the star magnitude, and this places               
limits on the density of faint stars acceptable within the programme);          
(iv)~to point to each target object, and to observe it with an optimum          
distribution of the available observing time, requires adequate {\it a          
priori} knowledge of the candidate's position and magnitude; (v)~the            
detector's instantaneous field of view profile places stringent                 
constraints on the separation and magnitude difference of double and            
multiple systems that can be usefully observed by the satellite, as             
well as on the selection of stars in dense regions where the signal             
from nearby, bright stars could influence the measurements.                     
                                                                                
\medskip                                                                        
In addition to the selection of the precise satellite observing                 
targets, the INCA Consortium also had the responsibility of compiling,          
and where appropriate improving, the data available for the proposed            
stars and minor planets in order to satisfy the conditions necessary            
for their observation with the Hipparcos satellite. Based upon the              
characteristics of the satellite detection system and measurement               
principle, specifications were set at $\pm 1.5$ arcsec on the {\it a            
priori} positional knowledge of each object at epoch 1990, and $\pm 0.5$        
mag on the {\it a priori} knowledge of the $B$ or $V$ magnitudes for            
all programme stars. As a consequence, extensive compilations of                
astrometric and photometric data were undertaken by the INCA Consortium         
(Turon 1988), along with systematic tests of reliability and                    
consistency of the collected data. Large preparatory ground-based               
observational programmes were subsequently organised in order to                
supplement the available information, and the resulting data finally            
included in the present Input Catalogue therefore comprise a                    
substantial body of previously unpublished data: measurements were              
made of about 100\,000 star positions from photographic plates, some            
10\,000 additional positions from automatic meridian circle                     
observations, 10\,000 star magnitudes and colours obtained from                 
multi-colour photoelectric photometry, and more than 100\,000 star              
colours computed from spectral types combined with a new model of               
galactic extinction. In addition, special programmes were undertaken to         
deal with particular objects, such as double and multiple stellar               
systems, variable stars, stars in galactic open clusters, and minor             
planets.                                                                        
                                                                                
\medskip                                                                        
For the minor planets, a substantial number of new observations                 
with the two automatic meridian circles of Bordeaux and La Palma, and           
with the astrographs of San Fernando and Barcelona, were necessary for          
improving the knowledge of the orbital elements to a standard suitable          
for the satellite observations. For the three satellites of the major           
planets, Europa, Iapetus and Titan, for which studies indicated that            
valuable astrometric information could be acquired from Hipparcos, the          
available ephemerides already satisfied the specified accuracy                  
requirements.                                                                   
                                                                                
%-------------------------------------------------                              
\section*{Contents of this publication}                                         
%-------------------------------------------------                              
                                                                                
The Hipparcos Input Catalogue includes the best available data                  
collected within the framework of the INCA Consortium. The                      
magnetic tape version is composed of the main catalogue, including              
data for each stellar target of the satellite, and one annex                    
containing more detailed data for individual components of double and           
multiple systems for which at least one component is included in the            
main Input Catalogue.                                                           
                                                                                
\medskip                                                                        
The printed version of the Catalogue is published as ESA SP-1136.               
It contains 7 volumes: Volumes~1-5 comprise the main Hipparcos Input            
Catalogue, Volume~6 contains Annex~1 (data for individual components of         
double and multiple systems), Volume~7 contains Annexes~2 to 4                  
(identification charts for the fainter Input Catalogue stars,                   
identification charts for all Input Catalogue  stars in galactic open           
clusters, identification charts for all Input Catalogue  stars in the           
Large and Small Magellanic Clouds).                                             
                                                                                
\medskip                                                                        
A CD-ROM version of the Hipparcos Input Catalogue is being prepared             
containing all data of the main catalogue and Annex~1, and all charts of        
Annexes~2 and 3, along with interrogating and mapping software.                 
                                                                                
                                                                                
\medskip                                                                        
In addition, the INCA Consortium structure and membership, the                  
Hipparcos Scientific Selection Committee membership, and the list of            
all scientific programmes received by ESA for observation with                  
Hipparcos, are given at the end of this introduction.                           
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{References}                                                           
%-------------------------------------------------                              
                                                                                
A complete description of all aspects of the preparation of                     
the Hipparcos Input Catalogue can be found in the proceedings of two            
Colloquia on `Scientific Aspects of the Input Catalogue Preparation'            
(Aussois, June 1985, ESA-SP 234, Turon \& Perryman eds; and Sitges,             
January 1988, Torra \& Turon eds), in ESA-SP 1111, Volume~II (The               
Hipparcos Mission: Pre-Launch Status, Perryman \& Turon 1989), and in           
a series of papers in {\it Astronomy} \& {\it Astrophysics} covering star       
selection (Turon \ETAL\ 1992a), astrometric aspects (Jahrei\ss~\ETAL\           
1992), photometric aspects (Grenon \ETAL\ 1992), solar system objects           
(Bec-Borsenberger 1992a), long-period variable stars (Mennessier                
\ETAL\ 1992), the adopted galactic extinction model (Arenou                     
\ETAL\ 1992), and the VLBI link to an extragalactic frame (Lestrade             
\ETAL\ 1992). The performances of the Input Catalogue, as tested by the         
first results from the satellite, are presented by Crifo \ETAL\ (1992)          
and Turon \ETAL\ (1992b). All aspects of the link of the Hipparcos              
reference frame to an extragalactic reference frame are described by            
Argue (1989) and Jahrei\ss~\ETAL\ (1992). The data on double and                
multiple systems will be contained in the `Catalogue of the Components          
of Double and Multiple Stars' (CCDM, Dommanget \ETAL, in preparation).          
Annex~1 is a subset of a preliminary version of this catalogue. The             
improved orbital elements of the relevant minor planets, along with             
predicted ephemerides for the years 1991 and 1992, have been given by           
Bec-Borsenberger (1990, 1992b).                                                 
                                                                                
                                                                                
                                                                                
%                                                                               
\vfill                                                                          
\eject                                                                          
%                                                                               
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\LARGE\bf Star Selection}                                               
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
                                                                                
\bigskip\bigskip                                                                
                                                                                
                                                                                
The 118\,000 stars of the Hipparcos Input Catalogue were                        
selected from some 214\,000 distinct candidates, contained in the 214           
observation programmes listed at the end of this introduction. The              
scientific proposals deal with a wide variety of astrophysical and              
astronomical subjects: solar system, stellar physics and evolution,             
galactic structure, kinematics, dynamics and evolution, cosmic distance         
scale, and reference systems. With the endorsement of the ESA Hipparcos         
Scientific Selection Committee, the INCA Consortium supplemented the            
proposed list of stars with others considered to be unrepresented in            
the original compilation. Most importantly, this included a basic list          
of bright stars, essentially complete to a well-defined limiting                
magnitude, and hence referred to as the `survey'.                               
                                                                                
\medskip                                                                        
The original set of proposed stars was, not surprisingly, poorly suited         
to the observing capabilities of the Hipparcos experiment: the sky              
distribution of the 214\,000 proposed stars                                     
showed a strong                                                                 
concentration towards the galactic plane, and especially towards the            
galactic centre, and their $V$ -magnitude distribution showed a predominance    
of faint stars. As a result of the work of the INCA Consortium in merging,      
optimising, and supplementing the original list, the final Hipparcos Input      
Catalogue of about 118\,000 stars can broadly be considered as being            
composed of two parts:                                                          
                                                                                
\begin{itemize}                                                                 
\item a basic list of 52\,000 `bright' stars (the `survey'), complete           
      to a limiting magnitude which is a function of the star's spectral type   
      and galactic latitude (Crifo \ETAL\ 1985; Turon \& Crifo 1986;            
      Turon \ETAL\ 1989a; G\'omez \ETAL\ 1989), and defined by:                 
      \[                                                                        
      \begin{array}{rcll}                                                       
       V_{\rm lim} &\le& 7.9 + 1.1\sin |b| &                                    
        \mbox{\rm ~~~for spectral types earlier or equal to G5,}\\              
       V_{\rm lim} &\le& 7.3 + 1.1\sin |b| &                                    
        \mbox{\rm ~~~for spectral types later than G5.}\\                       
      \end{array}                                                               
      \]                                                                        
      If no spectral type was available, the break was taken at $B-V=0.8$       
      mag. The original star selection for this survey was made from the        
      SIMBAD data base (Egret \ETAL\ 1991).                                     
\item 66\,000 `faint' additional stars selected from the proposed               
      observing programmes according to the priorities allocated by the         
      Hipparcos Scientific Selection Committee. The allocated priorities,       
      reflecting the Committee's assessment of the scientific importance of     
      the proposals, ranged from priority 1 (the highest) to priority 5 (the    
      lowest).                                                                  
\end{itemize}                                                                   
                                                                                
Although the inclusion of the bright stars was partly motivated by              
reasons related to the satellite operations (attitude determination)            
and data reductions, the precise choice of stars was not in itself              
significant for these purposes. The only two basic requirements were to         
retain a reasonably regular stellar density of bright stars all over            
the sky, and to ensure that a large sub-sample of these stars would             
have sufficiently accurate {\it a priori} positions. Stars were                 
therefore chosen such that any further statistical uses of the                  
catalogue, for example in the domains of galactic physics, would be             
enhanced by this choice. The above survey definition satisfies all              
three requirements, while at the same time reducing the proportion of           
red giant stars in favour of A and F stars. The latter, being                   
typically closer, will get a correspondingly more accurate                      
determination of their distances and space motions. \par                        
                                                                                
\medskip                                                                        
As a result, the 118\,000 selected stars, just 55 per cent of those             
originally proposed, actually represent 94 per cent of the `priority 1'         
stars. Their distribution on the sky is much smoother than                      
that of proposed stars, even though more (bright) stars are selected in         
the galactic plane than outside. Their $V$ -magnitude distribution              
shows a maximum between 7 and 10 mag, and very few stars                        
fainter than 12 mag (these stars require a very large fraction of the           
available observing time). The final star selection (Turon 1989) was            
made following an iterative process, using numerical simulations of the         
mission (Cr\'ez\'e \ETAL\ 1989). These simulations progressively took           
into account all the astrometric and photometric data collected or              
newly obtained within the INCA Consortium, as well as all data coming           
from parallel work on double, multiple and variable stars. All these            
data are collected in a dedicated data base, the INCA data base,                
originally constructed as a sub-base of SIMBAD, with the data and               
cross-identifications from SIMBAD (Arenou \& Morin 1988; Turon \ETAL\           
1991). The updating and interrogation software of this data base was an         
important asset in storing and managing all the data necessary for the          
construction of the Input Catalogue.                                            
                                                                                
\medskip                                                                        
In the context of the Hipparcos Input Catalogue, and especially in              
discussions of the Input Catalogue's statistical properties, the word           
`star' is frequently used when catalogue `entry' would be more                  
appropriate. An `entry' refers to a satellite target: it may be a               
single star, a component of a double or multiple system, or a unique            
joint entry for a close double or multiple system. This is a specific           
feature of the Hipparcos Input Catalogue, reflecting the satellite's            
detection system. It should be stressed again that the Input Catalogue          
was compiled specifically for the Hipparcos programme.  Its stellar and         
data contents reflect these fundamental requirements.                           
                                                                                
                                                                                
                                                                                
                                                                                
                                                                                
%*******************************************************************************
%*******************************************************************************
\part*{MAIN CATALOGUE}                                                          
%*******************************************************************************
%*******************************************************************************
                                                                                
                                                                                
                                                                                
                                                                                
                                                                                
                                                                                
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\LARGE\bf Main Catalogue Description}                                   
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
\bigskip                                                                        
\bigskip                                                                        
\noindent                                                                       
{\bf Note: the field numbers of the Main Catalogue are not identical            
to those of the printed version (ESA~SP-1136) as some additional information    
has been added: the correspondence between the two are given in the             
table describing the magnetic tape format. Field entries are blank if the       
corresponding data are not available.}                                          
                                                                                
                                                                                
\bigskip                                                                        
\noindent                                                                       
The description of the data given below follows the order of                    
the columns of the Hipparcos Input Catalogue.  Further explanations, along with 
relevant information on how the data were collected and selected, are included  
in smaller type. Full names and references of all catalogues are given          
at the end of this introduction \RPAGE{endintro}. In general, the number of     
decimals retained provides an indication of the precision of the data.          
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{Fields 1-3: Hipparcos Input Catalogue (HIC) Identification}           
%-------------------------------------------------                              
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{1}{Hipparcos Input Catalogue (HIC) running number}                      
%++++++++++++++++++++++++                                                       
                                                                                
The star entries are ordered by increasing HIC number. This numbering           
basically follows the order of the object's right ascension (equinox            
J2000.0), independent of declination. The catalogue epoch is J2000.0,           
although stars with unknown proper motion are referred to their                 
original epoch of measurement. There is one entry in the main catalogue         
corresponding to each satellite {\it target}, irrespective of the               
possible multiplicity of the star. If the star is a component of a              
known double or multiple system, fields 2-3 provide further                     
information.                                                                    
                                                                                
\medskip                                                                        
Entries which have been suppressed from the observing programme after           
launch, and therefore result in HIC numbers no longer contained within          
the Input Catalogue, are listed in Table~A1 \ref{table:A1}\RPAGE{table:A1}.     
                                                                                
                                                                                
\begin{table}[p]                                                                
\vspace{0.5cm}                                                                  
\CENTER {Table A1: HIC numbers of objects suppressed from the                   
Input Catalogue}                                                                
\label{table:A1}                                                                
\vspace{0.5cm}                                                                  
\centering                                                                      
\begin{tabular}{rrrrrr} \hline \\                                               
672 & 28810 & 48831 & 63158 & 86909 & 106808\\                                  
1569 & 31077 & 49190 & 64239 & 87011 & 108292\\                                 
3814 & 31441 & 49361 & 65576 & 88138 & 110971\\                                 
5200 & 31865 & 49550 & 66518 & 88168 & 111772\\                                 
5791 & 31869 & 50224 & 67089 & 89395 & 112054\\                                 
\\                                                                              
8402 & 32720 & 51431 & 67295 & 90057 & 112313\\                                 
9584 & 33870 & 52081 & 67920 & 90682 & 112445\\                                 
9626 & 33967 & 52754 & 67924 & 90688 & 114095\\                                 
11119 & 34232 & 54637 & 68098 & 91787 & 114122\\                                
11916 & 34593 & 55419 & 69217 & 91835 & 115426\\                                
\\                                                                              
11961 & 35175 & 56283 & 74720 & 92357 & 116059\\                                
12388 & 35292 & 56288 & 76367 & 96513 & 116992\\                                
15088 & 36230 & 56804 & 78626 & 96578\\                                         
15417 & 36353 & 57147 & 78778 & 96685\\                                         
15502 & 37807 & 57354 & 81359 & 97453\\                                         
\\                                                                              
18193 & 38450 & 58156 & 82616 & 98686\\                                         
18200 & 38452 & 58209 & 82846 & 99630 \\                                        
19006 & 39151 & 59097 & 82924 & 100410\\                                        
20461 & 39615 & 59304 & 83437 & 101609\\                                        
24045 & 40207 & 59860 & 83470 & 101775\\                                        
\\                                                                              
24908 & 41023 & 60606 & 84039 & 101872\\                                        
25384 & 43168 & 60656 & 85550 & 102008\\                                        
26911 & 45172 & 60898 & 85754 & 102079\\                                        
27274 & 47481 & 61056 & 86018 & 104519\\                                        
28058 & 47855 & 63146 &86337  & 105516\\                                        
\FINTABLE                                                                       
                                                                                
                                                                                
\begin{table}[p]                                                                
\centering                                                                      
\vspace{0.5cm}                                                                  
\CENTER {Table A2/1: Supplementary HIC numbers - ordered by running             
number}                                                                         
\label{table:A2/1} \vspace{0.5cm}                                               
\begin{tabular}{rlrlrl} \hline \\                                               
\multicolumn{1}{c}{HIC} & \multicolumn{1}{c}{RA} &                              
\multicolumn{1}{c}{HIC} & \multicolumn{1}{c}{RA} &                              
\multicolumn{1}{c}{HIC} & \multicolumn{1}{c}{RA}\\ \\ \hline \\                 
120001 & 05 10 42.37 & 120047 & 07 15 18.694 & 120212 & 12 27 48.113\\          
120002 & 05 59 25.16 & 120071 & 10 07 38.261 & 120229 & 21 58 41.732\\          
120003 & 06 31 09.68 & 120082 & 11 39 49.882 & 120248 & 06 49 51.093\\          
120004 & 08 25 48.528 & 120121 & 16 04 48.154 & 120250 & 21 10 01.778\\         
120005 & 09 14 24.723 & 120132 & 18 00 10.084 & 120276 & 10 02 04.672\\         
120006 & 14 53 20.95 & 120148 & 20 03 00.888 & 120290 & 16 57 40.942\\          
120027 & 03 19 13.104 & 120155 & 20 21 31.78 & 120306 & 23 06 44.94\\           
120046 & 07 03 52.545 & 120159 & 21 22 59.83 & 120313 & 13 45 35.65\\           
\\ \hline \\ \end{tabular}                                                      
                                                                                
\vspace{0.5cm}                                                                  
\CENTER {Table A2/2: Supplementary HIC numbers - ordered by right               
ascension}                                                                      
\label{table:A2/2} \vspace{0.5cm}                                               
\begin{tabular}{rlrlrl} \hline \\                                               
\multicolumn{1}{c}{HIC} & \multicolumn{1}{c}{RA} &                              
\multicolumn{1}{c}{HIC} & \multicolumn{1}{c}{RA} &                              
\multicolumn{1}{c}{HIC} & \multicolumn{1}{c}{RA}\\ \\ \hline \\                 
120027 & 03 19 13.104 & 120005 & 09 14 24.723 & 120290 & 16 57 40.942\\         
120001 & 05 10 42.37 & 120276 & 10 02 04.672 & 120132 & 18 00 10.084\\          
120002 & 05 59 25.16 & 120071 & 10 07 38.261 & 120148 & 20 03 00.888\\          
120003 & 06 31 09.68 & 120082 & 11 39 49.882 & 120155 & 20 21 31.78\\           
120248 & 06 49 51.093 & 120212 & 12 27 48.113 & 120250 & 21 10 01.778\\         
120046 & 07 03 52.545 & 120313 & 13 45 35.65 & 120159 & 21 22 59.83\\           
120047 & 07 15 18.694 & 120006 & 14 53 20.95 & 120229 & 21 58 41.732\\          
120004 & 08 25 48.528 & 120121 & 16 04 48.154 & 120306 & 23 06 44.94\\          
\\ \hline \\ \end{tabular}                                                      
                                                                                
                                                                                
\medskip                                                                        
\parbox{18cm}{                                                                  
The following stars in NGC 2516, added to the Hipparcos observing list at a late
stage of the measurement programme, are not included in the main catalogue (nor 
in the above table, nor in the finding chart for NGC 2516 given in Annex~3 of   
the printed version, where the reference to the adopted numbering system is     
given):}                                                                        
                                                                                
                                                                                
\CENTER{                                                                        
HIC 120401 = NGC 2516  12\\                                                     
HIC 120402 = NGC 2516  91\\                                                     
HIC 120403 = NGC 2516  11\\                                                     
HIC 120404 = NGC 2516  15                                                       
}                                                                               
                                                                                
\end{table}                                                                     
                                                                                
\begin{SMALLFIELD}                                                              
The Hipparcos Input Catalogue running number was created in                     
1988, for the first preliminary version distributed to ESA, to ESOC             
(ESA's European Space Operations Centre), and to the Data Reduction             
Consortia. This first version was used for the development of the               
software for operating the satellite, and for reducing the Hipparcos            
data. One consequence of the Input Catalogue's development is that              
increasing HIC number does not always correspond precisely to the order         
of increasing right ascension (field~4) for two reasons:                        
                                                                                
\begin{itemize}                                                                 
\item from the start of the Input Catalogue work, the star                      
      entries have been ordered and numbered for epoch J1990.0, corresponding   
      to the mean epoch adopted for Hipparcos operational considerations,       
      rather than for epoch J2000.0, the epoch adopted for the Input            
      Catalogue publication;                                                    
\item after the start of the satellite operations, and as a                     
      result of verifications made on the early observations, some stars were   
      deleted from the programme, and some corrections to the catalogue         
      entries were made. Where this resulted in a change in position of more    
      than several arcsec, a new HIC running number was allocated to the star   
      in order to provide a clear update at the operational level, and to       
      avoid any possible confusion within the data reductions. These 24         
      recently-assigned numbers, unrelated to the right ascension of the        
      affected entry, lie between 120\,001 and 120\,313.                        
\end{itemize}                                                                   
                                                                                
\medskip\noindent                                                               
As ordered by right ascension, 33 stars are out of sequence by 10 to 20         
places, and 70 by 5 to 9 places. Stars for which                                
the displacement would have been larger than 20 entries have been               
allocated a number larger than 120\,000. The 137                                
`missing' HIC numbers, resulting from these reallocations or from               
suppression of the original target after launch, are given in Table~A1          
\ref{table:A1} \RPAGE{table:A1}.                                                
The 24 `additional' HIC numbers, ordered by increasing                          
running number with their right ascension, and by right ascension, are          
listed in Table~A2/1 \ref{table:A2/1} \RPAGE{table:A2/1} and Table~A2/2         
\ref{table:A2/2}                                                                
\RPAGE{table:A2/2} respectively.                                                
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%                                                                               
\vfill                                                                          
\eject                                                                          
%                                                                               
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{2}{Component(s) considered}                                             
%++++++++++++++++++++++++                                                       
                                                                                
A letter (or letters) in this field indicates that the star is part of          
a known double or multiple system.  In the case of a double system with         
well-separated components, for example, `A' or `B' indicates that the           
entry corresponds to that component. In the case of a `joint' entry             
(see field~3) letters indicate which of the components of the system            
are considered (e.g. `AB', `AC', `APB', etc.).                                  
                                                                                
                                                                                
\begin{SMALLFIELD}                                                              
Due to the nature of the Hipparcos detection system (the                        
diameter of the instantaneous field of view of the primary detection            
system is about 38 arcsec), two stars or components within 10 arcsec            
are observed by the satellite as a unique target. If the component              
separation is larger than 10 arcsec, the number of discrete entries in          
the main catalogue will correspond to the number of separate observing          
targets defined within the observing programme. The number of such              
entries will not necessarily correspond to the number of known                  
components of the double or multiple system, for example in those cases         
where the fainter component(s) have not been retained for the satellite         
observations.                                                                   
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{3}{Satellite target in case of a joint entry}                           
%++++++++++++++++++++++++                                                       
                                                                                
While the location of the `satellite target' (the part of the sky on            
which the detector is centred for the particular observation) is well           
defined for single stars, being the best estimate of the star's                 
position at the epoch of the satellite observation, the situation is            
not so straightforward for double or multiple systems. For such                 
systems, the choice of the target position may be:                              
                                                                                
\begin{itemize}\itemsep=-4pt                                                    
\item the brighter component (designated by the                                 
      corresponding letter);                                                    
\item the geometric centre, i.e. the mid-point between two                      
      components (designated by {\it g});                                       
\item the photocentre (designated by {\it j}).                                  
\end{itemize}                                                                   
                                                                                
\begin{SMALLFIELD}                                                              
The nature of the target for the satellite observation depends                  
upon the separation and difference of magnitudes between the                    
components, and has been dictated by considerations of the observation          
and data reduction procedures (Turon \ETAL\ 1989b). The brighter                
component is chosen when the signal perturbation due to the other               
component(s) can be neglected ($\Delta m \ge 1.2$ mag).                         
For $\Delta m < 1.2$ mag, there are two possibilities according to the          
geometry of the system and the availability of data for                         
the components. The geometric centre has                                        
been selected when the positions and magnitudes of each component are           
known. A `geometric centre' may also have been adopted for some                 
multiple systems when the two brightest components dominate the other           
components. The photocentre has been selected if the separation is such         
that only one position or magnitude has been obtained for the system as         
a whole, or in the case of multiple systems. When the component                 
separation is smaller than 3 arcsec, the entry is considered as a               
photocentre irrespective of the difference of magnitude between the             
components.                                                                     
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{Fields 4-11: Position (Equinox J2000.0)}                              
%-------------------------------------------------                              
                                                                                
The position given here is the position of the satellite target.                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{4}{Right ascension (hours, minutes, and seconds, equinox J2000.0)}      
%++++++++++++++++++++++++                                                       
                                                                                
The right ascension, $\alpha$, is given for equinox J2000.0                     
in the FK5 system (Fricke \ETAL\ 1988), in hours, minutes, and seconds.         
The epoch is J2000.0, except when no proper motion is available.                
The epoch corresponding to the published right ascension is given in field~6.   
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{5}{Declination (degrees, minutes, and seconds, equinox J2000.0)}        
%++++++++++++++++++++++++                                                       
                                                                                
The declination, $\delta$, is given for equinox J2000.0 in                      
the FK5 system (Fricke \ETAL\ 1988), in degrees, minutes, and seconds.          
The epoch is J2000.0, except when no proper motion is available.                
The epoch corresponding to the published declination is                         
given in field~6.                                                               
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{6}{Epoch for the position}                                              
%++++++++++++++++++++++++                                                       
                                                                                
The epoch is for the position given in fields 4-5 and 10-15.                    
                                                                                
\begin{SMALLFIELD}                                                              
Epoch J2000.0 was chosen for the Input Catalogue publication,                   
corresponding to the `standard' epoch common to all recently-published          
catalogues, even though the epoch for the version used for satellite            
operations was 1990.                                                            
                                                                                
\medskip                                                                        
If the epoch is different from 2000.0, this indicates that only a single        
epoch position is available, and therefore no proper motion can be              
derived. Where relevant, the stated epoch refers to the average of the          
epochs for $\alpha$ and $\delta$.                                               
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{7}{Mean error of the right ascension}                                   
%++++++++++++++++++++++++                                                       
                                                                                
The mean error of the right ascension, $15\cos\delta$ $\times$ m.e. in          
$\alpha$, is given in field~7, expressed in units of arcsec.                    
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{8}{Mean error of the declination}                                       
%++++++++++++++++++++++++                                                       
                                                                                
The mean error of the declination is given in field~8, expressed in             
units of arcsec.                                                                
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{9}{Source of position}                                                  
%++++++++++++++++++++++++                                                       
                                                                                
The positions contained in the Hipparcos Input Catalogue are derived            
from a wide variety of sources. The correspondence between the letters          
used in field~9 and the source of the positions, along with the number          
of stars whose position was taken from the source, is given in Table~B1.        
\ref{table:B1}                                                                  
                                                                                
\begin{SMALLFIELD}                                                              
\begin{table}[htb]                                                              
\vspace{0.5cm}                                                                  
\CENTER {Table B1: Source of positions and proper motions}\label{table:B1}      
\vspace{0.5cm}                                                                  
\centering                                                                      
\begin{tabular}{clcrr} \hline \\                                                
\multicolumn{1}{c}{Source} & \multicolumn{1}{c}{Source} &                       
\multicolumn{1}{c}{Abbreviation} & \multicolumn{2}{c}{No. of Stars}\\           
\multicolumn{1}{c}{Code} & & & \multicolumn{1}{c}{Positions} &                  
\multicolumn{1}{c}{Motions}\\ \\ \hline \\                                      
B & General Catalogue (Boss)                                                    
& GC          & 140    & 2 577\\                                                
C & Cape Photographic Catalogue for 1950.0                                      
& CPC         & 18     & 4 738\\                                                
D & Catalogue of Components of Double and Multiple Stars*                       
& CCDM        & 7 596  & 5 867\\                                                
F & FK5 and FK5 extension **                                                    
& FK5/FK5 Ext & 2 523  & 2 526\\                                                
G & Guide Star Catalog                                                          
& GSC         & 618    & -\\                                                    
K & FK4 Supplement                                                              
& FK4 Sup     & 994    & 995\\                                                  
M & Bordeaux and/or Carlsberg automatic meridian circles***                     
& - / CAMC    & 8 221  & 6 075\\                                                
N & New plate measurements or new proper motions                                
& -           & 14 480 & 27\\                                                   
P & Catalogue of Positions and Proper Motions*                                  
& PPM         & 49 936 & 50 464\\                                               
R & International Reference Stars (AGK3RN, SRS*)                                
& IRS         & 14 695 & 8 918\\                                                
S & Smithsonian Astrophysical Observatory Star Catalogue                        
& SAO         & 163    & 14 341\\                                               
T & Cape Catalogue of Faint Stars                                               
& CF          & -      & 889\\                                                  
X & Miscellaneous                                                               
& -           & 114    & 3 524\\                                                
Y & Sydney Southern Star Catalogue                                              
& SSSC        & 4 786  & 4 260\\                                                
2 & Second Cape Photographic Catalogue****                                      
& CPC2        & 12 900 & 7 259\\                                                
3 & Catalogue of Standard Stars Based on the N30 System                         
& N30         & 277    & 381\\                                                  
5 & Second Cape Photographic Catalogue for 1950.0                               
& 2CP50       & 748    & 1 416\\                                                
  & [Entry without corresponding information]                                   
& [ - ]       & [ - ]  & [3 952]\\ \\ \hline \\                                 
\end{tabular}                                                                   
                                                                                
\begin{itemize}\itemsep=-4pt                                                    
\item[*] provisional version                                                    
\item[**] faint stars of the FK5 Extension were not included for                
     schedule reasons                                                           
\item[***] of these two sources, only the Carlsberg Meridian Catalogues         
     give proper motions                                                        
\item[****] preliminary version (courtesy W. Nicholson \& C. de Vegt)           
\end{itemize}                                                                   
\end{table}                                                                     
                                                                                
\medskip                                                                        
As far as possible, all positions and proper motions were                       
initially reduced to the FK4 system for equinox and epoch B1950.0.              
Subsequently, all data were transformed to the FK5 system and to                
equinox and epoch J2000.0, i.e. the old standard was replaced by the            
IAU (1976) system, and the systematic corrections FK5-FK4 were applied          
as given in Fricke \ETAL\ (1988). A recent discussion of such                   
transformations can be found in Smith \ETAL\ (1989).                            
                                                                                
\medskip                                                                        
The above procedure applies also to the new meridian circle                     
measurements, which were performed differentially with respect to the           
FK5 system for equinox J2000.0. However, for the basic FK5 (Fricke \ETAL\       
 1988) and the FK5 extension (Fricke \ETAL\ 1991) stars, the J2000.0            
data were taken directly from the respective catalogues. Their B1950.0          
data (fields 16-19) were then obtained by transforming the J2000.0 FK5          
data to equinox and epoch B1950.0 and eliminating all systematic                
corrections applied in the transition from FK4 to FK5.  Therefore, the          
B1950.0 data of the basic FK5 and FK4 Supplement stars are not                  
identical to those given in the FK4 and FK4 Supplement catalogues since         
the individual corrections FK5-FK4 are still included.                          
                                                                                
\medskip                                                                        
The data given in fields 4-9 are the result of extensive                        
compilations of previously-available data (Bastian \& Lederle 1985;             
Jahrei\ss\ 1988, 1989; Jahrei\ss\ \ETAL\ 1992), and new observations            
and measurements (R\'equi\`eme 1982, 1985, 1986, 1988a, 1988b, 1989;            
Mui\~nos \ETAL\ 1988; Le Poole \ETAL\ 1988; Morrison \& Gibbs 1985;             
Turon \& R\'equi\`eme 1984) performed by the INCA Consortium. The new           
observations were necessary since many of the stars of high                     
astrophysical interest were not contained in the major astrometric              
catalogues.                                                                     
                                                                                
\medskip                                                                        
The compilation of existing `astrometric data', i.e. position                   
and proper motion data of good quality, was performed at the                    
Astronomisches Rechen-Institut at Heidelberg, and collected within the          
CDA (Catalogue des Donn\'ees Astrom\'etriques, Bastian \& Lederle 1985;         
Jahrei\ss~ 1988, 1989). Data were taken from the FK5, FK5 extension,            
FK4~Sup, PPM, AGK3RN, SRS, NPZT74, N30, 2CP50, GC, AGK3, SSSC, CPC2,            
SAO, CPC (the given order corresponding roughly to decreasing order of          
positional accuracy). FK5 data were not used for the faint stars of the         
FK5 Extension for schedule reasons.                                             
                                                                                
%                                                                               
\vfill\eject                                                                    
%                                                                               
                                                                                
In addition to this compilation work, and once the list of                      
stars requiring new positional data was established, extensive                  
campaigns of new observations and measurements were initiated and               
organised according to the capabilities of the European institutes              
involved in the INCA Consortium. From south to north, in equatorial             
coordinates, contributions were made as follows:                                
                                                                                
\begin{itemize}\itemsep=-4pt                                                    
\item for $-90\degr < \delta < -17\degr.5$: measurements for this zone          
      were performed on glass                                                   
      copies of the ESO Quick Blue and ESO/SERC J Sky Survey Schmidt plates.    
      The measurements were shared by the Bordeaux, Royal Greenwich,            
      Marseille, and Leiden Observatories, which measured respectively some     
      100\,000, 5\,400, 15\,000, and 5\,000 (Input Catalogue and                
      `reference') stars;                                                       
\item for  $-25\degr < \delta < 0\degr$:                                        
      observations of about 2500 `non-astrometric stars' with the Carlsberg     
      Automatic Meridian Circle at La Palma;                                    
\item for $-5\degr < \delta < +81\degr$:                                        
      observations of about 5500 stars with the Bordeaux Observatory            
      automatic meridian circle;                                                
\item for $+80\degr < \delta < +90\degr$:                                       
      measurements on plates taken with an astrograph at the                    
      Hamburg Observatory.                                                      
\end{itemize}                                                                   
                                                                                
\medskip\noindent                                                               
In addition, 950 SAO stars with poor positions in the zone                      
$-40\degr < \delta < 0\degr$ were observed with the                             
Carlsberg Automatic Meridian Circle.                                            
                                                                                
\medskip                                                                        
All collected data, compiled and newly obtained from                            
ground-based observations or measurements, were then processed in a             
global and homogeneous way (Jahrei\ss~ 1989). The selection of the best         
data for each star was made following their expected positional                 
accuracy at epoch 1990, the adopted mean observing epoch of Hipparcos.          
This choice strongly depends on the errors of the available proper              
motions. Only for a very small number of catalogues (FK5, PPM, AGK3RN,          
GC, and the new meridian circle observations) are the positional error          
estimates given individually for each star. For other catalogues and            
for plate measurements, the central epoch (when individual epochs are           
not available), the mean error at that epoch, and the proper motion             
error (when a proper motion is available) had to be evaluated. For              
regions south of -17$\degr$.5, plate measurements were made for all             
proposed stars, yielding a significant overlap with the CDA. This               
allowed further comparisons and checks between the different sources of         
data. At the end of the campaigns of new observations and measurements,         
a few hundred stars remained without reliable positions.  Positions             
(and in a few cases magnitudes) were taken from the Guide Star Catalog          
(Lasker \ETAL\ 1990).                                                           
                                                                                
\medskip                                                                        
In parallel with the global observing and measuring campaigns,                  
specific measurement programmes were devoted to stars in galactic open          
clusters, for which careful attention had to be given to the problems           
of star identification, and to stars in double and multiple systems.            
Stars in galactic open clusters were measured on plates taken with an           
astrograph at Hamburg Observatory for the northern hemisphere, and at           
the M\"unster University Astronomy Department for the southern                  
hemisphere (Tucholke 1988, 1989). An additional verification was made           
for stars south of $-17\degr.5$ by the comparison of the                        
identifications and positions obtained respectively on astrograph and           
on Schmidt plates (from measurements made at Bordeaux).                         
                                                                                
\medskip                                                                        
For stars in double and multiple systems, the situation was                     
more problematical than for single stars for two main reasons. First,           
it was not straightforward to cross-identify their components with the          
stars in large astrometric catalogues. Second, in many cases                    
discrepancies exist between the individual positions given in these             
catalogues for each component, and the relative positions given in              
catalogues of double and multiple systems. As a consequence, an                 
extensive programme of compilation and analysis of the existing data            
was required, before defining the necessary measuring programmes                
(Dommanget 1985, 1988, 1989). The work was organised by the team of the         
Observatoire Royal de Belgique at Brussels, and the collected and newly         
obtained data were incorporated into the CCDM (Catalogue of Components          
of Double and Multiple stars, Dommanget \ETAL, in preparation). The             
construction of this catalogue was undertaken in Brussels starting from         
1981 (Dommanget 1983) and subsequently improved with newly compiled and         
observed data. CCDM positions are the result of a compilation from a            
large number of other sources: CDA positions were used when there               
was no doubt about component identification. Many other sources were            
compiled and new measurements obtained within the framework of the              
Double and Multiple Star Working Group of the INCA Consortium. This             
work has been presented in detail by Dommanget (1989), and is also              
summarised in the introduction to Annex~1. Depending on the                     
characteristics of the stellar system (separation and difference of             
magnitude between components) the positional and proper motion data             
were processed differently: systems with separation smaller than                
3~arcsec, and the bright components of systems where the expected               
Hipparcos signal perturbation due to the presence of secondaries was            
negligible, were processed as single stars. In most other cases, all            
data were taken from a preliminary version of the CCDM. A few hundred           
systems with very poor positions were processed individually, in a              
collaboration between Meudon and Brussels using new ground-based                
measurements, meridian circle observations and, in some cases, the              
GSC.                                                                            
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{10}{Right ascension (decimal degrees, equinox J2000.0)}                 
%++++++++++++++++++++++++                                                       
                                                                                
The right ascension, $\alpha$, is given for equinox J2000.0                     
in the FK5 system (Fricke \ETAL\ 1988), in decimal degrees.                     
The epoch is J2000.0, except when no proper motion is available.                
The epoch corresponding to the published right ascension is                     
given in field~6.                                                               
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{11}{Declination (decimal degrees, equinox J2000.0)}                     
%++++++++++++++++++++++++                                                       
                                                                                
The declination, $\delta$, is given for equinox J2000.0 in                      
the FK5 system (Fricke \ETAL\ 1988), in decimal degrees.                        
The epoch is J2000.0, except when no proper motion is available.                
The epoch corresponding to the published declination is                         
given in field~6.                                                               
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section* {Fields 12-15: Other coordinates}                                     
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{12}{Galactic longitude}                                                 
%++++++++++++++++++++++++                                                       
                                                                                
The galactic longitude is given in decimal degrees.                             
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{13}{Galactic latitude}                                                  
%++++++++++++++++++++++++                                                       
                                                                                
The galactic latitude is given in decimal degrees.                              
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{14}{Ecliptic longitude}                                                 
%++++++++++++++++++++++++                                                       
                                                                                
The ecliptic longitude is given in decimal degrees.                             
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{15}{Ecliptic latitude}                                                  
%++++++++++++++++++++++++                                                       
                                                                                
The ecliptic latitude is given in decimal degrees.                              
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section* {Fields 16-19: Position (Equinox B1950.0)}                            
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{16}{Right ascension (equinox B1950.0, hours, minutes, seconds)}         
%++++++++++++++++++++++++                                                       
                                                                                
The right ascension in field~16 is given in the FK4 system for                  
equinox B1950.0, in hours, minutes, and seconds. The epoch is 1950.0            
except when no proper motion is available. In this case, the epoch is           
given in field~6. See fields 4-9 for further                                    
explanation.                                                                    
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{17}{Declination (equinox B1950.0, degrees, minutes, seconds)}           
%++++++++++++++++++++++++                                                       
                                                                                
The declination in field~17 is given in the FK4 system for                      
equinox B1950.0, in degrees, minutes, and seconds. The epoch is 1950.0          
except when no proper motion is available. In this case, the epoch is           
given in field~6. See fields 4-9 for further                                    
explanation.                                                                    
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{18}{Right ascension (equinox B1950.0, decimal degrees)}                 
%++++++++++++++++++++++++                                                       
                                                                                
The right ascension in field~18 is given in the FK4 system for                  
equinox B1950.0, in decimal degrees. The epoch is 1950.0                        
except when no proper motion is available. In this case, the epoch is           
given in field~6. See fields 4-9 for further                                    
explanation.                                                                    
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{19}{Declination (equinox B1950.0, decimal degrees)}                     
%++++++++++++++++++++++++                                                       
                                                                                
The declination in field~19 is given in the FK4 system for                      
equinox B1950.0, in decimal degrees. The epoch is 1950.0                        
except when no proper motion is available. In this case, the epoch is           
given in field~6. See fields 4-9 for further                                    
explanation.                                                                    
                                                                                
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section* {Fields 20-24: Proper Motion}                                         
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{20}{Proper motion in right ascension (equinox J2000.0)}                 
%++++++++++++++++++++++++                                                       
                                                                                
The proper motion in right ascension, $15\mu_\alpha \cos\delta$,                
is expressed in units of arcsec per year. The equinox is                        
J2000.0.  The proper motion is given in the system of the FK5 whenever          
the necessary information was available.                                        
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{21}{Proper motion in declination (equinox J2000.0)}                     
%++++++++++++++++++++++++                                                       
                                                                                
The proper motion in declination, $\mu_\delta$,                                 
is expressed in units of arcsec per year. The equinox is J2000.0.  The          
proper motion is given in the system of the FK5 whenever the necessary          
information was available.                                                      
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{22}{Mean error of the proper motion in right ascension}                 
%++++++++++++++++++++++++                                                       
                                                                                
The mean error of the proper motion in right ascension ($15\mu_\alpha           
cos\delta$) is given in  field~22. It is  expressed in units of                 
milli-arcsec per year.                                                          
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{23}{Mean error of the proper motion in declination}                     
%++++++++++++++++++++++++                                                       
                                                                                
The mean error of the proper motion in declination ($\mu_\delta$) is given      
in  field~23. It is  expressed in units of  milli-arcsec per year.              
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{24}{Source of proper motion}                                            
%++++++++++++++++++++++++                                                       
                                                                                
The proper motions in the Hipparcos Input Catalogue are derived from a          
wide variety of sources.  The correspondence between the letters used           
in field~24 and the source of the proper motions, along with the number         
of stars whose proper motion was taken from this source, is given in            
Table~B1 \ref{table:B1}\RPAGE{table:B1}.                                        
                                                                                
\begin{SMALLFIELD}                                                              
For most stars the source of the proper motions and positions                   
is identical. In addition, data were taken from high proper motion              
surveys, in particular from the Luyten (LHS, NLTT, L, and LP) and               
Giclas surveys, either via the SIMBAD data base or through data newly           
included in the INCA data base. These proper motions have relatively            
large errors, of the order of 0.02~arcsec per year. However, if they            
are used for stars whose positions were newly obtained either by plate          
measurements (mean epoch around 1976) or by meridian circle                     
observations (mean epoch 1986), the final accuracy obtained at epoch            
1990 for the input to the Hipparcos observations (Jahrei\ss~ 1989) was          
still within the margin tolerated by the satellite operation                    
requirements.                                                                   
                                                                                
\medskip                                                                        
Consistency checks were performed when independent                              
machine-readable positions were available for epochs sufficiently well          
separated in time, and some new proper motions were individually                
computed using first epoch positions from the Astrographic Catalogue            
(AC, see van Biesbroeck 1963). About 4\,000 entries of                          
the Hipparcos Input Catalogue remain without known proper motions.              
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section* {Fields 25-31: Photometry}                                            
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{25}{Magnitude in the Hipparcos photometric system, $\HP$}               
%++++++++++++++++++++++++                                                       
                                                                                
The `Hipparcos magnitude', designated as $\HP$, is defined                      
by the pass-band of the Hipparcos main detection                                
chain, which ranges from 340 to 850~nm. This broad-band system yields           
magnitudes close to the visual $V$ magnitude, but                               
shows residuals with respect to $V$ especially for red stars. For the           
prediction of the $\HP$ magnitude with the specified accuracy (necessary for    
the optimum allocation of satellite observing time, which varies strongly       
with magnitude especially towards the fainter stars), it was necessary to       
obtain both a magnitude and a colour index for each programme star.             
Transformation formulae were established to obtain $\HP$                        
from the magnitudes and colours available or newly observed in                  
various photoelectric systems (Grenon 1988b). $\HP$                             
magnitudes given in the Input Catalogue have been derived using                 
on-ground calibration of the detection chain and preliminary                    
transformation formulae (which will be refined for the derivation of            
the $\HP$ magnitudes from the satellite data). An                               
approximate relation valid for O-F stars and G-K giants in terms of the         
Johnson $V$ magnitude and $B-V$ colour index is:                                
\[ \HP = V + 0.408(B-V) - 0.130(B-V)^2 \]                                       
For variable stars, further information is given in field~26,                   
and in fields 39-44.                                                            
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{26, 1st character}{Variability code}                                    
%++++++++++++++++++++++++                                                       
                                                                                
The variability code provides information on known or suspected                 
variable stars. Table~V1 \ref{table:V1} lists the possible values               
(all amplitudes are in $\HP$):                                                  
                                                                                
                                                                                
\begin{SMALLFIELD}                                                              
\begin{table}[htb]\vspace{0.5cm}                                                
\CENTER {Table V1: Variability code}\label{table:V1}                            
\vspace{0.5cm}\centering                                                        
\begin{tabular}{rl} \hline \\                                                   
blank & the star is not a known or suspected variable\\                         
1 & suspected variable, with a suspected amplitude variation smaller than       
2~mag\\                                                                         
2 & suspected variable, with a suspected amplitude variation larger than 2~mag\\
3 & known variable, with an amplitude variation larger than 0.2 mag\\           
4 & known variable, with large amplitude ($> 2$ mag) for which an ephemeris\\   
  & was necessary\\                                                             
5 & known variable, with an amplitude variation smaller than 0.2 mag\\          
\FINTABLE                                                                       
                                                                                
Details of the treatment of variable stars within the Hipparcos                 
programme have been given by Mennessier \& Figueras (1989) and                  
Mennessier \ETAL\ ~(1992).                                                      
                                                                                
\medskip                                                                        
A blank field (not a known or suspected variable) does not mean                 
that the star is {\it not} variable. The only stars                             
known to be not variable at the level of about 0.02 mag are those with          
a flag C as photometric standard stars, as described by the second              
character of field~26. Some stars were suspected variable by some               
observers, while subsequent observations have suggested that they are           
very stable. For such stars, their variability code may not be blank            
even though they are classified as photoelectric standard stars.                
                                                                                
\medskip                                                                        
Code `3': stars in this category have been assigned a unique                    
magnitude for the purposes of the Hipparcos observations, despite their         
(possibly large) amplitude variation. The definition of this unique             
magnitude depends on the type of variability (it may correspond to the          
maximum or minimum, or to a mean or weighted magnitude) and is                  
specified by the second character of field~44.                                  
                                                                                
\medskip                                                                        
Code `4': for these large-amplitude variable stars, the use                     
of an ephemeris was necessary for specifying the observing time to be           
allocated to the Hipparcos observations. In this case, a weighted               
magnitude is given in field~25. As specified by the second character of         
field~44, the weighted magnitude used for stars in this category                
corresponds to:                                                                 
\CENTER{[$0.33\times$ magnitude at maximum luminosity $+ 0.67\times$            
magnitude at minimum luminosity].}                                              
                                                                                
%\medskip                                                                       
Code `5': these stars, for which the amplitude of variation                     
is smaller than 0.2 mag, are processed in the same way as non-variable          
stars.                                                                          
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{26, 2nd character}{Photoelectric standard stars}                        
%++++++++++++++++++++++++                                                       
                                                                                
Two categories of photoelectric standards are                                   
distinguished:                                                                  
\begin{LISTONE}                                                                 
\item[\BPIT{C}] the star is a photoelectric standard with confirmed             
     long-term stability (with three or more independent measurements over      
     several years);                                                            
\item[\BPIT{S}] the star is a secondary photoelectric standard star             
     (based on two independent measurements).                                   
\end{LISTONE}                                                                   
                                                                                
\begin{SMALLFIELD}                                                              
The photometric accuracies required for a programme star to be                  
considered as a photometric standard range from 0.020 to 0.026 mag              
(standard error depending on the $\HP$                                          
magnitude, Grenon 1989b). The photoelectric standard stars are used to          
calibrate the magnitudes derived from the detection chains of the main          
mission (Hipparcos magnitude, $\HP$) and of the Tycho experiment                
($\BT$ and $\VT$ magnitudes), and for monitoring the detector responses         
(including their colour dependence), the linearity of these responses,          
and their evolution throughout the mission (Grenon 1985b, 1989b). In            
the final version of the Hipparcos Input Catalogue, there are 10\,822 C         
stars and 3\,068 S stars.                                                       
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{27}{$V$ magnitude}                                                      
%++++++++++++++++++++++++                                                       
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{28}{Error of $V$ magnitude}                                             
%++++++++++++++++++++++++                                                       
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{29}{$B-V$}                                                              
%++++++++++++++++++++++++                                                       
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{30}{Error of $B-V$}                                                     
%++++++++++++++++++++++++                                                       
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{31}{Source of photometry}                                               
%++++++++++++++++++++++++                                                       
                                                                                
The photometric data given in the Hipparcos Input Catalogue                     
are derived from a wide variety of sources. The correspondence between          
the letters used in field~31 and the source of the photometry, along            
with the number of stars whose photometry was taken from this source,           
is given in Table~B2. \ref{table:B2}                                            
                                                                                
\begin{SMALLFIELD}                                                              
\DEBTABLE{Table B2: Source of photometry}{B2}                                   
A & Photographic $B$ or $V$ from SIMBAD or proposers; colour from               
spectral type & 45\,445\\                                                       
C & $V$ magnitude derived from CAMC; colour estimated from spectral             
type & 13\,315\\                                                                
D & Joint systems (double or multiple) with combined or joint                   
magnitude and colour & 8\,009\\                                                 
P & Photoelectric photometry from GCPD, new                                     
measurements or proposers & 44\,634\\                                           
V & Variable stars (amplitude larger than 0.2 mag) & 2\,165\\                   
X & Miscellaneous & 4\,641 \\                                                   
\FINTABLE                                                                       
                                                                                
Stars were proposed for Hipparcos observation on the grounds of                 
their scientific interest, irrespective of the accuracy of available            
data on position or photometry. The photometric data given by the               
proposers were taken either from the SIMBAD data base or from various           
sources of very heterogeneous quality. Of the 214\,000                          
proposed stars, $UBV$ photoelectric photometry was                              
available for about 26\,000 stars, while approximate                            
photographic photometry was available for about 32\,000 other stars.            
In addition, it was possible to derive acceptable $B$ and $V$                   
magnitudes from the available estimates of blue and visual magnitudes           
for some 139\,000 stars. For the remaining 17\,000 stars, the                   
photometric information was not reliable. These stars belonged                  
primarily to the faint end of the proposed programmes.  The                     
observational effort was concentrated on stars having a high                    
probability of being finally retained in the Input Catalogue                    
considering the results of the successive numerical simulations of the          
mission. The observing lists were updated after each simulation.                
                                                                                
As for positional data, the data given in fields 25-31 are the                  
result of extensive compilations (Mermilliod \& Mermilliod 1985; Egret          
1985; Grenon 1989a), and new observations (Grenon 1985a, 1988a, 1988b;          
Torra \ETAL\ 1988). The photometric contents of the INCA data base,             
initially identical to those of SIMBAD, were updated in successive              
steps:                                                                          
                                                                                
\begin{itemize}                                                                 
\item compilation of photoelectric multi-colour photometry.                     
      This work was prepared in Lausanne and Geneva (Mermilliod \& Mermilliod   
      1985; Grenon 1989a) within the framework of the updating of the General   
      Catalogue of Photometric Data (GCPD, Hauck \ETAL\ 1990). $B$              
      and $V$ magnitudes (Johnson system) and the $\HP$                         
      magnitudes were computed from the data collected in the GCPD              
      for various multi-colour photometric systems after a determination of     
      the transformation formulae from these systems to the Johnson and         
      Hipparcos systems (Grenon 1985b). Identifiers used in the GCPD were       
      incorporated into the INCA data base, facilitating the inclusion of       
      the $B$, $V$ and $\HP$ magnitudes;                                        
                                                                                
%                                                                               
\vfill\eject                                                                    
%                                                                               
                                                                                
\item new observations in photoelectric multi-colour                            
      photometry.  This work was organised in Geneva (Grenon 1985a, 1988a,      
      1988b, 1989a) in order to obtain a Hipparcos magnitude and a colour for   
      all stars for which the available data were not reliable, and in order    
      to perform ground-based observations as far as possible complementary     
      to the outputs expected from Hipparcos and Tycho. The observations were   
      made using multi-colour photometry, with the system selected according    
      to the spectral type in order to be able to derive some basic physical    
      parameters (such as $T_{\rm eff}$, $\log g$, [M/H]) in addition to the    
      magnitudes. The selection was made as follows (Grenon 1985a):             
                                                                                
\begin{tabbing}                                                                 
Spectral type:~~~\=~~~\=~~~O~~~\=~~~B5~~~\=~~~AF~~~\=~~~G2~~~\=~~~G5~~~         
\=~~~K0~~~\=~~~K5~~~\=~~~M~~~\=~~~RNC~~~\=~~~\\                                 
\>\underline{$|~~~~~~UBV~~~~~~|$}\>~                                            
\>~\>~\>~\>~\>\underline{$|~~~~~UBV~~~~~|$}\\                                   
\>~\>~\>\underline{$|~~~~~~~~~~~~$Str\"omgren$~~~~~~~~~~~~~|$}\\                
\>~\>~\>\underline{$|~~~~~~~$Walraven$~~~~~~~|$}                                
\>~\>~\>~\>~\>\underline{$|~~~~~~~~~~~~VRI~~~~~~~~~~~~|$}\\                     
\>~\>~\>\underline                                                              
{$|~~~~~~~~~~~~~~~~~~~~~~~~$Geneva$~~~~~~~~~~~~~~~~~~~~~~~~|$}\\                
\end{tabbing}                                                                   
      All observations were published separately, and only the                  
      resulting $\HP$, $V$ and                                                  
      $B-V$ magnitudes are given here. They represent the result of             
      the combined effort of astronomers from Belgium, Denmark, France,         
      Germany, The Netherlands, Spain and Switzerland (Grenon 1989a). The       
      data were introduced into the INCA data base following the same           
      procedure as for the compiled photoelectric data described above. Among   
      these new observations, special mention should be made of the visual      
      magnitudes obtained by the Carlsberg Automatic Meridian Circle at La      
      Palma: it provides magnitudes in a band similar to the Johnson $V$        
      and with an accuracy only slightly lower than that achieved               
      with classical photometric techniques. The magnitudes published in the    
      Carlsberg Catalogues Vols 1-3 (1985, 1986, 1987) were reduced to          
      Johnson $V$ using a colour term derived from the spectral                 
      type, and were retained when no other photoelectric data were             
      available;                                                                
\item improvement of non-photoelectric data. For the                            
      remaining stars, data from the SIMBAD data base or from the original      
      programmes proposed for Hipparcos observation were used as a basis. The   
      magnitudes available in SIMBAD are the result of a hierarchy of           
      catalogue sources and of a unification of systems performed by            
      Ochsenbein (1974). When the sources available for both $B$                
      and $V$ magnitudes were not identical, the more reliable                  
      magnitude was retained, and the colour of the stars was computed from     
      the spectral type and a newly-derived extinction model (Arenou            
      \ETAL\ 1992);                                                             
\item for components of double and multiple systems, the                        
      photometric data were derived as described above when the components      
      are processed as single stars (i.e. systems with separation smaller       
      than 3 arcsec or systems with secondary components that have a            
      negligible impact on the quality of the Hipparcos observations). In the   
      other cases, new compilations (Oblak \& Mermilliod 1988) and new          
      observations (Oblak 1988, Argue \& Irwin 1988) were performed. Some       
      magnitudes were taken from the GSC (Lasker \ETAL\ 1990). In the absence   
      of additional data, the magnitudes were taken from the preliminary        
      version of the CCDM, which were, in turn, taken from the Index            
      Catalogue of Visual Double Stars (IDS, Jeffers \ETAL\ 1963).  Most        
      often the CCDM magnitudes are visual estimates but, especially for the    
      faintest systems, they may be photographic. The `magnitude difference'    
      given in field~49 was computed from the CCDM, and may not be consistent   
      with data given in field~27 for the separate components.                  
\end{itemize}                                                                   
                                                                                
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section* {Fields 32-33: Spectral Type}                                         
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{32}{Spectral type and luminosity class}                                 
%++++++++++++++++++++++++                                                       
                                                                                
Spectral types were taken either from SIMBAD or from other                      
miscellaneous sources, and thus follow various classification systems           
(MK, HD, etc). In the case of the MK classification system of Morgan            
\ETAL\ (1943), the spectral type, luminosity class, and peculiarity code        
are given with the following designations:                                      
                                                                                
\begin{itemize}\itemsep=-4pt                                                    
\item O, B, A, F, G, K, M plus sub-type (0, 1, etc), and                        
      sometimes intermediate sub-type (for example F7.2, F7.5, F7.7) for the    
      spectral types of `normal stars';                                         
\item R, S, N, C ~for carbon stars;                                             
\item DB, DA, DF, DG ~for white dwarfs;                                         
\item WR, WN, WC ~for Wolf-Rayet stars;                                         
\end{itemize}                                                                   
                                                                                
\medskip\noindent                                                               
For luminosity class, the following designations are used:                      
Ia0, Ia, Iab, Ib for supergiants, II for bright giants, III for giants,         
IV for sub-giants, V for dwarfs. The sub-dwarfs are either noted                
{\small\bf sd} followed by the spectral type, or class VI.                      
                                                                                
\medskip                                                                        
Peculiarities of the spectra are noted in lower case letters ({\small\bf        
e} for emission lines, {\small\bf m} for enhanced metallic lines, {\small\bf    
n} for nebulous lines, {\small\bf nn} for very nebulous, {\small\bf p} for      
peculiarity in the chemical composition, {\small\bf s} for sharp lines,         
{\small\bf sh} for the existence of a shell, {\small\bf v} for variations in    
the spectrum, {\small\bf w} for weak lines, etc).                               
{\small\bf CN} indicates stars with an anomaly in the cyanogen abundance.       
                                                                                
\medskip                                                                        
The following signs are also used:                                              
                                                                                
\medskip                                                                        
                                                                                
\makebox[1.5cm][l]{{\bf :}} indicates some doubt about the determination        
           of the spectral type or luminosity class;                            
                                                                                
\makebox[1.5cm][l]{{\bf /}} between two spectral types or luminosity            
         classes indicates Survey;                                              
                                                                                
\makebox[1.5cm][l]{{\bf -}} between two spectral types or luminosity            
         classes indicates that the parameter is                                
                                                                                
\makebox[2.5cm][l]{}      intermediate between those given;                     
                                                                                
\makebox[1.5cm][l]{{\bf +...}} indicates composite spectra (the second          
        spectrum is no given);                                                  
                                                                                
\makebox[1.5cm][l]{{\bf ...}} indicates truncated spectra (the source           
        catalogue gives more details on the spectra,                            
                                                                                
\makebox[2.5cm][l]{}      such as peculiarities).                               
                                                                                
                                                                                
\begin{SMALLFIELD}                                                              
In the INCA data base, the spectral types were initially taken                  
from the SIMBAD data base or from the original proposal when the data           
were not available in SIMBAD. The spectral types available in SIMBAD in         
1985, at the time of creation of the INCA data base, were mainly taken          
from the Michigan Spectral Survey (Houk \& Cowley 1975; Houk 1978,              
1982). Volume~4 of the MSS (Houk \& Smith-Moore 1988) was made available        
to the INCA Consortium in advance of publication by courtesy of N.              
Houk, and integrated into the INCA data base in 1988. For variable              
stars, many spectral types were taken from the Fourth Edition of the            
General Catalogue of Variable Stars (GCVS, Kholopov 1985, 1987).                
Furthermore, many additions and corrections were made from the various          
programmes proposed for Hipparcos observation, or from individual               
searches in the literature. Confidence tests were performed from a              
correspondence between the spectral types and the colour index when             
both $B$ and $V$ magnitudes were considered reliable,                           
and many resulting corrections were made either to the spectral types           
or to the photometric data.                                                     
                                                                                
The above description does not cover all MK designations which                  
may be found in field~32. A more complete description, with the                 
criteria used for classification, can be found in the introduction to           
the Michigan Spectral Survey.                                                   
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{33}{Source of the spectral type data}                                   
%++++++++++++++++++++++++                                                       
                                                                                
The spectral type and luminosity class information in the Hipparcos             
Input Catalogue is derived from a variety of sources. The                       
correspondence between the letters used in field~33 and the source of           
the data, along with the number of stars whose data was taken from this         
source, is given in Table~B3. \ref{table:B3}                                    
                                                                                
\begin{SMALLFIELD}                                                              
\DEBTABLE{Table B3: Source of spectral types}{B3}                               
1 & Michigan Spectral Survey, Vol. 1 (Houk \& Cowley 1975) & 12\,348\\          
2 & Michigan Spectral Survey, Vol. 2 (Houk 1978) & 9\,375\\                     
3 & Michigan Spectral Survey, Vol. 3 (Houk 1982) & 11\,232\\                    
4 & Michigan Spectral Survey, Vol. 4 (Houk \& Smith-Moore 1988) & 10\,304\\     
K & Fourth Edition of the General Catalogue of Variable Stars (GCVS) & 929\\    
S & SIMBAD & 57\,081\\                                                          
X & Miscellaneous & 13\,993\\                                                   
  & [Entry without corresponding information] & [2\,947]\\                      
\FINTABLE                                                                       
 ~                                                                              
\end{SMALLFIELD}                                                                
                                                                                
%                                                                               
\vfill\eject                                                                    
%                                                                               
                                                                                
%-------------------------------------------------                              
\section* {Fields 34-36: Parallax}                                              
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{34}{Parallax}                                                           
%++++++++++++++++++++++++                                                       
                                                                                
The parallax is expressed in units of milli-arcsec.                             
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{35}{Probable error of parallax}                                         
%++++++++++++++++++++++++                                                       
                                                                                
The probable error of the (trigonometric) parallaxes is                         
expressed in units of milli-arcsec. No errors are quoted for the                
dynamical parallaxes.                                                           
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{36}{Type of parallax}                                                   
%++++++++++++++++++++++++                                                       
                                                                                
The following abbreviations are used: `T' for                                   
trigonometric, `D' for dynamical.                                               
                                                                                
\begin{SMALLFIELD}                                                              
There are 5\,485 trigonometric parallaxes in the                                
Input Catalogue, which were taken, via SIMBAD, from the General                 
Catalogue of Trigonometric Parallaxes (Jenkins 1952) and its supplement         
(Jenkins 1963). There are also 389 dynamical parallaxes, taken from             
Dommanget (1967) and Dommanget \& Nys (1982). Since the New General             
Catalogue of Trigonometric Parallaxes (van Altena \ETAL, in                     
preparation) was not available at the time of publication of the Input          
Catalogue, no more recent parallaxes are given here.                            
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section* {Fields 37-38: Radial Velocity}                                       
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{37}{Radial velocity}                                                    
%++++++++++++++++++++++++                                                       
                                                                                
The radial velocity is expressed in units of km/s (with                         
positive values indicating recession).                                          
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{38, 1st character}{Quality of radial velocity}                          
%++++++++++++++++++++++++                                                       
                                                                                
The `quality' given in this field~is derived from information in                
the GCRV (Wilson 1953) and the catalogue of Evans (1978), according to          
which the estimated mean probable errors are `{\it based upon three             
factors: the number of observations, the dispersion of the                      
spectrograph used, and the interagreement of separate determinations}'.         
The radial velocities are characterised by five such values:                    
\begin{LISTONE}                                                                 
\item[\BPIT{a}] 0.5 km/s                                                        
\item[\BPIT{b}] 1.2 km/s                                                        
\item[\BPIT{c}] 2.5 km/s                                                        
\item[\BPIT{d}] 5 km/s                                                          
\item[\BPIT{e}] not given                                                       
\end{LISTONE}                                                                   
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{38, 2nd character}{Source of radial velocity}                           
%++++++++++++++++++++++++                                                       
                                                                                
There are three principal sources of radial velocity data used                  
in the present compilation: the General Catalogue of Stellar Radial             
Velocities (Wilson 1953) and the catalogue of Evans (1978), both                
accessed via the SIMBAD data base, and the catalogue of Barbier-Brossat         
(1989) which was later included in the INCA data base. The                      
correspondence between the letters used in this field and the source of         
the data, along with the number of stars whose radial velocity was              
taken from this source, is given in Table~B4. \ref{table:B4}                    
                                                                                
\begin{SMALLFIELD}                                                              
\DEBTABLE{Table B4: Source of radial velocities}{B4}                            
 B  &  Barbier-Brossat (1989) & 4\,094 \\                                       
 E  &  Evans (1978) & 4\,866 \\                                                 
 W  &  GCRV (Wilson 1953) & 9\,616 \\                                           
 X  &  Miscellaneous & 899 \\                                                   
\FINTABLE                                                                       
                                                                                
The data given here are very incomplete as they do not                          
include most radial velocities obtained by cross-correlation methods            
(not yet published or published in small lists). Furthermore, they do           
not include the results of the ongoing observations organised in                
parallel with the work of preparation of the Hipparcos Input Catalogue.         
In the northern hemisphere, a radial velocity programme for early-type          
stars brighter than $m_{\rm pg} = 9.0$ mag                                      
has been in progress since mid-1982 using objective-prism techniques            
and a slit spectrograph (Fehrenbach \& Burnage 1985; Grenier 1988;              
Burnage \ETAL\ 1988). In the southern hemisphere, three ESO                     
key-programmes have been in progress since the end of 1988, two for             
early-type stars (one for stars nearer than 100pc, one for stars in OB          
and early-A associations), and one for late-type stars using the                
Coravel spectrometer (one measurement has already been obtained for             
each of the 20\,000 or so stars on the observing                                
programme). These three programmes are described by Gerbaldi \ETAL\             
(1990), Hensberge \ETAL\ (1990), and Mayor \ETAL\ (1990).                       
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section* {Fields 39-44: Variability}                                           
%-------------------------------------------------                              
                                                                                
\begin{SMALLFIELD}                                                              
Variable stars, especially those with large amplitude, raise                    
specific problems for the Hipparcos observations. The optimum `target           
observing time' is determined from the Hipparcos magnitude, and this            
observing time varies strongly as a function of magnitude. The                  
allocation of excessive observing time to a star is inefficient, while          
allocating too short an observing time would result in less accurate            
astrometric parameters at the end of the mission (Mennessier \& Baglin          
1988). Ephemerides are therefore used for large-amplitude variable              
stars, while a unique magnitude is chosen for the others (Mennessier            
1985). The limiting amplitude for requiring the use of ephemerides was          
taken as $\Delta \HP = 2$ mag. For stars                                        
with a smaller amplitude, a unique magnitude was chosen according to            
the type of variability. The choice is indicated as a code in the               
second character of field~44.                                                   
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{39}{Variable star name}                                                 
%++++++++++++++++++++++++                                                       
                                                                                
The names of the variable stars are taken from the Fourth                       
Edition of the General Catalogue of Variable Stars (GCVS, Kholopov              
1985, 1987) or, where the NSV number is given, from the New Catalogue           
of Suspected Variable Stars (Kholopov 1982). The names were included in         
the INCA data base from SIMBAD, and some cross-identifications were             
corrected.                                                                      
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{40}{Type of variability}                                                
%++++++++++++++++++++++++                                                       
                                                                                
The data on variability type are taken from the GCVS and NSV                    
Catalogues (see field~39). The abbreviations given in Table~V2 \ref{table:V2}   
follow the main classes of variability (eruptive, pulsating, rotating,          
cataclysmic, eclipsing, and X-ray variable stars). If the 3-letter code used    
here is an abbreviation of the type of variability given in the two source      
catalogues, the complete designation is given in Table~V2 \ref{table:V2}        
\RPAGE{table:V2} between brackets.                                              
                                                                                
                                                                                
\begin{SMALLFIELD}                                                              
\begin{table}[p]\vspace{0.5cm}                                                  
\CENTER {Table V2: Types of variability}\label{table:V2}                        
\vspace{0.5cm}\centering                                                        
\begin{tabular}{lll} \hline \\                                                  
Code & \multicolumn{1}{c}{Description} & Class of Variability\\ \\              
\hline \\                                                                       
ACV & $\alpha^2$ Canum Venaticorum variables & rotating variable \\             
ACY & $\alpha$ Cygni variables (ACYG) & pulsating variable \\                   
BCE & $\beta$ Cephei variables (BCEP) & pulsating variable \\                   
BY & BY Draconis variables & rotating variable \\                               
CEP & Cepheids & pulsating variable \\                                          
CST & constant stars (formally believed variable by some observer) & \\         
CW & W Virginis variables & pulsating variable \\                               
CWA & W Virginis variables (periods $>8$ days) & pulsating variable \\          
CWB & W Virginis variables (periods $<8$ days) & pulsating variable \\          
DCE & $\delta$ Cephei variables (DCEP and DCEPS) & pulsating variable \\        
DSC & $\delta$ Scuti variables (DSCT and DSCTC) & pulsating variable \\         
E & (E+, E/ ..) & eclipsing binary \\                                           
EA & Algol type (EA+, EA/ ..) & eclipsing binary \\                             
EB & $\beta$ Lyrae type (EB/ ..) & eclipsing binary \\                          
ELL & rotating ellipsoidal variables (ELL+.. or /..) & rotating variable \\     
EW & W Ursae Majoris type (EW/ ..) & eclipsing binary \\                        
FKC & FK Comae Berenices variables (FKCOM) & rotating variable \\               
GCA & $\gamma$ Cassiopeiae variables (GCAS) & eruptive variable \\              
I & irregular variables (I, IA, In, InT, Is) & eruptive variable \\             
IN & irregular variables (INA, INAT, INB, INSA, INSB, INST, INT) & eruptive     
variable \\                                                                     
IS & irregular variables (ISA, ISB) & eruptive variable \\                      
L & slow irregular variables (L, LB, LC) & pulsating variable \\                
M & Mira Ceti variables & pulsating variable \\                                 
NA & fast novae & cataclysmic variable \\                                       
NB & slow novae & cataclysmic variable \\                                       
NC & slow novae & cataclysmic variable \\                                       
NL & nova-like variables & cataclysmic variable \\                              
NR & recurrent novae & cataclysmic variable \\                                  
PVT & PV Telescopii type (PVTEL) & pulsating variable \\                        
RCB & R Coronae Borealis type & eruptive variable \\                            
RR & RR Lyrae type (RR, RRAB, RRC) & pulsating variable \\                      
RS & RS Canum Venaticorum type & eclipsing binary \\                            
RV & RV Tauri type (RV, RVA, RVB) & pulsating variable \\                       
SDO & S Doradus type (SDOR) & eruptive variable \\                              
SR & semi-regular variables (also SRA, SRB, SRC, SRD) & pulsating variable \\   
SXA & SX Arietis type (SXARI) & rotating variable \\                            
SXP & SX Ph{\oe}nicis type & pulsating variable \\                              
UGS & SS Cygni type (UGSS) & cataclysmic variable \\                            
UV & UV Ceti type & eruptive variable \\                                        
WR & Wolf-Rayet variables & eruptive variable \\                                
XNG & X-ray nova-like system & X-ray binary \\                                  
XP & X-ray pulsar & X-ray binary \\                                             
ZAN & Z Andromedae type (ZAND) & cataclysmic variable \\                        
ZZA & Hydrogen ZZ Ceti type & pulsating variable \\                             
\FINTABLE                                                                       
 ~                                                                              
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{41}{Period of variation}                                                
%++++++++++++++++++++++++                                                       
                                                                                
The period of variation is expressed in days.                                   
                                                                                
\begin{SMALLFIELD}                                                              
The data are taken from the GCVS and NSV Catalogues (see field                  
39). In the GCVS, the dates of the last observed maxima or minima are           
also given for most stars.                                                      
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{42}{$V$ magnitude at maximum luminosity}                                
%++++++++++++++++++++++++                                                       
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{43}{$V$ magnitude at minimum luminosity}                                
%++++++++++++++++++++++++                                                       
                                                                                
\begin{SMALLFIELD}                                                              
For observations with Hipparcos, and for the preparatory                        
numerical simulations of the mission, $\HP$                                     
magnitudes at maximum and minimum luminosities were computed from the           
available luminosity curves (Mennessier \& Figueras 1989).  However, it         
was considered more useful to the future user to give here the $V$              
magnitudes at maximum and minimum luminosities, rather than                     
the $\HP$ magnitudes. These magnitudes are those                                
of the GCVS except for some stars for which more precise observations           
were available, and for the Mira stars. Indeed the GCVS gives the               
maximum and minimum magnitudes observed for each star. Due to the               
significant variability of Miras from one cycle to another one, it was          
considered more appropriate to give here the mean magnitudes of the             
luminosity extrema. A comparison of GCVS magnitudes with the mean               
magnitudes of the luminosity extrema, obtained from 30 years of                 
observation for about 200 Miras by Campbell (1955), gives the following         
statistical relations (where $P$ is the period, and                             
$V_{\rm GCVS(max)}$ and $V_{\rm GCVS(min)}$ are the magnitudes at maximum       
and minimum luminosities given in the GCVS respectively):                       
\[                                                                              
\begin{array}{lcl}                                                              
V_{\rm mean~at~maximum} &=& V_{\rm GCVS(max)} + 0.32 + 0.11{P\over100}\\        
V_{\rm mean~at~minimum} &=& V_{\rm GCVS(max)} - 0.6                             
\end{array}                                                                     
\]                                                                              
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{44, 1st character}{Coded error of $V$ magnitude at maximum/minimum      
luminosity}                                                                     
%++++++++++++++++++++++++                                                       
                                                                                
This code gives an estimation of the accuracy of the $V$ magnitudes at          
maximum and minimum luminosity given in fields 42 and 43. This estimate         
includes the errors of individual measurements and the possible                 
variability of the maxima and minima. This information is given for             
stars with a variability code of 3 or 4 (as specified by the first              
character of field~26), whenever the necessary information on the               
luminosity curve was available. The code can take the values given in           
Table~V3. \ref{table:V3}                                                        
                                                                                
\begin{SMALLFIELD}                                                              
\begin{table}[htb]\vspace{0.5cm}                                                
\CENTER {Table V3: Coded error of the $V$ magnitudes}\label{table:V3}           
\vspace{0.5cm}\centering                                                        
\begin{tabular}{rl} \hline \\                                                   
1 & $\le 0.2$ mag\\                                                             
2 & $0.2 - 0.5$ mag\\                                                           
3 & $0.5 - 1.0$ mag\\                                                           
4 & $\ge 1.0$ mag\\                                                             
\FINTABLE                                                                       
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{44, 2nd character}{Code specifying the magnitudes and colour given in   
fields 25, 27, 29}                                                              
%++++++++++++++++++++++++                                                       
                                                                                
The choice of the unique magnitude used for the determination of the            
target observing time with Hipparcos depends on the shape of the                
luminosity curve of each type of variable star. It can be the magnitude         
at minimum or maximum luminosity, a mean, or a weighted magnitude               
(Mennessier \& Figueras 1989). This information is given for stars with         
a variability code of 3 or 4 (as specified by the first character of field      
26), whenever the necessary information on the luminosity curve was             
available. It is coded as given in Table~V4. \ref{table:V4}                     
                                                                                
\begin{SMALLFIELD}                                                              
\begin{table}[htb]\vspace{0.5cm}                                                
\CENTER {Table V4: Magnitudes and colours given in fields 25, 27,               
29}\label{table:V4}                                                             
\vspace{0.5cm}\centering                                                        
\begin{tabular}{rl} \hline \\                                                   
Code & \multicolumn{1}{c}{magnitude used}\\ \\ \hline \\                        
1 &  magnitude at minimum luminosity\\                                          
2 &  magnitude at maximum luminosity\\                                          
3 &  mean magnitude\\                                                           
4 &  weighted magnitude (0.33 max + 0.67 min) for most                          
pulsating stars\\                                                               
5 &  weighted magnitude (0.85 max + 0.15 min) for eclipsing systems\\           
\FINTABLE                                                                       
\end{SMALLFIELD}                                                                
                                                                                
\vfill\eject                                                                    
                                                                                
%-------------------------------------------------                              
\section* {Fields 45-50: Multiplicity}                                          
%-------------------------------------------------                              
                                                                                
For double or multiple systems for which one or more                            
components are contained in the Hipparcos observing programme (see              
fields 2-3), fields 45-50 provide concise information (position angle,          
separation and                                                                  
magnitude difference, when available) describing the system.                    
                                                                                
\medskip                                                                        
The values given in fields 47-49 refer to the two components                    
specified in field~46. If the entry is a primary component, fields 46           
to 49 are blank.                                                                
                                                                                
\medskip                                                                        
The CCDM and HIC numbers provide the link between the main catalogue            
and Annex~1. More comprehensive explanations and data on the relevant           
double and multiple systems, and details of the data contained in these         
fields, are given in Annex~1.                                                   
                                                                                
\medskip                                                                        
The data given in fields 45-50 are taken from a provisional                     
version of the `Catalogue of the Components of Doubles and Multiple             
Stars' (CCDM, Dommanget \ETAL, in preparation).                                 
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{45}{CCDM number}                                                        
%++++++++++++++++++++++++                                                       
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{46}{Components considered}                                              
%++++++++++++++++++++++++                                                       
                                                                                
The first letter corresponds to the `reference' component,                      
with respect to which the separation and difference of magnitude are            
computed.                                                                       
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{47}{Position angle (degrees) between the components considered}         
%++++++++++++++++++++++++                                                       
                                                                                
Letters such as `NF', `SP' may be used.                                         
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{48}{Separation (arcsec) between the components considered}              
%++++++++++++++++++++++++                                                       
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{49}{Magnitude difference between the components considered}             
%++++++++++++++++++++++++                                                       
                                                                                
The `magnitude difference' given in this field is                               
computed from the available provisional version of the CCDM. It may not         
be consistent with data given in field~27 for separate components. If           
the `reference' component is fainter than the second one, this                  
difference is negative.                                                         
                                                                                
%                                                                               
\vfill\eject                                                                    
%                                                                               
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{50}{Information on orbital systems}                                     
%++++++++++++++++++++++++                                                       
                                                                                
The characters in this field have the following meaning:                        
\begin{LISTONE}                                                                 
\item[\BPIT{O}] the orbit of the system is known.                               
\item[\BPIT{A}] the star is a known astrometric binary.                         
\item[\BPIT{*}] the astrometric binary is also a member of an orbital system    
(details are given in Annex~1).                                                 
\end{LISTONE}                                                                   
                                                                                
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section* {Fields 51-60: Identifications}                                       
%-------------------------------------------------                              
                                                                                
                                                                                
\begin{SMALLFIELD}                                                              
During the preparation of the Hipparcos Input Catalogue,                        
numerous cross-identifications and systematic checks of these                   
identifications were carried out, resulting in many individual                  
corrections being included in the INCA data base. The basic initial             
material was taken from the SIMBAD data base. Some of the most                  
important identifiers are given here. The order adopted for the choice          
of identifications reflects the nature of the stars included in the             
Hipparcos observing programme (e.g. catalogues of nearby stars, of high         
proper motion stars, etc.).                                                     
                                                                                
\medskip                                                                        
In the following format descriptions, NNN... denotes a running                  
number; HH, DD, and MM (and MM.m) denote hours, degrees and minutes             
respectively; LLL and BB denote galactic longitude and latitude                 
respectively; VV (and VV.v) denote `volume'; ZZ indicates the                   
declination zone; FFF... denotes a `field' number;                              
and A indicates a component.                                                    
                                                                                
\medskip                                                                        
In case of joint entry, the identifier with the `smaller'                       
running number is given, irrespective of the brightness of the                  
components (e.g.~BD +50 222 is given, not BD +50 223; Mel 22 800 is given, not  
Mel 22 801; GL NNNA is given, not GL NNNB).                                     
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{51}{BD number}                                                          
%++++++++++++++++++++++++                                                       
                                                                                
The format is $\pm$ ZZ NNNNa. The last character of this field is used for      
additional BD stars, i.e. stars with suffix `a' or `b' (these stars were added  
to the BD Catalogue after the original numbering was made). Such                
identifications do not imply that the entry is a component of a double or       
multiple system.                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{52}{CD number}                                                          
%++++++++++++++++++++++++                                                       
                                                                                
The format is $\pm$ ZZ NNNNN                                                    
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{53}{CPD number}                                                         
%++++++++++++++++++++++++                                                       
                                                                                
The format is $\pm$ ZZ NNNNN                                                    
                                                                                
\begin{SMALLFIELD}                                                              
\medskip                                                                        
Reliability tests were performed to check the coherence between                 
the zones of the DM (BD, CD, and CPD) numbers and the declination at the epoch  
of the catalogue (1855 for BD, 1875 for CD and CPD), and also to check that     
the numbers increased with increasing right ascension at the epoch of           
the catalogue. Resulting corrections (from typing errors in the numbers         
or in the coordinates, originating from the source catalogue themselves         
or from an intermediate transcription, or confusion between the CD and          
CPD identifiers) have been included in the Hipparcos Input Catalogue.           
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{54}{HD/HDE number}                                                      
%++++++++++++++++++++++++                                                       
                                                                                
Cross-identifications are given to stars in the HD Catalogue                    
(Cannon \& Pickering 1918-24, with numbers in the range 1-225\,300), and        
its two extensions: HDE numbers in the range 225\,301-272\,150 (Cannon          
1925-36) and 272\,151-359\,083 (Cannon \& Walton Mayall 1949) respectively.     
                                                                                
\begin{SMALLFIELD}                                                              
As for the DM identification numbers, reliability tests were                    
performed to check that the HD numbers increased with increasing right          
ascension at the epoch of the catalogue (1900). Resulting corrections           
have been included in the Hipparcos Input Catalogue. The format is              
NNNNNN.                                                                         
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{55}{FK5/FK5 Ext/FK4 Sup, or IRS (AGK3R/SRS) number}                     
%++++++++++++++++++++++++                                                       
                                                                                
Cross-identifications are given to stars in the Fifth                           
Fundamental Catalogue (FK5, Fricke \ETAL\ 1988), its extension (FK5             
Ext, Fricke \ETAL\  1991), the FK4 Supplement (FK4 Sup, Fricke 1963),           
and to the International Reference Stars (IRS), which comprises the             
AGK3R (Smith 1980) and SRS (Smith \ETAL\ 1990) Catalogues. Abbreviation,        
format, range, number of identifiers in the Hipparcos Input Catalogue are       
given for each catalogue, in Table~I1. \ref{table:I1}                           
                                                                                
\begin{SMALLFIELD}                                                              
\begin{table}[h] \vspace{0.5cm}                                                 
\CENTER {Table I1: FK4-FK5, IRS catalogues} \label{table:I1}                    
\vspace{0.5cm}                                                                  
\centering \begin{tabular}{clrrr} \hline \\                                     
Abbreviation & Catalogue & Format & Range &                                     
\multicolumn{1}{c}{No. of stars} \\ \\                                          
\hline \\                                                                       
A & AGK3R & NNNNN & 1-21\,499 & 19\,777\\                                       
F & FK5 & NNNN & 1- 1\,670 & 1\,535\\                                           
F & FK5 Ext & NNNN & 2\,001- 6\,125 & 3\,103\\                                  
K & FK4 Sup & NNNN & 2\,001- 3\,997 & 995\\                                     
S & SRS & NNNNN & 1-20\,495 & 15\,472\\                                         
\FINTABLE                                                                       
                                                                                
                                                                                
Cross-identifications are included according to the following                   
hierarchy: FK5, FK5 Ext, FK4 Sup, AGK3R, SRS (e.g. if the star                  
appears in both the AGK3R and SRS catalogues, only the AGK3R number is          
given). Note that the FK5 stars are identical to the FK4 stars. Stars           
with FK4 Sup numbers are not contained in the FK5 extension.                    
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{56}{AGK3/CPC number}                                                    
%++++++++++++++++++++++++                                                       
                                                                                
Cross-identifications are given to stars in the AGK3 Catalogue                  
for $\delta > -2.5\degr$ (Dieckvoss \ETAL\ 1975), and otherwise to              
stars in the CPC Catalogue (Jackson \& Stoy 1954-68). The format of each        
catalogue is given in Table~I2. \ref{table:I2}                                  
                                                                                
\begin{SMALLFIELD}                                                              
\begin{table}[h] \vspace{0.5cm}                                                 
\CENTER {Table I2: AGK3-CPC catalogues} \label{table:I2}                        
\vspace{0.5cm}                                                                  
\centering \begin{tabular}{lcrr} \hline \\                                      
Catalogue & \multicolumn{3}{c}{Format}\\ \\                                     
\hline \\                                                                       
AGK3 & $\pm$ & DD & NNNN\\                                                      
CPC & & VV & NNNNN\\                                                            
& or & VV.v & NNNNN\\                                                           
Other* & & 0 & NNNNN\\                                                          
\FINTABLE                                                                       
                                                                                
* Note that the CPC Catalogue does not cover the declination                    
zone $-40\degr > \delta > -52\degr$.                                            
Cross-identifications for stars in this interval are given following            
the system adopted within the SIMBAD data base: a zero (0) is                   
adopted in place of the volume number (in contrast to $\pm00$ for stars         
from the AGK3 with zero declination) with cross-identifications made to         
stars from this zone from the older Cape Zone Catalogue (Gill \& Hough          
1923). These numbers, in the range 1 - 20843, correspond to those also          
used by the Yale Photographic Catalogues (known as the `Yale Zone'              
Catalogue, YZ) in the zone                                                      
$-40\degr > \delta > -50\degr$ (YZ does not cover the declination zone          
$-50\degr > \delta > -60\degr$).                                                
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{57}{SAO number}                                                         
%++++++++++++++++++++++++                                                       
                                                                                
Cross-identifications are given to stars in the SAO Catalogue                   
(Smithsonian Institute 1966). The format is: NNNNNN.                            
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{58-59}{Other principal identifiers}                                     
%++++++++++++++++++++++++                                                       
                                                                                
These fields provide up to two of the identifiers: GL, GJ,                      
G, LHS, LTT, LP, L, BPM, CF, McC (according to this hierarchy).                 
Abbreviation, reference and format are given, for each catalogue, in Table~I3.  
\ref{table:I3}                                                                  
                                                                                
\begin{SMALLFIELD}                                                              
\begin{table}[h] \vspace{0.5cm}                                                 
\CENTER {Table I3: Abbreviations and format of catalogues used in fields 58 and 
59} \label{table:I3}                                                            
\vspace{0.5cm} \centering                                                       
\begin{tabular}{clll} \hline \\                                                 
Abbreviation & \multicolumn{1}{c}{Catalogue} & Reference & Format \\ \\         
\hline \\                                                                       
BPM & Bruce Proper Motion Survey & Luyten (1963) & NNNNN\\                      
CF & Cape Faint Stars & Spencer-Jones \& Jackson (1939) & NNNNN\\               
G & Lowell Proper Motion Survey & Giclas \ETAL\ (1959-78) & FFF-NNN\\           
GL & Catalogue of Nearby Stars & Gliese (1969) & NNNA or NNN.NA\\               
GJ & ~~~''~~~ extensions & Gliese \& Jahrei\ss~ (1979) & NNNNA\\                
L & Luyten Catalogue & Luyten (1942) & FFFF-NNNN\\                              
LHS & Luyten Half-Second Catalogue & Luyten (1979) & NNNN\\                     
LP & Luyten Palomar Survey & Luyten (1963-87) & FFFF-NNN\\                      
LTT & Luyten Two-Tenths Catalogue & Luyten (1957) & NNNNN\\                     
McC & McCormick Observatory & Vyssotsky (1943-58) & NNN\\                       
\FINTABLE                                                                       
 ~                                                                              
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{60}{Other identifiers}                                                  
%++++++++++++++++++++++++                                                       
                                                                                
Cross-identifications are given for stars in galactic open                      
clusters, in the Large and Small Magellanic Clouds, or in the following         
catalogues: C*, IRC, PK, and WD.                                                
                                                                                
\medskip                                                                        
\begin{SMALLFIELD}                                                              
Table~B5 \ref{table:B5}\RPAGE{table:B5} gives the list of galactic              
open clusters names and                                                         
abbreviations for which at least one star is included in the Input              
Catalogue. The reference of the adopted numbering system in each                
cluster is given under each chart (see Annex~3 of the printed version). Usual   
names for some clusters are given hereafter:                                    
$\alpha$ Persei (Melotte~20), Coma Berenices (Melotte 111), h Persei            
(NGC 869), $\chi$ Persei (NGC 884), Hyades (Melotte 25), Pleiades               
(Melotte 22), Praesepe (NGC 2632), $\zeta$ Sculptoris (Blanco 1).               
                                                                                
Identifications in the Large and Small Magellanic Clouds are                    
given in Table~I4. \ref{table:I4}                                               
                                                                                
\begin{table}[htb] \vspace{0.5cm}                                               
\CENTER {Table I4: Identifiers in the Magellanic Clouds}                        
\label{table:I4}                                                                
\vspace{0.5cm} \centering                                                       
\begin{tabular}{clll} \hline \\                                                 
Abbreviation & \multicolumn{1}{c}{Catalogue} & Reference & Format \\ \\         
\hline \\                                                                       
Sk & Large Magellanic Cloud & Sanduleak (1969a) & - DD NNN\\                    
Sk & Small Magellanic Cloud & Sanduleak (1968, 1969b) & NNN\\                   
\FINTABLE                                                                       
 ~                                                                              
\vfill\eject                                                                    
                                                                                
Other possible cross-identifications are given in                               
Table~I5. \ref{table:I5}                                                        
                                                                                
\begin{table}[htb] \vspace{0.5cm}                                               
\CENTER {Table I5: Others identifiers}                                          
\label{table:I5} \vspace{0.5cm} \centering                                      
\begin{tabular}{clll} \hline \\                                                 
Abbreviation & \multicolumn{1}{c}{Catalogue} & Reference & Format \\ \\         
\hline \\                                                                       
C* & Cool Carbon stars & Stephensen (1973) & NNNN\\                             
IRC & Caltech 2$\mu$ Survey & Neugebauer \ETAL\ (1969) & $\pm$DDNNN\\           
PK & Planetary Nebulae & Perek \& Kohoutek (1967) & LLL$\pm$BB NN\\             
WD & White Dwarfs & McCook \& Sion (1977) & HHMM$\pm$DD\\                       
\FINTABLE                                                                       
 ~                                                                              
                                                                                
\begin{table}[p]                                                                
\vspace{0.5cm}                                                                  
\CENTER {Table B5: Galactic open clusters: names and                            
abbreviations}\label{table:B5} \vspace{0.5cm}                                   
\centering                                                                      
\begin{tabular}{llrrrrrrrrrrr} \hline \\                                        
Abbrev.& Cluster Name &                                                         
\multicolumn{11}{c}{Clusters with Stars in the Hipparcos Input Catalogue}\\     
\\ \hline \\                                                                    
NGC & New General                                                               
 &~129& ~188& ~225& ~457& ~581& ~654& ~659& ~663& ~744& ~752& ~869\\            
& Catalogue &~884& ~957& 1027& 1039& 1245& 1342& 1444& 1502& 1528& 1545& 1647\\ 
&&1662& 1750& 1778& 1807& 1857& 1893& 1901& 1907& 1912& 1960& 1977\\            
&&2099& 2129& 2168& 2169& 2204& 2232& 2244& 2251& 2264& 2281& 2286\\            
&&2287& 2301& 2323& 2335& 2343& 2353& 2354& 2360& 2362& 2383& 2395\\            
&&2414& 2422& 2423& 2437& 2439& 2447& 2451& 2467& 2477& 2482& 2483\\            
&&2489& 2516& 2527& 2533& 2539& 2546& 2547& 2548& 2567& 2571& 2579\\            
&&2632& 2669& 2670& 2682& 2925& 3033& 3114& 3228& 3293& 3324& 3496\\            
&&3532& 3572& 3603& 3680& 3766& 4103& 4337& 4349& 4439& 4463& 4609\\            
&&4755& 5138& 5281& 5316& 5460& 5606& 5617& 5662& 5749& 5822& 5823\\            
&&6025& 6067& 6087& 6124& 6167& 6169& 6178& 6193& 6204& 6208& 6231\\            
&&6242& 6249& 6250& 6281& 6322& 6383& 6405& 6425& 6475& 6494& 6514\\            
&&6530& 6531& 6546& 6604& 6611& 6613& 6618& 6633& 6664& 6694& 6709\\            
&&6716& 6755& 6811& 6823& 6830& 6834& 6866& 6871& 6882& 6883& 6910\\            
&&6913& 6940& 7039& 7062& 7063& 7086& 7092& 7128& 7142& 7160& 7209\\            
&&7235& 7243& 7261& 7380& 7510& 7654& 7686& 7788& 7789& 7790& 7822\\            
Ber & Berkeley & 87\\                                                           
Biu & Biurakan &  2\\                                                           
Bla & Blanco &  1\\                                                             
Boc & Bochum &  4 & 13\\                                                        
Col & Collinder & 96 & 121 & 132 & 140 & 185 &                                  
197 & (205*) & 228 & 258 & 463\\                                                
Hog & Hogg & 14 & 15 & (16**) & 17 & 18\\                                       
IC  & Index Catalogue & 348 & 1795 & 1805 & 1848 & 2391 & 2395 &                
2581 & 2602 & 2944 & 4651 & 4665\\ && 4725 & 4756 & 4996 & 5146\\               
Kin & King & 19\\                                                               
Lyn & Lyng\aa & 2\\                                                             
Mrk & Markarian & (6***) & 18 & 50\\                                            
Mel & Melotte & 20 & 22 & 25 & 111 & 227\\                                      
Pis & Pismis & 4 & 12 & 16 & 20\\                                               
Rup & Ruprecht & 44 & 98 & 108\\                                                
Sto & Stock & 2 & 7 & 14\\                                                      
Tru & Trumpler & 1 & 2 & 9 & 10 & 15 & 16 & 17 & 18 & 27 & 33 & 37\\            
Upg & Upgren & 1\\                                                              
\\ \hline \\                                                                    
\end{tabular}                                                                   
                                                                                
\begin{itemize}\itemsep=-4pt                                                    
\item[*] Collinder 205 = Markarian 18                                           
\item[**] Hogg 16 is also called Basel 19                                       
\item[***] Markarian 6 = Stock 7                                                
\end{itemize}                                                                   
\end{table}                                                                     
                                                                                
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section* {Fields 61: Miscellaneous Information}                                
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{61, 1st character}{Survey star and identification chart}                
%++++++++++++++++++++++++                                                       
                                                                                
The letters in this field have the following meaning:                           
                                                                                
\begin{LISTONE}                                                                 
\item[\BPIT{S}] the star is a `survey' star                                     
\item[\BPIT{C}] an identification chart is provided within the faint            
star Atlas (Annex~2, Volume~7 of the printed version)                           
\item[\BPIT{T}] the star is a `survey' star, and an identification chart is     
provided within the faint star Atlas \end{LISTONE}                              
                                                                                
\begin{SMALLFIELD}                                                              
The survey is the basic list of bright stars added to and                       
merged with the total list of proposed stars (see `Star Selection',             
page 5). Its limiting magnitude is a function of the star's spectral            
type and galactic latitude, and is defined by:                                  
\[                                                                              
\begin{array}{rcll}                                                             
V_{\rm lim} &\le& 7.9 + 1.1\sin |b| &                                           
\mbox{\rm ~~~for spectral types earlier or equal to G5,}\\                      
V_{\rm lim} &\le& 7.3 + 1.1\sin |b| &                                           
\mbox{\rm ~~~for spectral types later than G5.}\\                               
\end{array}                                                                     
\]                                                                              
(if no spectral type was available, the break was                               
taken at $B-V = 0.8$ mag).                                                      
                                                                                
Where there was considered to be some possible doubt as to the                  
identification of the star (e.g. for faint stars, for crowded zones, or         
for components of double or multiple systems), charts were constructed          
from the Guide Star Catalog (Lasker \ETAL\ 1990).                               
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{61, 2nd character}{Notes}                                               
%++++++++++++++++++++++++                                                       
                                                                                
The letter `N' in this field indicates that a note is given in this file.       
                                                                                
                                                                                
                                                                                
\begin{table}[p]                                                                
\CENTER{Table A3: Solar system objects observed by Hipparcos}\label{table:A3}   
\begin{flushleft}                                                               
\vspace{0.5cm}                                                                  
(a) Minor planets                                                               
\end{flushleft}                                                                 
\centering                                                                      
\begin{tabular}{rlrlrl} \hline \\                                               
\multicolumn{1}{c}{No.} & \multicolumn{1}{c}{Name} &                            
\multicolumn{1}{c}{No.} & \multicolumn{1}{c}{Name} &                            
\multicolumn{1}{c}{No.} & \multicolumn{1}{c}{Name}\\ \\ \hline \\               
1 & Ceres & 18 & Melpomene & 63 & Ausonia\\                                     
2 & Pallas & 19 & Fortuna & 88 & Thisbe\\                                       
3 & Juno & 20 & Massalia & 115 & Thyra\\                                        
4 & Vesta & 22 & Kalliope & 129 & Antigone\\                                    
\\                                                                              
5 & Astraea & 23 & Thalia & 192 & Nausikaa\\                                    
6 &  Hebe &  27 &  Euterpe &  196 &  Philomela\\                                
7 &  Iris &  28 &  Bellona  &  216 &  Kleopatra  \\                             
8 &  Flora &  29 &  Amphitrite &  230 &  Athamentis\\                           
\\                                                                              
9 &  Metis &  30 &  Urania  &  324 &  Bamberga \\                               
10 &  Hygiea &  31 &  Euphrosyne &  349 &  Dembowska\\                          
11 &  Parthenope &  37 &  Fides &  354 &  Eleonora\\                            
12 &  Victoria &  39 &  Laetitia  &  451 &  Patientia\\                         
\\                                                                              
13 &  Egeria  &  40 &  Harmonia &  471 &  Papagena\\                            
14 &  Irene &  42 &  Isis &  511 &  Davida\\                                    
15 &  Eunomia  &  44 &  Nysa &  532 &  Herculina\\                              
16 &  Psyche &  51 &  Nemausa &  704 &  Interamnia\\                            
\\ \hline \\ \end{tabular}                                                      
                                                                                
\begin{flushleft}                                                               
\bigskip                                                                        
\bigskip                                                                        
(b) Other solar system objects\\                                                
\medskip                                                                        
Satellite of Jupiter: Europa\\                                                  
Satellites of Saturn: Iapetus and Titan\\                                       
\medskip                                                                        
(Note that additional solar system objects, in particular Uranus and            
Neptune, are observed by the Hipparcos satellite's `star mapper' as             
part of the Tycho experiment)                                                   
\end{flushleft}                                                                 
\end{table}                                                                     
                                                                                
\vfill\eject                                                                    
                                                                                
                                                                                
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\Large\bf Catalogue Abbreviations}\label{endintro}                      
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
\footnotesize\begin{tabbing}                                                    
{\normalsize ~~~~~~~~~~~~} \=  \kill                                            
AC  \> Astrographic Catalogue, see van Biesbroeck (1963)\\                      
ADS  \> New General Catalogue of Double Stars within $120\degr$ of the          
North Pole, Aitken (1932) \\                                                    
AGK3  \> Catalogue of Positions and Proper Motions North of $-2\degr.5$,        
Vols 1-8, Dieckvoss \ETAL\ (1975)\\                                             
AGK3R \> Catalogue of Reference Stars for the AGK3, Smith (1980)\\              
AGK3RN \> Unpublished version of AGK3R, supplied with proper motions by         
T.E. Corbin\\                                                                   
BD  \> Bonner Durchmusterung, Sch\"onfeld (1886), Argelander (1903)\\           
BPM  \> Bruce Proper Motion Survey, Luyten (1963)\\                             
CAMC  \> Carlsberg Meridian Catalogues Vols 1-4 (1985-87)\\                     
CCDM  \> Catalogue of Components of Double and Multiple Stars, Dommanget \ETAL\ 
(in preparation)\\                                                              
CD  \> Cordoba Durchmusterung, Thome (1892, 1894, 1900, 1914); Perrine (1932)\\ 
CDA  \> Catalogue des Donn\a'{e}es Astrom\a'{e}triques, see Bastian \& Lederle  
(1985)\\                                                                        
CF  \> Cape  Catalogue of Faint Stars, Spencer-Jones \& Jackson (1939)          
\\ CPC  \> The Cape Photographic Catalogue for 1950.0, Jackson \& Stoy          
(1954-68)\\ CPC2  \> Second Cape Photographic Catalogue, see Nicholson \ETAL\   
(1984)\\ 2CP50  \> Second Cape Catalogue for 1950.0, Stoy (1968)\\              
CPD  \> Cape Photographic Durchmusterung, Gill (1903)\\                         
CSI  \> Catalogue of Stellar Identifications, Ochsenbein (1978)\\               
C*  \> Cool Carbon Stars Catalogue, Stephensen (1973) \\                        
DM  \> Durchmusterung (BD, CD or CPD)\\                                         
FK4  \> Fourth Fundamental Catalogue, Fricke \ETAL\ (1963)\\                    
FK4 Sup \> Preliminary Supplement to FK4, Fricke (1963)\\                       
FK5  \> Fifth Fundamental Catalogue, Fricke \ETAL\ (1988)\\                     
FK5 Ext \> The FK5 extension. New Fundamental Stars, Fricke \ETAL\ (1991)\\     
G  \> Lowell Proper Motion Survey, Giclas \ETAL\ (1959-78)\\                    
GC  \> General Catalogue of 33342 Stars for the Epoch 1950, Boss \ETAL\ (1937)\\
GCPD  \> General Catalogue of Photometric Data, Hauck \ETAL\ (1990) \\          
GCRV  \> General Catalogue of Radial Velocities, Wilson (1953) \\               
GCVS  \> General Catalogue of Variable Stars, Kholopov ed. (1985)\\             
GJ  \> Extension to the Catalogue of Nearby Stars, Gliese \& Jahrei\ss\ ~       
(1979)\\                                                                        
GL  \> Catalogue of Nearby Stars, Gliese (1969)\\                               
GSC\> Guide Star Catalog of the Space Telescope Science Institute, Lasker \ETAL\
(1990)\\                                                                        
HD  \> Henry Draper Catalogue, Cannon \& Pickering (1918-49)\\                  
HDE   \> Henry Draper Extensions, Cannon (1925-36), Cannon \& Walton Mayall     
(1949)\\                                                                        
HIC  \> Hipparcos Input Catalogue, ESA-SP1136 (1992)\\                          
IDS  \> Index of Double Stars, Jeffers \ETAL\ (1963)\\                          
IRC  \> Caltech 2m Survey, Neugebauer \ETAL\ (1969)\\                           
IRS  \> International Reference Stars, comprises AGK3R and SRS Catalogues\\     
L  \> Luyten Catalogue, Luyten (1942) \\                                        
LHS  \> Luyten Half-Second Catalogue, Luyten (1979) \\                          
LP  \> Luyten Palomar Catalogue (proper motion survey with the 48-inch Schmidt),
Luyten (1963-87) \\                                                             
LTT  \> Luyten Two-Tenth Catalogue, Luyten (1957) (see also NLTT)\\             
McC  \> McCormick Observatory, Vyssotsky (1943-58) \\                           
MSS  \> Michigan Spectral Survey Vols 1-4, Houk \ETAL\                          
(1975, 1978, 1982, 1988) \\                                                     
NLTT  \> New Luyten Two-Tenth Catalogue Vols I-IV, Luyten (1979-80)\\           
NPZT74 \> Northern PZT Stars Catalog, Yasuda \ETAL\ (1982)\\                    
NSV  \> New Catalogue of Suspected Variable Stars, Kholopov ed. (1982)\\        
N30  \> Catalogue of 5268 Standard Stars, 1950.0, based on the Normal           
System N30,                                                                     
Morgan (1952)\\                                                                 
Perth 70  \> A Catalogue of Positions of 24900 Stars, H{\o}g \ETAL\ (1976) \\   
PK  \> Planetary Nebulae, Perek \& Kohoutek (1967) \\                           
PPM  \> Positions and                                                           
Proper Motions: Stars north of -2$\degr$.5 declination, R\"oser \& Bastian      
(1991)\\                                                                        
SAO  \> Smithsonian Astrophysical Observatory Star Catalogue (1966)\\           
SIMBAD \> Data base of the Centre de Donn\a'{e}es Astronomiques de Strasbourg,  
Egret \ETAL\  (1991)\\                                                          
Sk  \> Stars in the Large \& Small Magellanic Clouds (Sanduleak 1968,           
1969a,b)\\                                                                      
SRS \> Southern Reference System Catalogue, Smith \ETAL\ (1990) \\              
SSSC  \> Sydney Southern Star Catalogue, King \& Lomb (1983)\\                  
WD  \> Catalogue of White Dwarfs, McCook \& Sion (1977) \\                      
WDS  \> Washington Catalog of Visual Double Stars 1984.0, Worley \& Douglass    
(1984)\\                                                                        
Woolley \> Catalogue of Stars within 25pc of the Sun, Woolley \ETAL\ (1970)\\   
YZ  \> Yale Photographic Catalogues, Trans. Astron. Obs.                        
Yale University, Vols 3-32 (1926-83)\\                                          
\end{tabbing}                                                                   
                                                                                
                                                                                
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\LARGE\bf References}                                                   
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
                                                                                
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R\'equi\`eme Y., 1988b, Proc. Sitges Coll. `Scientific                          
Aspects of the Input Catalogue Preparation', Torra J. \& Turon C. (eds),        
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R\'equi\`eme Y., 1989, ESA SP-1111, Vol. II, 107                                
                                                                                
R\"oser                                                                         
S., Bastian U., 1991, PPM Star Catalogue, Vols I \& II, Astron.                 
Rechen-Institut, Heidelberg                                                     
                                                                                
Sanduleak N., 1968, Astron.  J., 73, 246                                        
                                                                                
Sanduleak N., 1969a, Cerro Tololo Inter-American Observatory                    
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Sanduleak N., 1969b, Astron. J., 74, 877                                        
                                                                                
Sch\"onfeld E., 1886, Marcus \& Weber's Verlag, Bonn                            
                                                                                
Smith C.A.,                                                                     
1980, Mitt. der Astr. Gesellschaft 48, 95                                       
                                                                                
Smith C.A., Kaplan G.H.,                                                        
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Stephensen C.B., 1973, A General Catalogue of Cool Carbon                       
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Stoy R.H., 1968,                                                                
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Thome                                                                           
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Vyssotsky A.N.,                                                                 
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Vyssotsky A.N.,                                                                 
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\end{PRETTYREF}                                                                 
                                                                                
                                                                                
%                                                                               
\vfill                                                                          
\eject                                                                          
%                                                                               
                                                                                
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\LARGE\bf Notes}                                                        
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
\bigskip                                                                        
These notes include:                                                            
\begin{itemize}\itemsep=-4pt                                                    
\item references to erroneous data or incorrect identifications found in the    
      literature;                                                               
\item information for double or multiple systems not contained in the CCDM;     
\item other identifications, where appropriate;                                 
\item any inconsistencies noted from early results of the satellite data        
      processing.                                                               
\end{itemize}                                                                   
                                                                                
                                                                                
\begin{SMALLFIELD}                                                              
\begin{tabbing} 12345678\=et voila\kill                                         
 ~~~40 \> joint system: NGC 7822 11 (A)/ 12 (B)\\                               
 ~~183 \> although bright, this star is not in SAO\\                            
 ~~223 \> component B = NSV 3\\                                                 
 ~~350 \> erroneously identified with CPD -57$\degr$ 10423 and                  
	CPD -58$\degr$ 8130 in the literature\\                                        
 ~~592 \> central star of a reflection nebula\\                                 
 ~~755 \> erroneous value for proper motion in right ascension in GC and SAO\\  
 ~1021 \> central star of a reflection nebula\\                                 
 ~1158 \> component A = AD Cet \\                                               
 ~1501 \> component B is variable\\                                             
 ~1543 \> component A = V377 Cas\\                                              
 ~1860 \> other identification: LHS 1065. LHS 1066 (also G 242-52, V=14 mag)    
	 is at 11arcsec\\                                                              
 ~1902 \> globular cluster 47 Tucanae\\                                         
 ~2242 \> double system: $\theta=$ 215$\degr$, $\rho=$ 36 arcsec,               
	$\Delta V=$ 3.2 mag\\                                                          
 ~2355 \> component A = GN And\\                                                
 ~3243 \> erroneously identified with GJ 1017 in the literature\\               
 ~3856 \> error in HIC identification: LHS 124 is about 20 arcsec NNE of the    
	target \\                                                                      
 ~4189 \> double system with LP 990-139: $\theta=$ 202$\degr$, $\rho=$ 5        
arcsec,                                                                         
	$\Delta V=$ 0.9 mag\\                                                          
 ~4427 \> component A = gam Cas\\                                               
 ~4655 \> component A = WW Psc\\                                                
 ~4831 \> double system: $\theta=$ 170$\degr$, $\rho=$ 61 arcsec, $\Delta       
V=$ 1                                                                           
	mag. Component B = CD -48$\degr$ 249\\                                         
 ~5348 \> component A = zet Phe\\                                               
 ~5745 \> erroneously identified with CPD -51$\degr$ 179 in the literature\\    
 ~7024 \> component A = SY Phe\\                                                
 ~7410 \> double system: $\theta=$ 120$\degr$, $\rho=$ 90 arcsec,               
	$\Delta V=$ 1.5 mag\\                                                          
 ~8832 \> component A = gam Ari\\                                               
 ~8924 \> not LP 528-136 (error in HIC identification). Proper motion from      
	ESO plates and AC\\                                                            
 ~9230 \> component A = CI Eri\\                                                
 ~9258 \> component A = AA Cet\\                                                
 ~9383 \> component A = X Tri\\                                                 
 ~9711 \> not detected by the satellite at the expected position or with the    
	expected intensity\\                                                           
 ~9786 \> erroneously identified with SAO 167562 in the literature\\            
 ~9879 \> erroneously identified with G 274-149 and LTT 1101 in the literature\\
 10280 \> component A = TZ Tri\\                                                
 10704 \> component A = V438 Per\\                                              
 10826 \> component A = omi Cet; component P = VZ Cet\\                         
 11174 \> component A = V440 Per\\                                              
 11317 \> other identification: Woolley 9081\\                                  
 11569 \> component A = iot Cas\\                                               
 11604 \> other identification: Markarian 6 28\\                                
 11607 \> other identification: Markarian 6 23\\                                
 11612 \> other identification: Markarian 6 18\\                                
 11769 \> component A = V425 Per\\                                              
 12035 \> double system: $\theta=$ 30$\degr$, $\rho=$ 38 arcsec,                
	$\Delta V=$ 0.9 mag\\                                                          
 12097 \> erroneously identified with BD +19$\degr$ 381 in the literature\\     
 12101 \> erroneously identified with CD -48$\degr$ 698 and CPD -49$\degr$ 132  
	in the literature\\                                                            
 12495 \> component A = V482 Cas\\                                              
 12981 \> component A = CU Eri\\                                                
 13112 \> uncertain magnitude\\                                                 
 13215 \> this star is SW of LHS 1452, proper motion close to zero\\            
 13218 \> erroneously quoted as a double system in the literature\\             
 13290 \> erroneously identified with V500 Cas in the literature\\              
 14879 \> component B = NSV 1074\\                                              
 15087 \> erroneously identified with AGK +52$\degr$ 334 in the literature\\    
 15286 \> erroneous proper motion in SAO, correct in NLTT\\                     
 15474 \> component A = tau 04 Eri\\                                            
 15803 \> double system: $\theta=$ 215$\degr$, $\rho=$ 21 arcsec,               
	$\Delta B=$ 1.1 mag\\                                                          
 16490 \> double system on Palomar plates, $\theta=$ 100$\degr$,                
	$\rho=$ 20 arcsec, $\Delta B=$ 2 mag\\                                         
 16713 \> component A = IX Per \\                                               
 16846 \> component A = V711 Tau\\                                              
 17448 \> component A = omi Per\\                                               
 17465 \> joint system: IC 348  14/20\\                                         
 17572 \> joint system: Melotte 22  800 (B)/ 801 (A)\\                          
 17600 \> component A = S For\\                                                 
 17923 \> joint system: Melotte 22  2500 (C)/ 2503 (B)/ 2507 (A)\\              
 18322 \> erroneously identified with BD +12$\degr$ 530 in the literature\\     
 18377 \> not detected by the satellite at the expected position or with the    
	expected intensity\\                                                           
 18972 \> component A = RW Tau\\                                                
 19201 \> component A = AG Per\\                                                
 19261 \> joint system: Melotte 25  11 (A)/ 12 (B)\\                            
 19272 \> joint system: NGC 1502  1 (A)/ 4 (C)\\                                
 19424 \> component A = U Men\\                                                 
 19849 \> erroneously identified with DY Eri in the literature\\                
 20338 \> companion of HIC 20342, $\theta=$ 330$\degr$, $\rho=$ 61 arcsec\\     
 20342 \> companion of HIC 20338\\                                              
 20632 \> double system: $\theta=$ 2$\degr$, $\rho=$ 28 arcsec,                 
	$\Delta V=$ 2.1 mag\\                                                          
 20648 \> component A = V776 Tau\\                                              
 20990 \> component A = UX Tau\\                                                
 21185 \> not LHS 193 (error in HIC identification)\\                           
 21222 \> triple system:  AB: $\theta=$ 320$\degr$, $\rho=$ 34 arcsec,          
	$\Delta B=$ 1.1 mag\\                                                          
  \> AC: $\theta=$ 170$\degr$, $\rho=$ 27 arcsec, $\Delta B=$ 1.2 mag\\         
 21256 \> erroneously identified with McC 744 or G 8-23 in the literature\\     
 21278 \> component A = EH Eri\\                                                
 21492 \> not detected by the satellite at the expected position or with the    
	expected intensity\\                                                           
 21763 \> component A = DM Eri\\                                                
 21986 \> component B = DW Eri\\                                                
 22105 \> other identification: Melotte 25 8067\\                               
 22176 \> other identification: Melotte 25 164\\                                
 22260 \> component A = XZ Men \\                                               
 23873 \> component A = RW Aur \\                                               
 24575 \> component A = AE Aur  \\                                              
 25050 \> component A = UV Aur \\                                               
 25281 \> component A = eta Ori  \\                                             
 25473 \> component A = psi Ori  \\                                             
 25733 \> component A = LY Aur \\                                               
 25921 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 25966 \> double system: $\theta=$ 55$\degr$, $\rho=$ 25 arcsec,                
	$\Delta m=$ 0.6 mag\\                                                          
 26220 \> joint system: NGC 1977  587 (B = V1016 Ori)/ 595 (D = BM Ori)/        
584 (H)\\                                                                       
 26950 \> not detected by the satellite at the expected position or with the    
	expected intensity\\                                                           
 27656 \> erroneously identified with CD -41$\degr$ 2185 in the literature\\    
 27989 \> component A = alf Ori \\                                              
 28380 \> component A = tet Aur\\                                               
 28436 \> erroneously identified with CPD -65$\degr$ 633 in the literature\\    
 29055 \> probably fainter than indicated: 11.22 $<$ V $<$ 12.11 according      
	to GCVS\\                                                                      
 29100 \> not detected by the satellite at the expected position or with the    
	expected intensity\\                                                           
 29170 \> component B = NSV 2849\\                                              
 29385 \> optical pair with CD -35$\degr$ 2745 (satellite target is the faint   
	component at the NW)\\                                                         
 29401 \> component A = V638 Mon \\                                             
 29655 \> component A = eta Gem \\                                              
 30214 \> component A = FR CMa \\                                               
 30920 \> component B = V577 Mon\\                                              
 31070 \> not detected by the satellite at the expected position or with the    
	expected intensity\\                                                           
 31153 \> error in HIC identification (BD +14$\degr$ 1330 is at                 
	$\alpha=$ 06 32 12.0,  $\delta=$ +14 27 50)\\                                  
 31292 \> physical pair with HIC 31293, $\rho=$ 23 arcsec,                      
	$\theta=$ 215$\degr$, $\Delta B=$ 1.0 mag\\                                    
 31293 \> physical pair with HIC 31292\\                                        
 31349 \> erroneous proper motion in AGK3\\                                     
 31437 \> not detected by the satellite at the expected position or with the    
	expected intensity\\                                                           
 32270 \> erroneous position in NLTT\\                                          
 32349 \> Sirius. The adopted proper motion is the combination of the proper    
	motion of the centre of \\                                                     
	\> gravity of the system and of the orbital motion. The adopted value          
	is valid for the mean\\                                                        
	\> epoch of the Hipparcos mission. An ephemeris is given in the                
	introduction to \\                                                             
	\> Annex 1 (field 5)\\                                                         
 32504 \> other identification: Collinder 121 37\\                              
 33324 \> erroneously identified with CPD -56$\degr$ 1692 in the literature\\   
 34117 \> not detected by the satellite at the expected position or with the    
	expected intensity\\                                                           
 34234 \> component A = V569 Mon\\                                              
 34299 \> erroneously identified with BD -04$\degr$ 1825 in the literature\\    
 34301 \> component A = FN CMa\\                                                
 35381 \> double system: $\theta=$ 180$\degr$, $\rho=$ 12 arcsec                
	(this entry is the northern component)\\                                       
 35793 \> component A = VY CMa\\                                                
 36188 \> component A = bet CMi\\                                               
 36347 \> double system from ESO plate measurements, $\Delta B=$ 3 mag\\        
 36649 \> not detected by the satellite at the expected position or with the    
	expected intensity\\                                                           
 37279 \> Procyon. The adopted proper motion is the combination of the proper   
	motion of the centre \\                                                        
	\> of gravity of the system and of the orbital motion. The adopted             
	value is valid for the mean \\                                                 
	\> epoch of the Hipparcos mission. An ephemeris is given                       
	in the introduction to Annex 1 (field 5)\\                                     
 38014 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 38256 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 38398 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 38575 \> erroneously identified with SAO 116086 in the literature\\            
 38692 \> joint system: Trumpler 9  62/63\\                                     
 38957 \> component A = V Pup\\                                                 
 38966 \> joint system: NGC 2516  130 (A)/ 210 (B)\\                            
 39329 \> component A = QQ Pup\\                                                
 39652 \> erroneously identified with CD -39$\degr$ 3991 in the literature\\    
 39656 \> erroneously identified with CD -39$\degr$ 3987 in the literature\\    
 39826 \> erroneous proper motion in AGK3\\                                     
 39840 \> erroneously identified with BD -16$\degr$ 231 in the literature\\     
 40831 \> double on ESO plates, $\rho=$ 23 arcsec\\                             
 40935 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 40977 \> component A = V Cnc \\                                                
 41361 \> component A = NO Pup \\                                               
 41979 \> erroneously identified with BD +20$\degr$ 2113 and                    
	AGK +20$\degr$ 985 in the literature\\                                         
 42366 \> erroneously identified with CD -50$\degr$ 1691 in the literature\\    
 42712 \> component A = HX Vel \\                                               
 42988 \> other identification: IC 2391 46\\                                    
 43071 \> other identification: IC 2391 49\\                                    
 43406 \> error in HIC identification (LHS 2056 is about 30 arcsec SW of        
	the target)\\                                                                  
 43851 \> erroneously identified with NSV 4310 in the literature\\              
 44232 \> other identification: Collinder 205 2\\                               
 44243 \> other identification: Collinder 205 1\\                               
 45170 \> component P = GL 337B\\                                               
 45792 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 45908 \> erroneously identified with CPD -59$\degr$ 2351 in the literature\\   
 45954 \> erroneous position in NLTT\\                                          
 46586 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 46806 \> component A = R Car \\                                                
 46899 \> erroneously identified with BD -10$\degr$ 2681 in the literature\\    
 47145 \> component A = IM Vel \\                                               
 47480 \> erroneously identified with LHS 2169 (which is at 66 arcsec,          
	$\theta=$ 220$\degr$) in the literature\\                                      
 47694 \> component A = IP Vel \\                                               
 47727 \> component A = W UMa \\                                                
 48218 \> component B = DG Leo\\                                                
 49616 \> erroneously identified with GL 385 in the literature\\                
 50640 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 50829 \> component B = NSV 4836\\                                              
 51612 \> companion at $\rho=$ 25 arcsec, $\Delta m=$ 2 mag\\                   
 51802 \> component A = TX Leo \\                                               
 52526 \> component A = QZ Car \\                                               
 54131 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 54299 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 54360 \> component A = V815 Cen \\                                             
 54365 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 54724 \> erroneous proper motion in SAO\\                                      
 55052 \> double on ESO plates, $\theta=$ 75$\degr$, $\rho=$ 12.4 arcsec,       
	$\Delta B >$ 2 mag\\                                                           
 55106 \> component A = SV Crt  \\                                              
 56327 \> erroneously identified with BD -11$\degr$ 3122 in the literature\\    
 56518 \> component A = V763 Cen \\                                             
 56991 \> component A = UZ Cen \\                                               
 57936 \> component A = bet Hya \\                                              
 59219 \> erroneously identified with BD +22$\degr$ 233 in the literature\\     
 59683 \> component A = AH Vir \\                                               
 60197 \> joint system: Melotte 111  72 (B)/ 73 (A)\\                           
 60417 \> erroneously identified with CPD -66$\degr$ 1212 in the literature\\   
 60500 \> component A = FK Vir \\                                               
 60557 \> joint system: NGC 4337  17 (A)/ 18 (B)\\                              
 60878 \> this component B is at 1196.3 arcsec from A\\                         
 60936 \> 3C 273\\                                                              
 61826 \> erroneously identified with BD -15$\degr$ 3342 in the literature\\    
 62038 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 62967 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 63494 \> component B = NSV 6053\\                                              
 64094 \> component A = tet Mus \\                                              
 65182 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 65977 \> component A = V701 Cen \\                                             
 66187 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 66307 \> erroneous proper motion in CPC2\\                                     
 66747 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 66934 \> erroneous proper motion in SAO\\                                      
 67090 \> optical double system\\                                               
 67261 \> component A = V766 Cen \\                                             
 67487 \> erroneous position in CPC2\\                                          
 68264 \> erroneously identified with CPD -40$\degr$ 4376 in the literature\\   
 68702 \> component A = bet Cen  \\                                             
 69454 \> erroneously identified with CPD -56$\degr$ 5362 and                   
	IDS 14064 S 5617 B in the literature\\                                         
 69972 \> erroneously identified with CPD -58$\degr$ 5564 in the literature\\   
 70958 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 70890 \> Proxima Centauri\\                                                    
 71681-71683 = $\alpha$ Centauri. The adopted proper motion is the combination  
	of the proper motion of \\                                                     
	\> the centre of gravity of the system and of the orbital motion.              
	The adopted value is valid for \\                                              
	\> the mean epoch of the Hipparcos mission. An ephemeris is given              
	in the introduction to \\                                                      
	\> Annex 1 (field 5)\\                                                         
 71766 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 71876 \> component A = DL Dra  \\                                              
 72436 \> erroneous right ascension in NLTT\\                                   
 72659 \> component A = ksi Boo  \\                                             
 73695 \> component A = 44 Boo; component B = i Boo (variable component)\\      
 74192 \> component A = T TrA  \\                                               
 74332 \> double system: $\theta=$ 50$\degr$, $\rho=$ 25 arcsec,                
	$\Delta V=$ 3.6 mag\\                                                          
 74386 \> component A = FL Ser \\                                               
 74838 \> double system: $\theta=$ 165$\degr$, $\rho=$ 21 arcsec,               
	$\Delta V=$ 1.4 mag\\                                                          
 75695 \> component A = bet CrB  \\                                             
 75727 \> component A = GO Lup \\                                               
 76196 \> component A = TW Dra  \\                                              
 76276 \> component A = del Ser  \\                                             
 76334 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 76377 \> component A = R Nor \\                                                
 76952 \> component A = gam CrB  \\                                             
 77157 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 77895 \> double system: $\theta=$ 100$\degr$, $\rho=$ 25 arcsec,               
	$\Delta V=$ 3.0 mag\\                                                          
 78233 \> double system: $\theta=$ 25$\degr$, $\rho=$ 20 arcsec,                
	$\Delta V=$ 3.5 mag\\                                                          
 78528 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 78999 \> erroneously identified with BD -05$\degr$ 4242 in the literature\\    
 79080 \> C component = V856 Sco\\                                              
 79126 \> proper motion derived from the position in the GSC and in AC\\        
 79212 \> component A = EQ TrA \\                                               
 79607 \> component A = TZ CrB  \\                                              
 79734 \> double system: $\theta=$ 185$\degr$, $\rho=$ 15 arcsec,               
	$\Delta V=$ 3.5 mag\\                                                          
 79844 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 80463 \> component A = ome Her \\                                              
 80509 \> double system: $\theta=$ 205$\degr$, $\rho=$ 24 arcsec, $\Delta       
V=$ 3.0 mag\\                                                                   
 80706 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 80763 \> component A = alf Sco  \\                                             
 80851 \> double system: $\theta=$ 35$\degr$, $\rho=$ 26 arcsec,                
	$\Delta V=$ 0.9 mag\\                                                          
 81455 \> CD -29$\degr$ 12698, not  CD -29$\degr$ 12689 (error in YZ and SAO)\\ 
 81490 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 81519 \> component A = WW Dra \\                                               
 81538 \> error in HIC position: target is 25 arcsec from BD+52 1986 \\         
	\> ($\alpha=$ 16 39 73.88, $\delta=$ +52 37 37.7)\\                            
 81582 \> double system: $\theta=$ 25$\degr$, $\rho=$ 28 arcsec,                
	$\Delta V=$ 2.5 mag\\                                                          
 81589 \> component A = R Ara \\                                                
 81960 \> double system: $\theta=$ 50$\degr$, $\rho=$ 30 arcsec,                
	$\Delta V=$ 0.2 mag\\                                                          
 82321 \> component A = V637 Her  \\                                            
 83059 \> component A = RV Sco \\                                               
 83070 \> double system: $\theta=$ 225$\degr$, $\rho=$ 15 arcsec,               
	$\Delta V=$ 3.6 mag\\                                                          
 84289 \> component A = V655 Her \\                                             
 84293 \> component A = AK Her \\                                               
 84345 \> component A = alf Her \\                                              
 84573 \> component A = u Her  \\                                               
 84708 \> double system: $\theta=$ 360$\degr$, $\rho=$ 16 arcsec,               
	$\Delta B=$ 0.3 mag\\                                                          
 85302 \> component A = V640 Her \\                                             
 85467 \> component A = V750 Ara \\                                             
 85622 \> component B = NSV 8918\\                                              
 86062 \> erroneous proper motion in SAO\\                                      
 86101 \> error on BD number in YZ\\                                            
 86789 \> double system: $\theta=$ 300$\degr$, $\rho=$ 11 arcsec,               
	$\Delta V=$ 2.6 mag\\                                                          
 86873 \> component A = SZ Sgr \\                                               
 86892 \> double system: $\theta=$ 10$\degr$, $\rho=$ 23 arcsec,                
	$\Delta V=$ 2.9 mag\\                                                          
 87345 \> component A = RY Sco \\                                               
 87482 \> double system: $\theta=$ 205$\degr$, $\rho=$ 10 arcsec,               
	$\Delta V=$ 3.8 mag\\                                                          
 87616 \> component A = V906 Sco \\                                             
 87937 \> Barnard's star\\                                                      
 88069 \> component A = V1647 Sgr \\                                            
 88438 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 88495 \> satellite target is CPC 21.1 4198 = CPD -64$\degr$ 3774,              
	probably not L 157-110\\                                                       
 88643 \> double system: $\theta=$ 190$\degr$, $\rho=$ 11 arcsec,               
	$\Delta V=$ 3.0 mag\\                                                          
 88827 \> erroneously identified with BD +01$\degr$ 3597 in the literature\\    
 89057 \> double system: $\theta=$ 135$\degr$, $\rho=$ 25 arcsec,               
	$\Delta V=$ 4.2 mag\\                                                          
 89156 \> component B = NSV 10363\\                                             
 89163 \> double system: $\theta=$ 20$\degr$, $\rho=$ 10 arcsec,                
	$\Delta V=$ 2.4 mag\\                                                          
 89299 \> companion of AGK +49$\degr$ 1397 = SAO 47320, $\rho=$ 14 arcsec\\     
 89642 \> component A = eta Sgr \\                                              
 89908 \> component A = phi Dra \\                                              
 90008 \> this star is CD -47$\degr$ 12228, not CD -47$\degr$ 12218\\           
 ~~~~~ \> ~~~~~~~ \\                                                            
 90048 \> triple system:  AB: $\theta=$ 40$\degr$, $\rho=$ 20 arcsec,           
	$\Delta V >$ 3 mag\\                                                           
	\> AC: $\theta=$ 315$\degr$, $\rho=$ 28 arcsec, $\Delta V=$ 1.8 mag\\          
 90441 \> component A = d Ser \\                                                
 90474 \> probably fainter than expected\\                                      
 90539 \> double system: $\rho <$ 5 arcsec from Palomar plates\\                
 90959 \> variability and photoelectric data are not coherent\\                 
 91256 \> double system: $\rho=$ 9 arcsec from ESO plates\\                     
 91389 \> component A = X Oph \\                                                
 91924 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 92221 \> double system: $\theta=$ 305$\degr$, $\rho=$ 12 arcsec,               
	$\Delta V=$ 0.3 mag\\                                                          
 92414 \> component A = AD Her \\                                               
 92499 \> erroneous proper motion in SAO, correct in CPC\\                      
 92536 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 93124 \> component A = FF Aql \\                                               
 93605 \> component A = SU Sgr \\                                               
 94155 \> double system: $\theta=$ 320$\degr$, $\rho=$ 20 arcsec,               
	$\Delta V=$ 3.9 mag\\                                                          
 94197 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 94368 \> erroneously identified with CPD -56$\degr$ 7638 in the literature\\   
 94827 \> component A = ES Vul  \\                                              
 94982 \> component A = V1208 Aql \\                                            
 95024 \> component A = U Lyr  \\                                               
 95198 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 95672 \> double system: $\theta=$ 0$\degr$, $\rho=$ 13 arcsec;                 
	component B $<$ 11 mag\\                                                       
 95676 \> probably fainter than expected\\                                      
 95820 \> component A = U Aql  \\                                               
 96007 \> component A = V822 Aql  \\                                            
 96108 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 96480 \> component A = V1744 Cyg  \\                                           
 96515 \> double system: $\theta=$ 200$\degr$, $\rho=$ 8 arcsec,                
	$\Delta V <$ 2 mag\\                                                           
 96840 \> component A = QS Aql  \\                                              
 97091 \> component A = PS Vul  \\                                              
 97241 \> double system: $\theta=$ 330$\degr$, $\rho=$ 15 arcsec,               
	$\Delta V=$ 0.9 mag\\                                                          
 98237 \> double system: $\theta=$ 320$\degr$, $\rho=$ 8 arcsec\\               
 99002 \> component A = V1676 Cyg \\                                            
 99085 \> component B = RY Cap \\                                               
 99283 \> joint system: Biurakan 2  130 (B)/ 131 (A)\\                          
 99397 \> not detected by the satellite at the expected position or with        
	the expected intensity\\                                                       
 99629 \> double system: $\theta=$ 305$\degr$, $\rho=$ 40 arcsec,               
	$\Delta V=$ 1.4 mag\\                                                          
 99675 \> component A = V695 Cyg  \\                                            
 100048 \> erroneous proper motion in AGK3\\                                    
 100227 \> component A = V478 Cyg  \\                                           
 100287 \> component A = V1687 Cyg  \\                                          
 100383 \> not detected by the satellite at the expected position or with       
	the expected intensity\\                                                       
 100515 \> component B = NSV 13053\\                                            
 100695 \> double system: $\rho=$ 32 arcsec, $\Delta V=$ 1.1 mag\\              
 101341 \> component A = V729 Cyg \\                                            
 101750 \> component A = VW Cep \\                                              
 101972 \> erroneous proper motion in GC and SAO\\                              
 102352 \> not detected by the satellite at the expected position or with       
	the expected intensity\\                                                       
 102571 \> component A = T Cyg \\                                               
 102817 \> physical pair with LP 928-63 at 23 arcsec, $\theta=$ 270$\degr$\\    
 103542 \> component A = KZ Pav \\                                              
 103766 \> other identification: Woolley 9715\\                                 
 104371 \> component A = V389 Cyg \\                                            
 104521 \> component A = gam Equ \\                                             
 104887 \> component A = tau Cyg \\                                             
 105539 \> erroneous proper motion in AGK3\\                                    
 105638 \> probably fainter than expected\\                                     
 106161 \> erroneously identified with G 26-8 = BD -02$\degr$ 5557 in the       
	literature\\                                                                   
 106774 \> other identification: IC 1396 452\\                                  
 106843 \> other identification: IC 1396 171\\                                  
 106998 \> not LHS 3700 (G 213-9). Error in HIC identification\\                
 107156 \> not SS Cyg. Error in HIC identification. Good coordinates (J2000)    
         for SS Cyg:\\                                                          
        \>  $\alpha=$ 21 42 42.6 $\delta=$ +43 35 09, at $\theta=$ 75           
         $\degr$, $\rho=$ 252 arcsec \\                                         
        \> from star indicated on the chart\\                                   
 107164 \> other identification: IC 1396 750\\                                  
 107259 \> other identification: IC 1396 1319\\                                 
 107594 \> component A = AP Cap \\                                              
 108426 \> component A = IR Cep \\                                              
 108797 \> component A = DX Aqr \\                                              
 109930 \> not detected by the satellite at the expected position or with       
	the expected intensity\\                                                       
 110478 \> component A = pi.01 Gru \\                                           
 110892 \> erroneous proper motion in SAO\\                                     
 110893 \> Kr\"uger 60 (component A = NSV 14168; component B = DO Cep).         
	The proper motion, \\                                                          
	\> taken from AGK3, is given for the centre of gravity of the system.          
	The orbital motion \\                                                          
	\> produces a small deviation from this value.\\                               
 111293 \> error in HIC position: target is 80 arcsec from LHS 525 \\           
	\> ($\alpha=$ 22 32 54.22 $\delta=$ +53 47 39.2)\\                             
 111363 \> double system: $\theta=$ 5$\degr$, $\rho=$ 22 arcsec,                
	$\Delta V=$ 2.4 mag\\                                                          
 111400 \> component A = V362 Lac \\                                            
 111692 \> CD -29$\degr$ 18408, not CD -29$\degr$ 18404 (error in YZ and SAO)\\ 
 111858 \> not detected by the satellite at the expected position or with       
	the expected intensity\\                                                       
 111932 \> double system: $\theta=$ 295$\degr$, $\rho=$ 19 arcsec,              
	$\Delta V=$ 0.6 mag\\                                                          
 113017 \> component A = IL Cep \\                                              
 113652 \> erroneously identified with HD 215173 in the literature\\            
 113738 \> component A = NN Cep \\                                              
 113802 \> component A = LN And \\                                              
 114092 \> erroneously identified with AGK +61$\degr$ 1415 in the literature\\  
 114107 \> erroneously identified with AGK +61$\degr$ 1413 in the literature\\  
 114669 \> component B = NSV 14460\\                                            
 114994 \> optical pair, see Giclas chart. The faint component is LHS 3923,     
	G 190-17. \\                                                                   
	\> The bright component is BD +37$\degr$ 4803 and has a very small             
	proper motion. Separation\\                                                    
	\> estimation from Palomar plates (epoch 1953.8):                              
	24 arcsec (10 arcsec in 1990)\\                                                
 115344 \> CPD -37$\degr$ 9332, not CPD -37$\degr$ 9232                         
	(error in the literature)\\                                                    
 115715 \> erroneous proper motion in GC and SAO; correct in NLTT and Giclas\\  
 115990 \> component A = AR Cas \\                                              
 115993 \> not detected by the satellite at the expected position or with       
	the expected intensity\\                                                       
 116214 \> doubtful magnitudes\\                                                
 116389 \> component A = iot Phe \\                                             
 116430 \> the large proper motion from SAO and NLTT seems questionable,        
	and is not retained\\                                                          
 117011 \> erroneous proper motion in LTT, correct in NLTT\\                    
 117114 \> CD -62$\degr$ 1460, not CD -62$\degr$ 1464 (error in NLTT)\\         
 117154 \> other identification: V405 Cas\\                                     
 117595 \> double system: $\theta=$ 330$\degr$, $\rho=$ 29 arcsec,              
	$\Delta V=$ 3.1 mag\\                                                          
 117779 \> double system: $\theta=$ 310$\degr$, $\rho=$ 22 arcsec,              
	$\Delta V=$ 1.3 mag\\                                                          
 117987 \> central star of a reflection nebula\\                                
 118209 \> component B = NSV 14785\\                                            
 120159 \> there is a faint optical companion at $\rho=$ 13 arcsec,             
	$\theta=$ 170$\degr$,~$\Delta m=$ 1 mag\\                                      
 120212 \> erroneously identified with AGK +01$\degr$ 1462 in the literature\\  
 120229 \> not detected by the satellite at the expected position or with       
	the expected intensity\\                                                       
 120248 \> erroneously identified with BD +66$\degr$ 466 and                    
       AGK +66$\degr$ 355 in the literature\\                                   
\end{tabbing}                                                                   
\end{SMALLFIELD}                                                                
                                                                                
\vfill\eject                                                                    
                                                                                
                                                                                
                                                                                
                                                                                
%*******************************************************************************
%*******************************************************************************
\part*{ANNEX 1 \\                                                               
\bigskip                                                                        
 Components of Double and Multiple Systems}                                     
%*******************************************************************************
%****************************************************************************** 
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\huge\bf Introduction}                                                  
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
\bigskip                                                                        
                                                                                
%-------------------------------------------------                              
\section*{Annex 1}                                                              
%-------------------------------------------------                              
                                                                                
The Hipparcos measurement system is not optimum for the                         
observation and detection of all categories of double and multiple              
stars. If the components of such systems are sufficiently well                  
separated, and sufficiently bright, each component may be observed              
separately, and may be included in the main catalogue according to its          
astrophysical or astrometric interest. However, for closer systems, or          
systems with fainter components, the instantaneous field of view of the         
Hipparcos observations may be centred on only one of the components, or         
on the geometric centre, or on the photocentre, depending on the                
precise geometric and photometric configuration of the system.                  
                                                                                
\medskip                                                                        
Annex 1 gives information and data for all known individual components          
of around fourteen thousand double and multiple systems for which at            
least one component is identified in the main Hipparcos Input                   
Catalogue, i.e.  when at least one component of the system is observed          
by the Hipparcos satellite. Because of their astronomical interest, all         
known components of double or multiple systems involved in the                  
Hipparcos observations have been collected together in Annex 1, even            
though they may be completely negligible, in the context of the                 
Hipparcos observations, because of their faint magnitude or distance            
from the primary component.                                                     
                                                                                
\medskip                                                                        
Annex 1 was constructed from a subset of a preliminary version of the           
Catalogue of Components of Double and Multiple Stars (CCDM, Dommanget           
at al., in preparation). A complete description of the information              
contained in the CCDM will be given in its first edition. This subset           
was supplemented by 452 stars (candidates for observation with                  
Hipparcos) discovered as double systems by M.~Rousseau when measuring           
ESO Survey Schmidt plates within the preparatory programme of                   
ground-based measurements.                                                      
                                                                                
\medskip                                                                        
The INCA data base (the source of the main catalogue), and the                  
preliminary version of CCDM (the source of Annex 1), have necessarily           
evolved separately during the course of the Input Catalogue                     
preparation. However, systematic comparisons were made regularly                
between them in order to improve their agreement. In some cases, in the         
construction of Annex~1, data from the INCA data base have been                 
preferred (for example, in the case of magnitudes or some proper                
motions), while in other cases, data from the CCDM were retained (for           
example, positions of components of the same system when they originate         
from the same source catalogue). This choice has been necessary in              
order to preserve the {\it internal} consistency of the (relative) data         
on the various components of a system, whilst at the same time                  
preserving the `absolute' positional information required for the               
Hipparcos observations. As a result, there are discrepancies between            
the details of such systems in the main catalogue and in Annex~1.               
                                                                                
\medskip                                                                        
The systems are ordered by increasing CCDM numbers (constructed from            
equatorial coordinates at equinox and epoch J2000.0). For a same right          
ascension, the systems are ordered from the North to the South Pole.            
Each system is distinguished from the next one by a blank line. The             
CCDM and HIC numbers provide the link between the main catalogue and            
this annex.                                                                     
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{Catalogue~~of~~Components~~of~~Double~~and~~Multiple~~Stars}          
%-------------------------------------------------                              
                                                                                
At the beginning of the INCA Consortium work in 1982, no                        
specific general {\it astrometric} catalogue of double and multiple             
stars was available, and the construction of such a catalogue was               
therefore undertaken. This project is being carried out at the                  
Observatoire Royal de Belgique (Dommanget 1983, 1989), under the name           
of the `Catalogue of Components of Double and Multiple Stars' (CCDM).           
The original basis of this catalogue is the Index Catalogue of Visual           
Double Stars (Jeffers \ETAL\ 1963) augmented by a number of                     
measurements collected at the US Naval Observatory by C.E.~Worley and           
transmitted to the Meudon (later to the Nice) and Royal Greenwich               
Observatories until 1976. For logistical reasons, the WDS (Washington           
Visual Double Star Catalog, Worley \& Douglass 1984) was not used. The          
CCDM has been complemented during the years 1982-91 by more than                
40\,000 accurate positions and proper motions for individual                    
components, compiled at the Astronomisches Rechen-Institut at                   
Heidelberg (CDA, Bastian \& Lederle 1985) or observed within the                
framework of the INCA Consortium Working Group on Double Stars.                 
                                                                                
\medskip                                                                        
The CCDM includes about 63\,000 systems, and aims to provide                    
(for each component) accurate positions (better than one arcsec),               
proper motions, and cross-identifications with the most important               
reference and fundamental catalogues.                                           
                                                                                
\vfill\eject                                                                    
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\huge\bf Annex 1 description}                                           
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{Annex 1, Fields 1-3:  Component Identification}                       
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{1}{CCDM number}                                                         
%++++++++++++++++++++++++                                                       
                                                                                
The CCDM number is constructed from a mean (approximate) position of            
the system ( $\alpha$ to a precision of 0.1~min, $\delta$ to a                  
precision of 1 arcmin) referred to equinox and epoch J2000.0 (or                
equinox J2000.0 and the epoch of the original measurement if no proper          
motion is available).                                                           
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{2, 1st character}{Reference component when different from A}            
%++++++++++++++++++++++++                                                       
                                                                                
This field specifies the component with respect to which the                    
position angle and separation of the secondary component(s) are given           
in fields 8 and 9. A blank indicates that the reference component is            
the `A' component of the system.                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{2, 2nd character}{Component considered}                                 
%++++++++++++++++++++++++                                                       
                                                                                
This field specifies the component considered (letters A, B,                    
C..., P, Q...), taken from the CCDM.                                            
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{3}{Hipparcos Input Catalogue (HIC) running number}                      
%++++++++++++++++++++++++                                                       
                                                                                
This running number is that of the corresponding entry in the                   
main Hipparcos Input Catalogue.                                                 
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{Annex 1, Fields 4-5:  Position (Equinox J2000.0)}                     
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{4}{Right ascension (equinox J2000.0)}                                   
%++++++++++++++++++++++++                                                       
                                                                                
The right ascension is given for equinox J2000.0. The epoch is                  
J2000.0, or that of the original measurement if no proper motion is             
available. The epoch is not given in Annex 1.                                   
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{5}{Declination (equinox J2000.0)}                                       
%++++++++++++++++++++++++                                                       
                                                                                
The declination is given for equinox J2000.0. The epoch is                      
J2000.0, or that of the original measurement if no proper motion is             
available. The epoch is not given in Annex 1.                                   
                                                                                
\begin{SMALLFIELD}                                                              
The positions in Annex 1 are taken from the CCDM (see                           
Introduction), and are not necessarily identical to those given in the          
Main Catalogue. The `absolute' positions in the CCDM are themselves             
taken from various sources, but primarily from the CDA (Catalogue des           
Donn\'ees Astrom\'etriques, Bastian \& Lederle 1985; Jahrei\ss~ 1989).          
In addition, specific astrometric observations were organised within            
the framework of a dedicated Working Group of the INCA Consortium.              
Numerous institutes participated in these observations:  Observatoire           
Royal de Belgique, Bonn, Bordeaux, Brera, and Turin Observatories,              
Cambridge, La Plata, Leningrad, Lille and M\"unchen Universities with           
observations also made at ESO and at La Palma. New data have been               
included, first into the CCDM, and then into the INCA data base, after          
systematic checks of their internal consistency. Some positions are             
also taken from the Guide Star Catalog (Lasker \ETAL\  1990). Further           
details of the INCA Consortium's preparatory work on double and                 
multiple stars are given by Dommanget (1983, 1985, 1988, 1989).                 
                                                                                
\medskip                                                                        
Preference has always been given to source catalogues or new                    
observations giving positions for the largest number of components, so as to    
maximise the internal consistency of the data on the system. This explains      
some of the discrepancies with the main catalogue where updated data (related   
to the components observed by Hipparcos) have been included, even               
though these were available for only some of the components of a                
system.                                                                         
                                                                                
\medskip                                                                        
For systems closer than 3 arcsec, the same position and proper                  
motion are adopted for all components, unless separate data have been           
explicitly published. For larger separations, when no absolute position         
was available for the secondary component(s), these have been computed          
from the absolute position of the primary and the relative position of          
the secondary. In the case of orbital pairs, the same proper motion is          
also adopted for all components, even for separations larger than 3             
arcsec, except for a few cases with large separations but slow relative         
motions. Ephemerides are given below                                            
for three exceptional cases. The                                                
values of $\Delta\alpha$ and $\Delta\delta$ have                                
been obtained from the orbital elements given by van den Bos (1960) for         
Sirius, by Strand (1951) for Procyon, and by Heintz (1960)                      
for $\alpha$ Centauri.                                                          
                                                                                
\begin{table}[htb]                                                              
\begin{center}                                                                  
\CENTER {Ephemerides for three orbital pairs}\label{table:ephem}                
\begin{tabular}{rrrrrrrrrrrrr}                                                  
\\                                                                              
&\multicolumn{4}{c}{HIC 32349}&                                                 
\multicolumn{4}{c}{HIC 37279}&\multicolumn{4}{c}{HIC 71683 - HIC 71681}\\       
&\multicolumn{4}{c}{Sirius}&                                                    
\multicolumn{4}{c}{Procyon}&\multicolumn{4}{c}{$\alpha$ Centauri}\\             
&\multicolumn{4}{c}{CCDM 06451-1643 A\&B}&                                      
\multicolumn{4}{c}{CCDM 07393+0514 A\&B}&                                       
\multicolumn{4}{c}{CCDM 14396-6050 A\&B}\\                                      
\\ \hline \\                                                                    
&\multicolumn{2}{c}{A - centre}&\multicolumn{2}{c}{A - centre}&                 
\multicolumn{2}{c}{A - centre}&\multicolumn{2}{c}{A - centre}&                  
\multicolumn{2}{c}{A - centre}&\multicolumn{2}{c}{A - centre}\\                 
&\multicolumn{2}{c}{of gravity}&\multicolumn{2}{c}{of gravity}&                 
\multicolumn{2}{c}{of gravity}&\multicolumn{2}{c}{of gravity}&                  
\multicolumn{2}{c}{of gravity}&\multicolumn{2}{c}{of gravity}\\                 
\\ \hline \\                                                                    
Date&$\Delta\alpha$&$\Delta\delta$&$\Delta\alpha$&$\Delta\delta$&               
$\Delta\alpha$&$\Delta\delta$&$\Delta\alpha$&$\Delta\delta$&                    
$\Delta\alpha$&$\Delta\delta$&$\Delta\alpha$&$\Delta\delta$\\                   
&(s)&($\prime\prime$)&(s)&($\prime\prime$)&(s)&($\prime\prime$)&                
(s)&($\prime\prime$)&(s)&($\prime\prime$)&(s)&($\prime\prime$)\\                
\\ \hline \\                                                                    
1990&- 0.01&- 1.5&+0.02&+3.0&- 0.03&- 1.3&+0.09&+3.5&+0.67&+7.2&- 0.86&- 9.1\\  
1991&+0.01&- 1.2&- 0.03&+2.4&- 0.04&- 1.2&+0.11&+3.4&+0.67&+7.0&- 0.85&- 8.8\\  
1992&+0.04&- 0.8&- 0.07&+1.7&- 0.05&- 1.2&+0.13&+3.2&+0.66&+6.8&- 0.84&- 8.6\\  
1993&+0.05&- 0.3&- 0.11&+0.7&- 0.06&- 1.1&+0.15&+3.0&+0.66&+6.5&- 0.83&- 8.3\\  
1994&+0.06&+0.2&- 0.12&- 0.3&- 0.06&- 1.0&+0.17&+2.8&+0.65&+6.3&- 0.82&- 8.0\\  
1995&+0.06&+0.6&- 0.12&- 1.3&- 0.07&- 0.9&+0.18&+2.5&+0.64&+6.0&- 0.81&- 7.7\\  
1996&+0.04&+1.0&- 0.08&- 2.0&- 0.07&- 0.8&+0.20&+2.2&+0.63&+5.8&- 0.80&- 7.3\\  
1997&+0.02&+1.2&- 0.04&- 2.5&- 0.08&- 0.7&+0.21&+1.9&+0.62&+5.5&- 0.78&- 7.0\\  
1998&- 0.01&+1.3&+0.01&- 2.7&- 0.08&- 0.6&+0.22&+1.6&+0.60&+5.2&- 0.77&- 6.6\\  
1999&- 0.03&+1.3&+0.06&- 2.7&- 0.08&- 0.4&+0.22&+1.2&+0.59&+4.9&- 0.75&- 6.3\\  
2000&- 0.05&+1.3&+0.11&- 2.7&- 0.08&- 0.3&+0.22&+0.8&+0.58&+4.6&- 0.73&- 5.9\\  
\\ \hline \\                                                                    
\end{tabular}                                                                   
\end{center}                                                                    
\end{table}                                                                     
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{Annex 1, Field 6: Photometry}                                         
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{6}{Magnitude}                                                           
%++++++++++++++++++++++++                                                       
                                                                                
The magnitude given in this field is taken from the CCDM. It is                 
generally the original magnitude from the IDS (Index Catalogue of               
Visual Double Stars, Jeffers \ETAL\ 1963, updated, up to 1976, at               
Meudon, Nice and Brussels Observatories from new measurements collected         
by C.E. Worley). In most cases it is a $V$ magnitude, since                     
many of these magnitudes are visual estimates. For the faintest                 
systems, it can be a photographic magnitude if the system has been              
discovered photographically. However, the type of magnitude is not              
specified in the IDS, and is therefore not given here.                          
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{Annex 1, Fields 7-10: System Geometry}                                
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{7}{Date of observation of the relative position (for                    
separations smaller than 10 arcsec)}                                            
%++++++++++++++++++++++++                                                       
                                                                                
The field is blank for separations larger than 10 arcsec. In                    
this case, the relative position is obtained from the position of each          
component as given in fields 4 and 5, and it refers to the epochs of            
these data.                                                                     
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{8}{Position angle in degrees (when available)}                          
%++++++++++++++++++++++++                                                       
                                                                                
The position angle is defined with the origin at North, and                     
increasing through increasing right ascension.                                  
                                                                                
\medskip                                                                        
For some stars, only a rough indication of the position angle is                
given and not a value in degrees: F (Following), P (Preceding), N               
(North), S (South), or a combination of these letters.                          
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{9}{Separation in arcsec (when available)}                               
%++++++++++++++++++++++++                                                       
                                                                                
\begin{SMALLFIELD}                                                              
Fields 7-9 provide details of the position of the secondary                     
component(s) with respect to the position of the reference component            
identified by the first character of field 2, and thus provide a concise        
summary of the geometry of the system. For separations smaller than 10          
arcsec, these {\small\it relative} positions are taken from                     
the CCDM and thus from the IDS. For separations larger than 10 arcsec,          
the position angle and separation were deduced from the data on each            
component (for these systems, the relative positions are thus                   
consistent with the absolute positions of the components).                      
                                                                                
\medskip                                                                        
For several thousand double systems, the relative position and                  
proper motion of the secondary components were computed (Brosche \&             
Sinachopoulos 1986, 1988a, 1988b), using all available observations             
communicated by C.E.~Worley from the USNO double star data base.                
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{10, 1st character}{O = system with known orbit}                         
%++++++++++++++++++++++++                                                       
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{10, 2nd character}{A = astrometric binary}                              
%++++++++++++++++++++++++                                                       
                                                                                
\bigskip                                                                        
                                                                                
%-------------------------------------------------                              
\section*{Annex 1, Fields 11-12:  Proper Motion}                                
%-------------------------------------------------                              
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{11}{Proper motion in right ascension}                                   
%++++++++++++++++++++++++                                                       
                                                                                
Proper motion in right ascension, $15\mu_\alpha \cos\delta$,                    
in arcsec per year.                                                             
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{12}{Proper motion in declination}                                       
%++++++++++++++++++++++++                                                       
                                                                                
Proper motion in declination, $\mu_\delta$, in arcsec per year.                 
                                                                                
\begin{SMALLFIELD}                                                              
The proper motions are generally taken from the CCDM. The                       
sources are generally the same as for positions (see explanations given         
under fields 4 and 5, and under fields 7 to 10). As for positions,              
there may be differences between the proper motions given in Annex 1            
and in the main catalogue. The equinox of the proper motion is that of          
the source catalogue (this information is not given in Annex 1).                
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{Annex 1, Fields 13-19:  Cross-Identifications}                        
%-------------------------------------------------                              
                                                                                
For joint systems, some additional identifications, especially                  
for variable and cluster stars, are given in the notes of the main              
Catalogue.                                                                      
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{13}{DM number}                                                          
%++++++++++++++++++++++++                                                       
                                                                                
DM identification numbers for stars in the Bonner Durchmusterung, the           
Cordoba Durchmusterung, and the Cape Photographic Durchmusterung (BD,           
CD or CPD respectively) are given following the HD convention, i.e.             
                                                                                
\begin{itemize}\itemsep=-4pt                                                    
\item when the zone of the DM number is between $+90\degr$ and                  
      $-22\degr$, the BD number is used;                                        
\item when the zone of the DM number is between $-23\degr$ and                  
      $-51\degr$, the CD number is used;                                        
\item when the zone of the DM number is between $-52\degr$ and                  
      $-90\degr$, the CPD number is used.                                       
\end{itemize}                                                                   
                                                                                
                                                                                
\begin{SMALLFIELD}                                                              
The format is $\pm$ ZZ NNNNN, with ZZ indicating the                            
declination zone, and NNNNN denoting a running number.                          
                                                                                
The BD, CD and CPD catalogues overlap, and in the overlapping regions their     
stellar content is not identical. It may thus happen, for example, that some    
stars in the zone $-23\degr >\delta >-51\degr$ only appear in the CPD catalogue.
In such a case, where the HD convention cannot be followed, the available       
number is given, followed by $\ast$ in the last character of this field.        
The last character of this field is also used for additional BD stars, i.e.     
stars with suffix {\it a} or {\it b} (these stars were added to the BD Catalogue
after the original numbering was made). Such identifications do not imply that  
the entry is a component of a double or multiple system.                        
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{14}{HD/HDE number}                                                      
%++++++++++++++++++++++++                                                       
                                                                                
Cross-identifications are given to stars in the HD Catalogue (Cannon \&         
Pickering 1918-24, with numbers in the range 1-225300), and its two             
extensions: HDE numbers in the range 225301-272150 (Cannon 1925-36)             
and 272151-359083 (Cannon \& Walton Mayall 1949) respectively.  The             
format is NNNNNN.                                                               
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{15}{AGK3 or SAO number}                                                 
%++++++++++++++++++++++++                                                       
                                                                                
Cross-identifications are given to stars in the AGK3 and SAO                    
Catalogues (the AGK3 number is given preferentially).                           
                                                                                
\begin{center}                                                                  
\begin{tabular}{lll}                                                            
Catalogue & Reference & Format\\                                                
AGK3 & Dieckvoss \ETAL\ (1975) & $\pm$ DD NNNN\\                                
SAO & Smithsonian Institution (1966) & NNNNNN\\                                 
\end{tabular}                                                                   
\end{center}                                                                    
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{16}{IDS number}                                                         
%++++++++++++++++++++++++                                                       
                                                                                
Cross-identifications are given to (double or multiple) stars                   
in the IDS Catalogue (Jeffers \ETAL\ 1963). The IDS number is                   
constructed from approximate positions at equinox B1900.0, with                 
component indication. The format is HHMMm X DDMM A (where X = N or S).          
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\SUBSEC{17}{ADS number}                                                         
%++++++++++++++++++++++++                                                       
                                                                                
Cross-identifications are given to (double or multiple) stars                   
in the ADS Catalogue (Aitken 1932). The format is NNNNN.                        
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\section*{Acknowledgements}                                                     
%++++++++++++++++++++++++                                                       
                                                                                
Special mention should be made of the contribution of                           
amateur astronomers to the identification of some doubtful systems by           
visual or photographic observations (the `Commission des Etoiles                
Doubles' of the Soci\'et\'e Astronomique de France, and the German              
group coordinated by the Astronomisches Rechen-Institut in Heidelberg).         
These new data have been included in the CCDM since 1984.                       
                                                                                
                                                                                
                                                                                
%++++++++++++++++++++++++                                                       
\section*{References}                                                           
%++++++++++++++++++++++++                                                       
                                                                                
\begin{PRETTYREF}                                                               
 ~                                                                              
                                                                                
Aitken R.G., 1932, New General Catalogue of Double Stars                        
within 120$\degr$ of the North Pole, Carnegie Inst. Washington                  
                                                                                
Bastian U., Lederle T., 1985, Proc. Aussois Coll.  `Scientific                  
Aspects of the Input Catalogue Preparation', Turon C. \& Perryman               
M.A.C. (eds), ESA SP-234, 185                                                   
                                                                                
van den Bos W.H., 1960, Journal des Observateurs, 43, 145                       
                                                                                
Brosche P., Sinachopoulos D., 1986, Astron. Astrophys., 65, 189                 
                                                                                
Brosche P., Sinachopoulos D., 1988a, Astrophys. Space Sci., 142, 255            
                                                                                
Brosche P., Sinachopoulos D., 1988b, Bull. Inf. CDS, 34, 39                     
                                                                                
Cannon A.J., 1925-36, The Henry Draper Extension I, Ann.                        
Astron. Obs. Harvard College, Vol. 100                                          
                                                                                
Cannon A.J., Pickering, E.C., 1918-24, The Henry Draper                         
Catalogue, Ann. Astron. Obs. Harvard College, Vol. 91-99                        
                                                                                
Cannon A.J., Walton Mayall M., 1949, The Henry Draper Extension II, Ann.        
Astron. Obs. Harvard College, Vol. 112                                          
                                                                                
Dieckvoss W., Kox H., Gunther A., Brosterhus E, 1975,                           
The AGK3 catalogue of positions and proper motions north of -                   
2$\degr.5$ declination, Vols 1-8, Hamburg-Bergedorf                             
                                                                                
Dommanget J., 1983, Bulletin d'Information du Centre de Donn\'ees               
Stellaire, Strasbourg, 24, 83                                                   
                                                                                
Dommanget J., 1985, Proc. Aussois Coll. `Scientific Aspects of the              
Input Catalogue Preparation', Turon C. \& Perryman M.A.C. (eds), ESA            
SP-234, 153                                                                     
                                                                                
Dommanget J., 1988, Proc. Sitges Coll. `Scientific                              
Aspects of the Input Catalogue Preparation', Torra J. \& Turon C.               
(eds), 191                                                                      
                                                                                
Dommanget J., 1989, ESA SP-1111, Vol. II, 149                                   
                                                                                
Heintz W., 1960, Ver\"off.  Sternwarte M\"unchen, 5, 10                         
                                                                                
Jahrei\ss~ H., 1989, ESA SP-1111, Vol. II, 115                                  
                                                                                
Jeffers H.M., van den Bos W.H., Greeby F.M., 1963, Index                        
Catalogue of Visual Double Stars, Univ.  California, Publ. Lick Obs.,           
Vol. XXI                                                                        
                                                                                
Lasker B.M., Sturch C.R., McLean B.J., Russell J.L.,                            
Jenkner H., Shara, M.M., 1990, Astron. J. 99, 2019                              
                                                                                
Smithsonian Institution, 1966, Smithsonian Astrophysical                        
Observatory Star Catalogue, Washington D.C.                                     
                                                                                
Strand K.Aa., 1951,Astrophys. J 113, 1                                          
                                                                                
Worley C.E., Douglass G.G., 1984, Washington                                    
Catalog of Visual Double Stars 1984.0, US Naval Observatory                     
                                                                                
\end{PRETTYREF}                                                                 
                                                                                
                                                                                
                                                                                
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\LARGE\bf Executive and Steering Committees \\of the INCA Consortium}   
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
                                                                                
%-------------------------------------------------                              
\section* {The Executive Committee}                                             
%-------------------------------------------------                              
                                                                                
\small                                                                          
                                                                                
The work of the Input Catalogue Consortium is supervised and                    
managed by the Team Leader, Dr~Catherine Turon, of the Observatoire de          
Paris, Meudon. The work has been divided into six main tasks, the               
leaders and description of which are as follows:                                
                                                                                
\BEGTAB                                                                         
Cr\a'{e}z\a'{e}, M. \> Besan\c{c}on \> Mission simulations \\                   
Egret, D. \> Strasbourg \> Collection, analysis and homogenisation of           
astrophysical data \\                                                           
G\a'{o}mez, A. \> Meudon \> Management of proposals                             
and versions of the Input Catalogue \\                                          
Grenon, M. \> Gen\a`{e}ve \> New                                                
ground-based photometric observations and calibrations \\                       
Jahrei\ss~, H.\UPNOTE{1} \> Heidelberg \>                                       
Astrometric data collection, analysis and reduction to FK5\\                    
R\a'{e}qui\a`{e}me, Y. \> Bordeaux \> New ground-based astrometric              
observations and measurements                                                   
\ENDTAB                                                                         
\UPNOTE{1} Previously T. Lederle, Heidelberg                                    
                                                                                
\bigskip\noindent                                                               
In addition, four INCA Working Groups were established to                       
coordinate the work performed in particular subject areas, and two              
astronomers undertook the selection of stars to be observed by                  
Hipparcos in particularly dense areas of the sky:                               
                                                                                
\BEGTAB                                                                         
Argue, A.N. \> Cambridge \> Linking to an extragalactic frame \\                
Bec-Borsenberger, A. \> Paris \> Minor planets and satellites \\                
Dommanget, J. \> Bruxelles \> Double and multiple stars \\                      
Mennessier, M.O. \> Montpellier \> Variable stars \\                            
Mermilliod, J.C. \> Lausanne \> Stars in selected galactic clusters \\          
Pr\a'{e}vot, L.  \> Marseille \> Stars in the Magellanic Clouds \\              
\ENDTAB                                                                         
\noindent                                                                       
These task and working group leaders constitute the                             
Executive Committee of the INCA Consortium.                                     
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{The Steering Committee}                                               
%-------------------------------------------------                              
                                                                                
The activities of the Input Catalogue Consortium are monitored                  
by the INCA Steering Committee, comprising representatives of the               
participating countries, originally composed ($1982-88$) as follows:            
                                                                                
\medskip\noindent                                                               
Belgium \hfill J. Dommanget, Bruxelles \\                                       
France \hfill J.  Delhaye, Paris \\                                             
Germany \hfill W. Fricke (Chairman), Heidelberg \\                              
Netherlands \hfill R.S. Le Poole, Leiden \\                                     
Spain \hfill J.J. de Or\'us, Barcelona \\                                       
Switzerland \hfill F. Rufener, Gen\a`{e}ve \\                                   
United Kingdom \hfill C.A. Murray, (formerly) Herstmonceux                      
                                                                                
\bigskip\noindent                                                               
>From 1988, the Steering Committee was re-organised as follows:                 
                                                                                
\medskip\noindent                                                               
Belgium \hfill J. Dommanget (Chairman), Bruxelles \\                            
France \hfill J. Delhaye, Paris \\                                              
Germany \hfill R. Wielen, Heidelberg \\                                         
Netherlands \hfill R.S. Le Poole, Leiden \\                                     
Spain \hfill J. Torra, Barcelona \\                                             
Switzerland \hfill M. Mayor, Gen\a`{e}ve \\                                     
United Kingdom \hfill C.A. Murray, (formerly) Herstmonceux                      
                                                                                
                                                                                
\vfill\eject                                                                    
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\LARGE\bf Members of the INCA Consortium}                               
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
\bigskip                                                                        
                                                                                
%-------------------------------------------------                              
\section*{Main Participants}                                                    
%-------------------------------------------------                              
                                                                                
\begin{SMALLFIELD}                                                              
\medskip\noindent                                                               
{\bf Belgium: }                                                                 
\BEGTAB                                                                         
Dommanget, J. \> Observatoire Royal de Belgique, Bruxelles \\                   
Lampens, P. \> Observatoire Royal de Belgique, Bruxelles \\                     
Manfroid, J. \> Institut d'Astronomie, Li\a`{e}ge \\                            
Nys, O. \> Observatoire Royal de Belgique, Bruxelles \\                         
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf Denmark: }                                                                 
\BEGTAB                                                                         
Helmer, L. \> Astronomisk Observatorium, Brorfelde \\                           
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf Federal Republic of Germany: }                                             
\BEGTAB                                                                         
Brosche, P. \> Universit\"ats-Sternwarte Bonn, Daun \\                          
Dettbarn, C. \> Astronomisches Rechen-Institut, Heidelberg \\                   
Fricke, W. $\dag$ \> Astronomisches Rechen-Institut, Heidelberg \\              
Jahrei\ss~, H. \> Astronomisches Rechen-Institut, Heidelberg \\                 
Lederle, T. \> Astronomisches Rechen-Institut, Heidelberg \\                    
Schwan, H. \> Astronomisches Rechen-Institut, Heidelberg \\                     
Tucholke, H.-J. \> Astronomisches Institut, Universit\"at M\"unster \\          
Vegt, C. de \> Hamburger Sternwarte, Hamburg \\                                 
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf France: }                                                                  
\BEGTAB                                                                         
Arenou, F. \> Observatoire de Paris, Meudon \\                                  
Arlot, J.E. \> Bureau de Longitudes, Paris \\                                   
Baglin, A.  \> Observatoire de Paris, Meudon \\                                 
Barth\a`{e}s D. \> Equipe d'Astrophysique, Montpellier \\                       
Bec-Borsenberger, A. \> Bureau des Longitudes, Paris \\                         
Chareton, M. \> Observatoire de Besan\c{c}on \\                                 
Cordoni, J.P. \> Equipe d'Astrophysique, Montpellier \\                         
Cr\a'{e}z\a'{e}, M. \> CDS, Observatoire de Strasbourg \\                       
Crifo, F. \> Observatoire de Paris, Meudon \\                                   
Delhaye, J. \> Observatoire de Paris, Meudon \\                                 
Egret, D. \> CDS, Observatoire de Strasbourg \\                                 
G\a'{o}mez, A. \> Observatoire de Paris, Meudon \\                              
Grenier, S. \> Observatoire de Paris, Meudon \\                                 
Mazurier, J.M. \> Observatoire de Bordeaux \\                                   
Mennessier, M.O. \> Equipe d'Astrophysique, Montpellier \\                      
Morin, D. \> Observatoire de Paris, Meudon \\                                   
Oblak, E. \> Observatoire de Besan\c{c}on \\                                    
Pr\a'{e}vot, L. \> Observatoire de Marseille \\                                 
Rapaport, M. \> Observatoire de Bordeaux \\                                     
R\a'{e}qui\a`{e}me, Y. \> Observatoire de Bordeaux \\                           
Rousseau, M. \> Observatoire de Bordeaux \\                                     
Souli\a'{e}, G. \> Observatoire de Bordeaux \\                                  
Turon, C. \> Observatoire de Paris, Meudon \\                                   
\ENDTAB                                                                         
                                                                                
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf The Netherlands: }                                                         
\BEGTAB                                                                         
Lub, J. \> Sterrewacht, Leiden \\                                               
Le Poole, R.  \> Sterrewacht, Leiden \\                                         
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf Spain: }                                                                   
\BEGTAB                                                                         
Figueras, F. \> Universitat de Barcelona \\                                     
Jordi C.  \> Universitat de Barcelona \\                                        
Or\a'{u}s, J.J. de \> Universitat de Barcelona \\                               
Quijano, L \> Real Instituto y Observatorio de la Armada, San Fernando \\       
Torra, J. \> Universitat de Barcelona \\                                        
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf Switzerland: }                                                             
\BEGTAB                                                                         
Burnet, M. \> Observatoire de Gen\a`{e}ve \\                                    
Grenon, M. \> Observatoire de Gen\a`{e}ve \\                                    
Mermilliod, J.C. \> Institut d'Astronomie, Lausanne \\                          
Nicolet, B. \> Observatoire de Gen\a`{e}ve \\                                   
Pernier, B. \> Observatoire de Gen\a`{e}ve \\                                   
Rufener, F. \> Observatoire de Gen\a`{e}ve \\                                   
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf United Kingdom: }                                                          
\BEGTAB                                                                         
Argue, A.N. \> University of Cambridge \\                                       
Morrison, L.V.  \> Royal Greenwich Observatory, Cambridge \\                    
Murray, C.A.  \> (formerly) Royal Greenwich Observatory, Herstmonceux \\        
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf U.S.A.: }                                                                  
\BEGTAB                                                                         
Hemenway, P.D. \> University of Texas \\                                        
Mattei J.A. \> AAVSO, USA \\                                                    
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip                                                                        
\end{SMALLFIELD}                                                                
                                                                                
                                                                                
%-------------------------------------------------                              
\section*{Occasional Observers and Participants}                                
%-------------------------------------------------                              
                                                                                
\begin{SMALLFIELD}                                                              
\medskip\noindent                                                               
{\bf Argentina: }                                                               
\BEGTAB                                                                         
Perdomo, R. \> Universidad de La Plata \\                                       
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf Australia: }                                                               
\BEGTAB                                                                         
Jauncey, D.L. \> Australia Telescope National Facility, CSIRO, Epping \\        
White, G.L. \> Australia Telescope National Facility, CSIRO, Epping \\          
\ENDTAB                                                                         
                                                                                
\vfill\eject                                                                    
                                                                                
\medskip\noindent                                                               
{\bf Belgium: }                                                                 
\BEGTAB                                                                         
Sinachopoulos, D. \> Observatoire Royal de Belgique, Bruxelles \\               
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf Denmark: }                                                                 
\BEGTAB                                                                         
Fabricius, C. \> Astronomisk Observatorium, Brorfelde \\                        
Petersen, C. \> Astronomisk Observatorium, K{\o}benhavn \\                      
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf Federal Republic of Germany: }                                             
\BEGTAB                                                                         
Schmeidler, F. \> Institut f\"ur Astronomie, Universit\"at M\"unchen \\         
Walter, H.G. \> Astronomisches Rechen-Institut, Heidelberg \\                   
Zacharias, N. \> Hamburger Sternwarte, Hamburg \\                               
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf France: }                                                                  
\BEGTAB                                                                         
Bacchus, P. \> Universit\a'{e} de Lille \\                                      
Ochsenbein F. \> CDS, Observatoire de Strasbourg \\                             
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf The Netherlands: }                                                         
\BEGTAB                                                                         
Geus, E. de \> Sterrewacht, Leiden \\                                           
Hartman, L. \> Sterrewacht, Leiden \\                                           
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf Spain: }                                                                   
\BEGTAB                                                                         
Calaf, J. \> Universitat Polit\a`{e}cnica de Catalunya \\                       
Mui\~nos L. \> Real Instituto y Observatorio de la Armada, San Fernando \\      
N\a'{u}\~nez, J. \> Universitat de Barcelona \\                                 
Paredes, J.M. \> Universitat de Barcelona \\                                    
Rossell\a'{o}, G. \> Universitat de Barcelona \\                                
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf United Kingdom: }                                                          
\BEGTAB                                                                         
Argyle R.W. \> Royal Greenwich Observatory, Cambridge \\                        
Benn, C.J. \> Royal Greenwich Observatory, Cambridge \\                         
Leeuwen, F. van \> Royal Greenwich Observatory, Cambridge \\                    
Penston, M.J. \> Royal Greenwich Observatory, Cambridge \\                      
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf U.S.A.: }                                                                  
\BEGTAB                                                                         
Florkowski, D.R. \> U.S. Naval Observatory, Washington D.C. \\                  
Johnston, K.J. \> Naval Research Laboratory, Washington D.C. \\                 
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip\noindent                                                               
{\bf U.S.S.R.: }                                                                
\BEGTAB                                                                         
Anosova J.P. \> St Petersbourg \\                                               
\ENDTAB                                                                         
                                                                                
\end{SMALLFIELD}                                                                
                                                                                
\medskip\noindent                                                               
                                                                                
%-------------------------------------------------                              
\section*{Contributors to the Tasks and Working Groups}                         
%-------------------------------------------------                              
                                                                                
\begin{SMALLFIELD}                                                              
                                                                                
\medskip\noindent                                                               
The names of all persons who have contributed to the work of                    
the INCA Consortium are listed here according to task or working                
group.                                                                          
                                                                                
\bigskip\noindent                                                               
{\bf (a) Management of proposals and versions of the                            
Input Catalogue: }                                                              
\BEGTAB                                                                         
G\a'{o}mez, A. \> Task Leader \> Observatoire de Paris, Meudon \\               
\medskip\noindent                                                               
Arenou, F. \> \> Observatoire de Paris, Meudon \\                               
Baylac, M.O. \> \> Observatoire de Paris, Meudon \\                             
Crifo, F. \> \> Observatoire de Paris, Meudon \\                                
Delhaye, J. \> \> Observatoire de Paris, Meudon \\                              
Grenier, S. \> \> Observatoire de Paris, Meudon \\                              
Marouard, M. \> \> Observatoire de Paris, Meudon \\                             
Mekkas, M. \> \> Observatoire de Paris, Meudon \\                               
Morin, D. \> \> Observatoire de Paris, Meudon \\                                
Sellier, A. \> \> Observatoire de Paris, Meudon \\                              
Turon, C. \> \> Observatoire de Paris, Meudon \\                                
\ENDTAB                                                                         
                                                                                
                                                                                
\bigskip\noindent                                                               
{\bf (b) Astrometric data collection, analysis and                              
reduction to FK5: }                                                             
\BEGTAB                                                                         
Jahrei\ss~, H. \> Task Leader \> Astronomisches Rechen-Institut,                
Heidelberg \\                                                                   
\medskip\noindent                                                               
Bastian, U. \> \> Astronomisches Rechen-Institut, Heidelberg \\                 
Dettbarn, C. \> \> Astronomisches Rechen-Institut, Heidelberg \\                
Erbach, M. \> \> Astronomisches Rechen-Institut, Heidelberg \\                  
Fricke, W.$\dag$ \> \> Astronomisches Rechen-Institut, Heidelberg \\            
Lederle, T. \> \> Astronomisches Rechen-Institut, Heidelberg \\                 
Schwan, H. \> \> Astronomisches Rechen-Institut, Heidelberg \\                  
Vegt, C. de \> \> Hamburger Sternwarte, Hamburg \\                              
\ENDTAB                                                                         
                                                                                
                                                                                
\bigskip\noindent                                                               
{\bf (c) Collection, analysis and homogenisation of                             
astrophysical data: }                                                           
\BEGTAB                                                                         
Egret, D. \> Task Leader \> CDS, Observatoire de Strasbourg \\                  
\medskip\noindent                                                               
Ochsenbein, F. \> \> CDS, Observatoire de Strasbourg \\                         
Wenger, M. \> \> CDS, Observatoire de Strasbourg \\                             
\ENDTAB                                                                         
                                                                                
                                                                                
\bigskip\noindent                                                               
{\bf (d) New ground-based astrometric observations and                          
measurements: }                                                                 
\BEGTAB                                                                         
R\a'{e}qui\a`{e}me, Y. \> Task Leader \> Observatoire de Bordeaux \\            
\medskip\noindent                                                               
Argyle, R.W; \> \> Royal Greenwich Observatory \\                               
Benn, C.J. \> \> Royal Greenwich Observatory \\                                 
Bosq, F. \> \> Observatoire de Bordeaux \\                                      
Busset, J.P. \> \> Observatoire de Bordeaux \\                                  
Fabricius, C. \> \> Astronomisk Observatorium, Brorfelde \\                     
Gachard, M.T. \> \> Observatoire de Bordeaux \\                                 
Geus, E. de \> \> Sterrewacht, Leiden \\                                        
Gibbs, P. \> \> Royal Greenwich Observatory \\                                  
Hartman, L. \> \> Sterrewacht, Leiden \\                                        
Helmer, L. \> \> Astronomisk Observatorium, Brorfelde \\                        
Le Campion, J.E. \> \> Observatoire de Bordeaux \\                              
Leeuwen, F. van \> \> Royal Greenwich Observatory \\                            
Mazurier, J.M. \> \> Observatoire de Bordeaux \\                                
McLean, B. \> \> Space Telescope Science Institute, USA \\                      
Montignac, G. \> \> Observatoire de Bordeaux \\                                 
Morrison, L.V. \> \> Royal Greenwich Observatory \\                             
Mui\~nos, J.L. \> \> Real Instituto y Observatorio de la Armada, San Fernando \\
Murray, C.A. \> \> Royal Greenwich Observatory \\                               
Penston, M.J. \> \> Royal Greenwich Observatory \\                              
P\a'{e}ri\a'{e}, J.P. \> \> Observatoire de Bordeaux \\                         
Peyrin, Y.  \> \> Observatoire de Marseille \\                                  
Poole, R.S. Le \> \> Sterrewacht, Leiden \\                                     
Pr\a'{e}vot, L. \> \> Observatoire de Marseille \\                              
Quijano, L. \> \> Real Instituto y Observatorio de la Armada, San Fernando \\   
Ralite, N. \> \> Observatoire de Bordeaux \\                                    
Rapaport, M. \> \> Observatoire de Bordeaux \\                                  
Robin, A. \> \> Observatoire de Marseille \\                                    
Rousseau, M. \> \> Observatoire de Bordeaux \\                                  
Rousseau, S. \> \> Observatoire de Bordeaux \\                                  
Tellechea, M. \> \> Observatoire de Bordeaux \\                                 
Vegt, C. de \> \> Hamburger Sternwarte, Hamburg \\                              
Zacharias, N. \> \> Hamburger Sternwarte, Hamburg \\                            
\ENDTAB                                                                         
                                                                                
                                                                                
\bigskip\noindent                                                               
{\bf (e) New photometric data compilation, observations, and                    
photometric calibrations: }                                                     
\BEGTAB                                                                         
Grenon, M. \> Task Leader \> Observatoire de Gen\a`{e}ve \\                     
\medskip\noindent                                                               
Bopp, J.F. \> \> Observatoire de Gen\a`{e}ve \\                                 
Bruyn, J.W. de \> \> Sterrewacht, Leiden \\                                     
Burnet, M. \> \> Observatoire de Gen\a`{e}ve \\                                 
Cramer, N. \> \> Observatoire de Gen\a`{e}ve \\                                 
Figueras, F. \> \> Universitat de Barcelona \\                                  
Hartman, L. \> \> Sterrewacht, Leiden \\                                        
Jenniskens, P. \> \> Sterrewacht, Leiden \\                                     
Jordi, C. \> \> Universitat Barcelona \\                                        
Koninx, J.P.  \> \> Sterrewacht, Leiden \\                                      
Langevelde, H.J. van \> \> Sterrewacht, Leiden \\                               
Lub, J. \> \> Sterrewacht, Leiden \\                                            
Manfroid, J. \> \> Institut d'Astronomie, Li\a`{e}ge \\                         
Mermilliod, J.C. \> \> Institut d'Astronomie, Lausanne \\                       
Mermilliod, M. \> \> Institut d'Astronomie, Lausanne \\                         
Nicolet, B. \> \> Observatoire de Gen\a`{e}ve \\                                
N\a'{u}\~nez, J. \> \> Universitat de Barcelona \\                              
Oblak, E. \> \> Observatoire de Besan\c{c}on \\                                 
Pernier, B. \> \> Observatoire de Gen\a`{e}ve \\                                
Petersen, C. \> \> Astronomisk Observatorium, K{\o}benhavn \\                   
Scales, D. \> \> Astronomisches Institut, Universit\"at T\"ubingen \\           
Torra, J. \> \> Universitat de Barcelona \\                                     
\ENDTAB                                                                         
                                                                                
                                                                                
\bigskip\noindent                                                               
{\bf (f) Mission simulations: }                                                 
\BEGTAB                                                                         
Cr\a'{e}z\a'{e} M. \> Task Leader \> Observatoire de Besan\c{c}on \\            
\medskip\noindent                                                               
Bartholdi, P. \> \> Observatoire de Gen\a`{e}ve \\                              
Chareton, M. \> \> Observatoire de Besan\c{c}on \\                              
Feaugas, J.C.  \> \> CNES, Toulouse \\                                          
Nicolet, B. \> \> Observatoire de Gen\a`{e}ve \\                                
Oblak, E. \> \> Observatoire de Besan\c{c}on \\                                 
Roman, V. \> \> CNES, Toulouse \\                                               
\ENDTAB                                                                         
                                                                                
                                                                                
\vfill\eject                                                                    
                                                                                
\bigskip\noindent                                                               
{\bf (g) Double and multiple stars: }                                           
\BEGTAB                                                                         
Dommanget, J. \> Coordinator \> Observatoire Royal de Belgique, Bruxelles \\    
\medskip\noindent                                                               
Anosova, J.P. \> \> Leningrad University \\                                     
Argue, A.N. \> \> Cambridge University \\                                       
Bacchus, P. \> \> Universit\a'{e} de Lille \\                                   
Bastian, U. \> \> Astronomisches Rechen-Institut \\                             
Bourgeois, J. \> \> Observatoire Royal de Belgique, Bruxelles \\                
Bridgeland, M.T. \> \> Cambridge University \\                                  
Brosche, P. \> \> Universit\"ats-Sternwarte Bonn, Daun \\                       
Bunclark, P.S. \> \> Cambridge University \\                                    
Caceres, O.\dag \> \> La Plata Observatory \\                                   
Candy, M.P. \> \> Perth Observatory \\                                          
Guibert, J. \> \> Observatoire de Paris \\                                      
Harmon, R.T. \> \> Cambridge University \\                                      
Hensberge, H. \> \> Leiden Observatory \\                                       
Irwin, M.J. \> \> Cambridge University \\                                       
Jorissen, A. \> \> Observatoire Royal de Belgique, Bruxelles \\                 
Kazeza, S.M.  \> \> Observatoire Royal de Belgique, Bruxelles \\                
Kint, C. \> \> Observatoire Royal de Belgique, Bruxelles \\                     
Lampens, P. \> \> Observatoire Royal de Belgique, Bruxelles \\                  
Leonis, G. \> \> Observatoire Royal de Belgique, Bruxelles \\                   
Louys, L. \> \> Observatoire Royal de Belgique, Bruxelles \\                    
Nithakorn, D.S.	\> \> Cambridge University \\                                   
Nys, O.	\> \> Observatoire Royal de Belgique, Bruxelles \\                      
Oblak, E.	\> \> Observatoire de Besan\c{c}on \\                                 
Orlov, V.V. \> \> Leningrad University \\                                       
Pannunzio, R. \> \> Osservatorio di Pino Torinese \\                            
Perdomo, R. \> \> Universidad de La Plata \\                                    
Scardia, M. \> \> Merate Observatory \\                                         
Schmeidler, E. \> \> Institut f\"ur Astronomie, Universit\"at M\"unchen \\      
Sinachopoulos, D. \> \> Observatoire Royal de Belgique, Bruxelles \\            
Souli\a'{e}, G.  \> \> Observatoire de Bordeaux \\                              
Worley, C.E. \> \> U.S. Naval Observatory, Washington D.C. \\                   
\ENDTAB                                                                         
                                                                                
                                                                                
\bigskip\noindent                                                               
{\bf (h) Variable stars: }                                                      
\BEGTAB                                                                         
Mennessier, M.O. \> Coordinator \> Equipe d'Astrophysique, Montpellier \\       
\medskip\noindent                                                               
Baglin, A. \> \> Observatoire de Paris, Meudon \\                               
Barth\a`{e}s, D. \> \> Equipe d'Astrophysique, Montpellier \\                   
Coll, R. \> \> Equipe d'Astrophysique, Montpellier \\                           
Cordoni, J.P. \> \> Equipe d'Astrophysique, Montpellier \\                      
Figueras, F. \> \> Universitat de Barcelona \\                                  
Mattei, J. \> \> AAVSO, USA \\                                                  
\ENDTAB                                                                         
                                                                                
                                                                                
                                                                                
\bigskip\noindent                                                               
{\bf (i) Linking the Hipparcos frame to an extragalactic frame: }               
\BEGTAB                                                                         
Argue, A.N. \> Coordinator \> Cambridge University, Cambridge \\                
\medskip\noindent                                                               
Brosche, P. \> \> Universit\"ats-Sternwarte Bonn, Daun \\                       
Duncombe, R.L. \> \> University of Texas, Austin \\                             
Estalella, R. \> \> Universidad de Barcelona \\                                 
Florkowski, D.R. \> \> U.S. Naval Observatory, Washington D.C. \\               
Geffert, M. \> \> Universit\"at Bonn \\                                         
Hemenway, P.D. \> \> University of Texas, Austin \\                             
Jauncey, D.L.  \> \> CSIRO, Epping \\                                           
Johnston, K.J. \> \> U.S. Naval Research Laboratory, Washington D.C. \\         
Klemola, A.R. \> \> Lick Observatory \\                                         
Kovalevsky, J. \> \> CERGA, Observatoire de la C\^ote d'Azur, Grasse \\         
Lestrade, J.F. \> \> Bureau des Longitudes, Paris \\                            
Ma, C. \> \> Goddard Space Flight Center \\                                     
Morrison, L.V. \> \> Royal Greenwich Observatory, Cambridge \\                  
Murray, C.A. \> \> (formerly) Royal Greenwich Observatory, Herstmonceux \\      
Paredes, J. \> \> Universitat de Barcelona \\                                   
R\a'{e}qui\a`{e}me, Y. \> \> Observatoire de Bordeaux \\                        
Ruben, G. \> \> Sternwarte Babelsberg, Postdam \\                               
Sinachopoulos, D. \> \> Observatoire Royal de Belgique \\                       
Vegt, C. de \> \> Hamburger Sternwarte, Hamburg \\                              
Walter, H.G. \> \> Astronomisches Rechen-Institut, Heidelberg \\                
White, G.L. \> \> CSIRO, Epping \\                                              
\ENDTAB                                                                         
                                                                                
                                                                                
                                                                                
\bigskip\noindent                                                               
{\bf (j) Minor planets and satellites: }                                        
\BEGTAB                                                                         
Bec-Borsenberger, A. \> Coordinator \> Bureau des Longitudes, Paris \\          
\medskip\noindent                                                               
Arlot, J.E. \> \> Bureau des Longitudes, Paris \\                               
Baron, N.  \> \> Bureau des Longitudes, Paris \\                                
Calaf, J. \> \> Universitat de Barcelona \\                                     
Catal\a`{a}, M.A. \> \> Universitat de Barcelona \\                             
Chareton, M. \> \> Observatoire de Besan\c{c}on \\                              
Jordi, C. \> \> Universitat de Barcelona \\                                     
Morrison, L.V. \> \> Royal Greenwich Observatory, Cambridge \\                  
Mui\~nos, J.-L. \> \> Observatorio de Marina, San Fernando \\                   
N\a'{u}\~nez, J. \> \> Universitat de Barcelona \\                              
Quijano, L. \> \> Observatorio de Marina, San Fernando \\                       
Rapaport, M. \> \> Observatoire de Bordeaux \\                                  
R\a'{e}qui\a`{e}me, Y. \> \> Observatoire de Bordeaux \\                        
Rossell\a'{o}, G. \> \> Universitat de Barcelona \\                             
Ruatti, C. \> \> Bureau des Longitudes, Paris \\                                
Sala, F. \> \> Universitat de Barcelona \\                                      
Schmadel, L. \> \> Astronomisches Rechen-Institut, Heidelberg \\                
Scholl, H. \> \> Observatoire de la C\^ote d'Azur, Nice \\                      
Torra, J. \> \> Universitat de Barcelona \\                                     
\ENDTAB                                                                         
                                                                                
                                                                                
\bigskip\noindent                                                               
{\bf (k) Stars in selected galactic clusters: }                                 
\BEGTAB                                                                         
Mermilliod, J.C. \> Coordinator \> Institut d'Astronomie, Lausanne \\           
\medskip\noindent                                                               
Cr\a'{e}z\a'{e}, M. \> \> Observatoire de Besan\c{c}on \\                       
Delhaye, J. \> \> Observatoire de Paris, Meudon \\                              
Dettbarn, C. \> \> Astronomisches Rechen-Institut, Heidelberg \\                
Fehlberg, H.J. \> \> Hamburger Sternwarte, Hamburg \\                           
Saltel, M. \> \> Observatoire de Paris, Meudon \\                               
Sellier, A. \> \> Observatoire de Paris, Meudon \\                              
Tucholke, H.-J. \> \> Astronomisches Institut, Universit\"at M\"unster \\       
Turon, C. \> \> Observatoire de Paris, Meudon \\                                
Vegt, C. de \> \> Hamburger Sternwarte, Hamburg \\                              
Wielen, R. \> \> Astronomisches Rechen-Institut, Heidelberg \\                  
Zacharias, N. \> \> Hamburger Sternwarte, Hamburg \\                            
\ENDTAB                                                                         
                                                                                
                                                                                
\vfill\eject                                                                    
                                                                                
\bigskip\noindent                                                               
{\bf (l) Stars in the Magellanic Clouds: }                                      
\BEGTAB                                                                         
Pr\a'{e}vot, L. \> Coordinator \> Observatoire de Marseille \\                  
\medskip\noindent                                                               
Figon, P. \> \> Observatoire de Marseille \\                                    
Peyrin, Y. \> \> Observatoire de Marseille \\                                   
Rebeirot, E. \> \> Observatoire de Marseille \\                                 
Robin, A. \> \> Observatoire de Marseille \\                                    
\ENDTAB                                                                         
                                                                                
                                                                                
                                                                                
\bigskip\noindent                                                               
The activities on double and multiple stars included the                        
participation of the Commission des Etoiles Doubles (Soci\'et\'e                
Astronomique de France) and of a German group of amateur astronomers            
(Heidelberg).                                                                   
                                                                                
\medskip\noindent                                                               
The variable star work included the participation of the AAVSO                  
staff (USA), AFOEV, CRIM and INRIA (France).                                    
                                                                                
\end{SMALLFIELD}                                                                
\vfill\eject                                                                    
                                                                                
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\LARGE\bf The ESA Hipparcos Scientific Selection Committee}             
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
\bigskip\bigskip\bigskip\noindent                                               
The proposals submitted by the scientific community were                        
reviewed by a peer committee, established under the guidance of the ESA         
Astronomy Working Group. The composition was as follows:                        
                                                                                
\medskip\noindent                                                               
\BEGTAB                                                                         
Prof. A. Blaauw \> ({\it Chairman}) \>  Groningen \\                            
Dr J. Dommanget \> \>  Bruxelles \\                                             
Dr W. Gliese  \> \>  Heidelberg \\                                              
Prof. M. Hack \> \> Trieste \\                                                  
Prof. E.P.J. van den Heuvel \> \>  Amsterdam \\                                 
Prof. C.  Jaschek \> \>  Strasbourg \\                                          
Prof. J. Lequeux \> \>  Paris \\                                                
Prof. P.O. Lindblad \> \>  Stockholm \\                                         
Prof. A. Maeder \> \>  Gen\a`{e}ve \\                                           
Dr P.E. Nissen \> \>  Aarhus \\                                                 
Prof. B.E.J. Pagel \> \> Herstmonceux \\                                        
Dr A. Renzini \> \>  Bologna \\                                                 
Prof. C.  de Vegt \> \>  Hamburg \\                                             
Prof. P.A. Wayman \> \>  Dunsink \\                                             
Prof. R. Wielen  \> \>  Heidelberg                                              
\ENDTAB                                                                         
                                                                                
                                                                                
\medskip                                                                        
This Scientific Selection Committee met on three occasions.  At                 
the first meeting, general priorities were assigned to proposals or             
subsets of the proposals.                                                       
                                                                                
\medskip                                                                        
At the second meeting, after the results of the first round of                  
simulations had been made by the INCA Consortium, and after proposers           
had been invited to comment on the general recommendations of the               
Committee, the preliminary recommendations were reviewed. Members of            
the INCA Consortium presented the simulation results, and the Selection         
Committee recommended topics for further study.                                 
                                                                                
\medskip                                                                        
At the third meeting of the Selection Committee, the INCA                       
Consortium made a detailed presentation of the results of the selection         
process, showing the extent to which various proposals and categories           
of proposals had been included in the Input Catalogue.                          
                                                                                
\medskip                                                                        
The various meetings of the Selection Committee were also                       
attended by the leaders of the Hipparcos Data Reduction Consortia, who          
were able to provide advice on technical aspects of the data analysis           
which might impact on considerations of the Input Catalogue                     
compilation.                                                                    
                                                                                
\medskip                                                                        
In June 1988, the INCA Consortium distributed, to each of the                   
proposal Principal Investigators, a listing of the stars from the               
original proposal finally contained in the Input Catalogue. A second            
opportunity was provided for comments on the listing. In this way,              
since the observing programme for the Hipparcos satellite would not be          
changed throughout the mission, proposers were given the opportunity to         
comment on the selection, achieved amongst the stars they had proposed,         
until just a few months before the satellite's launch.                          
                                                                                
\vfill\eject                                                                    
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\LARGE\bf Scientific Proposals received by ESA}                         
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
\bigskip                                                                        
\CENTER{The following table lists the proposals received by the European \\     
Space Agency as a result of the Invitation for Proposals issued in\\            
1982. For each proposal, the Principal Investigator, institute, \\              
and title of the proposed investigation are listed.}                            
                                                                                
\vfill\eject                                                                    
                                                                                
\PROTABLE                                                                       
143& Acker, A.& Strasbourg& Calibration of the distance                         
scale of planetary nebulae\\                                                    
35& Adelman, S.J.& Charleston,\,USA& The Ursa Major stream\\                    
22& Alksnis, A.& Latvia & Luminosity calibration of carbon                      
stars\\                                                                         
10& Antonello, E.& Milan& Luminosity and related parameters of                  
variable A and F stars ($\delta$ Scuti stars)\\                                 
127& Ardeberg, A.& Lund& Physical parameters and kinematics of                  
late-type stars and the history of the Galaxy\\                                 
26& Argue, A.N.& Cambridge& Super-priority radio stars\TINOTE{1}\\              
56& Argue, A.N.& Cambridge& Link to extragalactic                               
reference frame (via Space Telescope): the southern sky\\                       
210& Argue, A.N.& Cambridge& Radio stars (master list)\\                        
221& Argue, A.N.& Cambridge& Super-high priority 'link' stars\\                 
50& Arlot, J.E.& Paris& Determination of precise positions of                   
faint stars in the ecliptic zone\\                                              
223& Arlot, J.E. & Paris& Observations of Europa and Titan\\                    
52& Aslan, Z.& Ankara, Turkey& Kinematics of RS CVn-type binary                 
stars\\                                                                         
66& Auvergne, M.& Meudon& Dwarf and subgiant A stars\\                          
166& Barbieri, C.& Padova& Search for sub-stellar and planetary                 
masses accompanying the nearest stars\\                                         
57& Bartkevicius, A.&Vilnius,Lithuania& The HR diagram and                      
kinematic properties of F-M field stars with metal deficiency\\                 
103& Bastian, U.& Heidelberg& Parallaxes and proper motions of                  
Herbig-Ae/Be stars\\                                                            
104& Bastian, U.& Heidelberg& Observations of Magellanic Cloud                  
OB supergiants\\                                                                
105& Bastian, U.& Heidelberg& Distances of T Tauri stars\\                      
76& Baudry, A.& Bordeaux& Observations of late-type stars                       
coinciding with radio line masers and of 3C 273B\\                              
43& Benacchio, L.& Padova& Astrometry of the planet Pluto\\                     
179& Bergeat, J.& Lyon& Carbon stars and stellar evolution\\                    
168& Bernacca, P.L.& Asiago& Astrodynamics of trapezia systems                  
from space and ground\\                                                         
88& Bien, R.& Heidelberg& Observations of the fundamental stars                 
of FK4 and of new fundamental stars\\                                           
197& Bonneau, D.& Grasse& Linear geometry of stellar atmospheres\\              
140& Brand, J.& Leiden& Proper motions of Herbig-Haro objects\TINOTE{2}\\       
171& Briot, D.& Paris& Absolute magnitudes and comparative                      
kinematical studies of B and Be stars\\                                         
38& Brosche, P.& Bonn& Extragalactic calibration of the Hipparcos               
proper motion system\\                                                          
42& Brosche, P.& Bonn& Absolute proper motions of thirteen                      
globular clusters\\                                                             
63& Buarque, J.A.& Rio de Janeiro& Stellar orbits in the                        
solar neighbourhood\\                                                           
32& Caprioli, G.& Rome& Improved earth's rotation and polar motion              
since 1968\\                                                                    
209& Carquillat, J.M.& Toulouse& Contribution \`a l'\'etude des                 
\'etoiles \`a spectre composite\\                                               
71& Catchpole, R.M.& SAAO,                                                      
S.~Africa& Astrometric orbit of the spectroscopic binary HD 1273\\              
153& Cayrel, R.& Paris& Kinematics of halo subdwarfs: the clue                  
to early galactic evolution\\                                                   
160&{Cayrel\,de\,Strobel,G}&Meudon& The HR diagram of the Hyades,               
Pleiades, Coma Berenices \& Ursa Major clusters\\                               
157& Chevalier, C& OHP& Kinematical studies of galactic X-ray                   
sources\\                                                                       
69& Clube, S.V.M. & Oxford, UK& Kinematics of early-type stars\\                
60& Cottrell, P.L.& Canterbury, NZ& RCrB and He-rich B stars:                   
are they evolutionary partners?\\                                               
100& Couteau, P. & Nice& Masses of faint visual binary systems\\                
164& Cramer, N.& Gen\`eve& Internal dynamics and ages of                        
Scorpius-Centaurus $\zeta$ Persei and I Lac associations\\                      
172& Cramer, N.& Gen\`eve& Magnetic Ap stars detected by                        
Geneva photometry\\                                                             
189& Cr\'ez\'e, M.& Besan\c{c}on& Kinematics of distant red giants              
in the Galactic plane\\                                                         
158& Delhaye, J.& Meudon& Kinematics, age and chemical composition              
of F, G \& K stars in the Fe/H catalogue\\                                      
159& Delhaye, J.& Meudon& The escape velocity in the vicinity of                
the sun\\                                                                       
146& Divan, L. & Paris& Calibration in absolute magnitudes of the               
BCD spectral classification\\                                                   
196& Dolan, J.F.&{\tiny NASA\,GSFC,\,USA}& Parallaxes of galactic X-ray         
sources\\                                                                       
23& Dommanget, J.& Bruxelles& Les masses stellaires et                          
l'\'evolution des binaires\\                                                    
24& Dommanget, J.& Bruxelles& Les caracteristiques                              
physiques, l'origine et l'\'evolution des binaires spectroscopiques\\           
25& Dommanget, J.& Bruxelles& Duplicit\'es d\'ecouvertes pour                   
certaines \'etoiles lors de leurs occultations par la lune\\                    
54& Dommanget, J.& Bruxelles& Recherches statistiques sur les                   
\'etoiles doubles et multiples proches\\                                        
204& Dommanget, J.& Bruxelles& Recherches statistiques sur les                  
\'etoiles multiples de toutes cat\'egories\\                                    
48& Dravins, D.& Lund& Convection in stellar atmospheres\\                      
82& D\"urbeck, H.W.& Bonn& W UMa-type contact binaries:                         
luminosities, masses, motions and evolution\\                                   
193& Dunham, D.W.& Silver\,Spring,USA& Lunar occultation stars:                 
(1)\,stars from the Zodiacal Catalogue\\                                        
194& Dunham, D.W. & Silver\,Spring,USA& Lunar occultation stars:                
(2)\,stars not in the Zodiacal Catalogue\\                                      
195& Dunham, D.W.& Silver\,Spring,USA&Lunar occultation stars:                  
(3)\,stars from the USNO\,C-Catalogue observed during 1982\\                    
161& Duncombe, R.L. & Austin,\,USA& Dynamical reference for the                 
Hipparcos instrumental system\\                                                 
163& Duncombe, R.L.& Austin,\,USA& Extragalactic reference for the              
Hipparcos instrumental system\\                                                 
137& Egret, D.& Strasbourg& Luminosity of G5-M3 stars near the                  
giant branch\\                                                                  
114& Estalella, R.& Barcelona& Connection of the Hipparcos and                  
extra-galactic reference frame using radio stars\\                              
185& Feast, M.W. & SAAO, S.~Africa& Parallaxes and proper motions               
of Mira variables\\                                                             
186& Feast, M.W.& SAAO, S.~Africa& Parallaxes and proper motions                
of Cepheid variables\\                                                          
79& Feissel, M.& Paris& Earth rotation and continental drift\\                  
80& Feitzinger, J.& Bochum& Proper motion and parallaxes of the                 
Magellanic Cloud stars\\                                                        
217& Florkowski, D.R.& Washington,\,USA& Radio stars\\                          
6& Fracassini, M.& Milan& Absolute radii of stars from the CADARS\\             
7& Fresneau, A.& Strasbourg& The internal velocities of PER OB III cluster      
members\\                                                                       
150& Fringant, A.M.& Paris& Faibles \'etoiles bleues \`a haute latitude         
galactique\\                                                                    
149& Friedjung, M. &Paris& Distances of cataclysmic variables\\                 
120& Gass, H.& Heidelberg& Search for low-luminosity carbon stars\\             
77& Geyer, E.H.& Bonn& Common proper motion investigations of                   
young to medium age stellar troops                                              
\PRFTABLE                                                                       
\vfill\eject                                                                    
\PROTABLE                                                                       
119& Gilmore, G.& Cambridge& Kinematic properties of the galactic               
spheroid\\                                                                      
108& G\'omez, A. & Meudon& Estimation of the gradients of the                   
velocity dispersions\\                                                          
147& G\'omez, A.& Meudon& The stellar luminosity function and                   
quantitative HR diagram\TINOTE{2}\\                                             
29& Goossens, M.& Leuven& Faint early-type stars at high galactic               
latitudes\\                                                                     
122& Grenier, S.& Meudon& Determination of masses for G and K                   
giants\\                                                                        
139& Grenon, M.& Gen\`eve& Physical and kinematical properties of               
halo, old disc and nearby stars from NLTT\\                                     
107& Grosb{\o}l, P.& ESO, Garching& Birthplaces of nearby                       
early-type stars\\                                                              
182& Guibert, J.& Paris& Interstellar reddening and distribution                
of B stars in the solar neighbourhood\\                                         
98& Habing, H.J.& Leiden& Mira variables\\                                      
68& Harrington, R.S.& Washington,\,USA& Comparison of Hipparcos and             
USNO trigonometric parallaxes\\                                                 
55& Hauck, B.& Lausanne &                                                       
Fundamental data for B and A chemically-peculiar stars\\                        
61& Hearnshaw, J.B.& Canterbury, NZ& Eggen's moving groups:                     
fact or fiction?\\                                                              
62& Hearnshaw, J.B.& Canterbury, NZ& Ages and kinematics of the                 
oldest disk stars\\                                                             
28& Heck, A.& Strasbourg& Statistical parallaxes of field RR Lyrae              
stars\\                                                                         
162& Hemenway, P.D.& Austin,\,USA& Galactic distribution and                    
motions of A5-F5 stars\\                                                        
85& Hering, R.& Heidelberg& Observation of early-type stars for                 
investigations of galactic structure\\                                          
81& Hidajat, B. & Java, Indonesia& Astrophysical research on                    
particular visual binaries\\                                                    
83& Hilditch, R.W.& St. Andrews& Studies of O to F8 stars at the                
galactic poles\\                                                                
19& Hobbs, L.M.& Yerkes,\,USA& Interstellar gas and young stars in              
the galactic halo\\                                                             
128& Houziaux, L.& Li\`ege& Peculiar objects:  their positions                  
in the HR diagram\\                                                             
30&Hucht,K.A.van\,der&Utrecht& A proper motion study of                         
evolved massive candidate runaway stars\\                                       
198& Hughes, J.A.& Washington,\,USA& Astrometric parameters of the              
NPZT stars\\                                                                    
199& Hughes, J.A.& Washington,\,USA& Astrometric                                
parameters of the supplement list to the AGK3R and SRS(IRS) lists\\             
200& Hughes, J.A.& Washington,\,USA& Astrometric parameters of the              
AGK3R stars\\                                                                   
201& Hughes, J.A.& Washington,\,USA& Astrometric parameters of the              
SRS list\\                                                                      
44& H{\o}g, E.& Copenhagen& Nature of $\delta$ Scuti variables\\                
64& Ishida, K.& Tokyo, Japan& Kinematical analysis of C- and                    
M-type stars in the solar neighbourhood\\                                       
72& Jahrei\ss~, H.& Heidelberg& Parallaxes for Smethells' red                   
dwarf stars\\                                                                   
73& Jahrei\ss~, H.& Heidelberg& Parallaxes of NLTT stars\TINOTE{2}\\            
89& Jahrei\ss~, H.& Heidelberg& Nearby stars\\                                  
90& Jahrei\ss~, H.& Heidelberg& K and M dwarfs at low galactic                  
latitudes\\                                                                     
91& Jahrei\ss~, H. & Heidelberg& High-velocity stars\\                          
92& Jahrei\ss~, H.& Heidelberg& McCormick K and M dwarfs\\                      
93& Jahrei\ss~, H.& Heidelberg& Southern K and M dwarfs\\                       
212& Jahrei\ss~, H.& Heidelberg& M dwarf stars (Robertson list)\\               
169& Jaschek, C.& Strasbourg& Luminosities and kinematics of                    
spectroscopically-peculiar groups\\                                             
220& Jauncey, D.L. & Epping, Australia& Stars around                            
quasars, $\delta < 40\degr$\\                                                   
208& Kharchenko, N.& Kiev, Ukrania& Studies of the galactic main                
meridional section\\                                                            
15& Kilkenny, D.& SAAO, S.~Africa &                                             
Parallaxes and proper motions of OB stars at high galactic latitudes\\          
21& Kilkenny, D.& SAAO, S.~Africa& Parallaxes and proper motions                
of hot subdwarfs\\                                                              
167& Klare, G.& Heidelberg& Kinematics of young stars within 3~kpc\\            
75& Klemola, A.R.& Lick,\,USA& Comparison of Lick proper motion and             
Hipparcos reference frames\TINOTE{2}\\                                          
205& Klemola, A.R.& Santa Cruz,\,USA& Subset of the Lick comparison             
programme (AGK3 stars)\\                                                        
206& Klemola, A.R.& Santa Cruz,\,USA& Lick proper motion catalogue              
(part)\TINOTE{2}\\                                                              
170& Kovalesky, J.& Grasse& Stars occulted by Uranus and Neptune\\              
207& Kovalevsky, J. & Grasse& RS CVn systems in the southern                    
hemisphere\\                                                                    
156& Krautter, J.& Heidelberg& Evolutionary status of low and                   
medium mass pre-main-sequence stars\\                                           
125& Kristensen, L.K.& Aarhus& Catalogue rotation using (51)                    
Nemausa\\                                                                       
37& Lacy, J.H.& Austin,\,USA& Reference stars near the galactic                 
centre\\                                                                        
59& Laval, A.& Marseille& Expansion of the association Sco OB1\\                
86& Lederle, T.& Heidelberg& Determination of proper motions for                
the IRS and NPZT stars\\                                                        
129& Lequeux, J.& Meudon& Direct distance calibration for stars                 
closer than 500 pc\TINOTE{2}\\                                                  
130& Lequeux, J.& Meudon& Distances and proper motions of runaway               
O-B stars and supergiants\\                                                     
40& Lestrade, J.F.& Paris& Stars around millisecond pulsars                     
\TINOTE{1}\\                                                                    
41& Lod\'en, K.& Stockholm& Kinematics of the local Gould's Belt                
system of early-type stars\\                                                    
78& Lortet, M.C.& Meudon & Wolf-Rayet runaways\\                                
65& Lundstr\"om, I.& Lund& Proper motions                                       
in the region of the open cluster Collinder 121\\                               
117& Lutz, T.E.& Pullman,\,USA& Proper motions of central stars of              
planetary nebulae\\                                                             
152& Lutz, T.E.& Pullman,\,USA& Parallax standard stars\\                       
13& Lynden-Bell, D.& Cambridge& Proper motion of the Magellanic                 
Clouds\\                                                                        
47& Lyng\aa, G.& Lund& Cluster membership of the cepheids S~Nor                 
and U~Sgr\\                                                                     
133& Malyuto, V.& Tartu, Estonia& Determination of absolute                     
magnitudes for spectral classification standard stars\\                         
131& Mayor, M.& Gen\`eve& F stars of all ages as tracers of                     
galactic chemical and dynamical evolution\\                                     
190& Mayor, M.& Gen\`eve& Propri\'et\'es dynamiques et chimiques du             
halo galactique par le biais des sous-naines\\                                  
99& Mennessier, M.O.& Montpellier& Young stars: irregularities of the velocity  
field and spiral structures\\                                                   
148& Mennessier, M.O.& Montpellier& Mira stars and stellar evolution\\          
214& Mermilliod, J.C.& Lausanne& Selected absolute proper motions               
of stars in galactic open clusters\\                                            
215& Mermilliod, J.C.& Lausanne& Stars in NGC 188 (HST calibration              
field)\\                                                                        
97& Mirzoyan, L.V.&Byurakan,Armenia&Nearby OB associations and                  
trapezium-type multiple systems\\                                               
39& Miyamoto, M.& Japan& Kinematics of RR Lyrae stars:  where is                
the galactic mass?\\                                                            
3& Monnet, G.& Lyon& Determination of the `local' rotational                    
angular velocity in our Galaxy                                                  
\PRFTABLE                                                                       
\vfill\eject                                                                    
\PROTABLE                                                                       
184& Murray, C.A.& Herstmonceux& Candidate stars within 100 pc\\                
113& Nicolet, B.& Gen\`eve& Evolution stage of the Am stars\\                   
101& N\'u\~nez, J.& Barcelona& Towards an inertial reference frame              
through observations of minor planets\\                                         
177& Oblak, E. & Besan\c{c}on& Etoiles doubles \`a \'eclipse\\                  
178& Oblak, E.& Besan\c{c}on& Etoiles doubles visuelles\\                       
135& Oja, T.& Uppsala& kinematics at the north galactic pole\\                  
95& Olsen, E.H.& Copenhagen& HD stars (A5 to G0) brighter than                  
$m=8.3$ mag\TINOTE{2}\\                                                         
96& Olsen, E.H.& Copenhagen& HD stars (G5) brighter than $m=8.6$                
mag\TINOTE{2}\\                                                                 
115& Or\'us, J.J. de& Barcelona& Study of the local stellar                     
velocity distribution\\                                                         
183& Pagel, B.E.J.& Herstmonceux& Astrometry of nearby stars of                 
halo population\\                                                               
9& Pasinetti, L.E.& Milan& Solar standards:  the search for                     
groups of solar spectral analogues\\                                            
2& Paturel, G.& Lyon& The extragalactic distance scale from                     
Cepheids\\                                                                      
211& Pedoussaut, A.& Toulouse& Contribution \`a l'\'etude des                   
\'etoiles binaires spectroscopiques\\                                           
123& Penston, M.V.& Cambridge& Distances of T associations\\                    
132& Perrin, M.N.& Paris& Precise trigonometric parallaxes of                   
non-evolved G- and K-type dwarfs and subdwarfs\\                                
84& Pettersen, B.R.& Oslo& The absolute luminosities of flare                   
stars and their variability\\                                                   
8& Popper, D.M.& Los Angeles, USA &                                             
Absolute fluxes from nearby eclipsing binaries\\                                
31& Popper, D.M.& Los Angeles,\,USA& Parallaxes of visual binaries              
with reliable orbits\\                                                          
106& Pottasch, S.R.& Groningen& Distances to planetary nebulae\\                
74& Praderie, F.& Meudon& Physical parameters for programme stars               
in the satellite project\\                                                      
213& Pr\'evot, L.& Marseille& Selection of stars in the Magellanic Clouds \\    
118& Reid, I.N.& Pasadena, USA& Astrometry of low-lumimosity stars \\           
102& Rossell\'{o}, G.& Barcelona& Analysis of 7296 lunar occultations           
observed by photoelectric methods\\                                             
124& Ruben, G.& Potsdam& Establishment of a reference system with a             
Schmidt telescope\\                                                             
203& Ruben, G.& Potsdam& Link to the extragalactic reference frame in           
three fields of the northern hemisphere  \\                                     
40& Schmidt, M.& Pasadena, USA& Extragalactic reference frame based on          
bright quasars\TINOTE{2} \\                                                     
126& Schmidt-Kaler, T.& Bochum& Proper motions of O-type runaway                
stars\\                                                                         
154& Schmidt-Kaler, T. & Bochum& Parallaxes and proper motions of               
solar-type stars (solar twins)\\                                                
155& Schmidt-Kaler, T.& Bochum& Be stars in open clusters\\                     
188& Schober, H.J.& Graz& Search for binary asteroids\\                         
11& Scholl, H.& Nice& Observations of minor planets for                         
determination of the dynamical reference system\\                               
12& Scholl, H.& Nice& Determination of the masses of                            
asteroids (20) Massalia and (44) Nysa\\                                         
121& Schutz, B.F.& Cardiff& Search for a solar companion\TINOTE{2}\\            
87& Schwan, H.& Heidelberg& Determination of improved proper                    
motions for the GC stars\\                                                      
151& Schwarzenberg,A.& Brighton& Critical mass-transfer rate for                
stable accretion disks in cataclysmic variables\\                               
94& Schwerdtfeger, M.& Heidelberg& Positions and motions of                     
pulsating variables\\                                                           
138& Shipman, H.L.& Delaware,\,USA& Distances and luminosities of               
highly-evolved stars\\                                                          
216& Smith, C.& Washington,\,USA& FK5 candidate stars\\                         
173& Snow, T.P.& Boulder,\,USA& The interstellar medium in three                
dimensions\\                                                                    
33& Soderblom, D.R.& Baltimore,\,USA& Luminosities of solar-type                
stars\\                                                                         
34& Soderblom, D.R.& Baltimore,\,USA& Positions of stars associated             
with nebulosity\\                                                               
45& S\"oderhjelm, S.& Lund& Minor planets for a dynamical                       
reference frame\\                                                               
142& Spite, F.& Meudon& Kinematics and age of population I stars with           
observed lithium abundances\\                                                   
144& Squeren,A.M. Le& Meudon& Study of                                          
intrinsic parameters of OH Mira stars\\                                         
49& Stenholm, B.& Lund& Proper motions of Wolf-Rayet stars\\                    
36& Sutton, E.C.& Berkeley,\,USA& Determination of the IR reference             
frame\\                                                                         
14& Szabados, L.&Budapest,Hung.& Calibration of the Cepheid                     
distance scale\\                                                                
145& Taylor, G.E.& Herstmonceux& Occultations of stars by planets               
and satellites\\                                                                
70& Th\'e, P.S.& Amsterdam& Location of pre-main sequence Herbig                
Ae/Be stars in the HR diagram\\                                                 
116& Th\'e, P.S.& Amsterdam& The absolute magnitude of M-type                   
giants of various spectral types\\                                              
187& Tobin, W.& Canterbury,                                                     
NZ& Kinematic study of high-latitude OB stars\\                                 
27& Trefzger, C.& Binningen& Parallaxes and absolute magnitudes of              
population II dwarf stars\\                                                     
58& Trimble, V.& Irvine,\,USA& Parallaxes and proper motions of                 
astrophysically-puzzling classes of stars\\                                     
176& Turon, C.& Meudon& Local mass density through the kinematical              
study of F-stars in the meridian plane\\                                        
180& Turon, C.& Meudon& Density and velocity distribution of M dwarfs\\         
181& Turon, C.& Meudon& Evolution of late dwarf stars\\                         
191& Upgren, A.& Van Vleck,\,USA& Dwarf K and M stars found spectro             
scopically without bias toward high velocity\\                                  
192& Upgren, A.& Van Vleck,\,USA& Space densities and location in t             
he HR diagram of common types of stars\\                                        
165& Vauclair, G.& Toulouse& Parallaxes of bright white dwarf stars\\           
109& Vegt, C. de& Hamburg& Selected radio stars for an                          
extragalactic reference link using the VLA\\                                    
110& Vegt, C. de & Hamburg& Transformation of the Hipparcos stellar frame to an 
extragalactic reference frame\\                                                 
111& Vegt, C. de& Hamburg& Investigations of systematic errors and              
improvement of ground-based catalogues\TINOTE{2}\\                              
112& Vegt, C. de& Hamburg& Proper motions and space velocities of               
open clusters in the northern hemisphere\TINOTE{2}\\                            
218& Vegt, C. de& Hamburg& Optical\,\&\,radio positions of radio *              
for a link to the extragalactic reference frame\\                               
174& Viotti, R.& Frascati& Observations of hot subdwarf stars\\                 
175& Viotti, R. & Frascati& Observations of VV Cephei and                       
symbiotic stars\\                                                               
67& Vogt, N.& Santiago, Chile& Astrometry of cataclysmic variables\\            
20& Walter, H.G.& Heidelberg& Astrometric parameters of selected                
radio stars\\                                                                   
26& Walter, H.G.& Heidelberg& Positions and proper motions of                   
stars in the fields of extragalactic radio sources\TINOTE{2}\\                  
1& Weiss, W.& Vienna& Parallaxes of Ap and Am stars in the field                
and in clusters\\                                                               
134& Westerlund, B.E.& Uppsala& The $\zeta$                                     
Sculptoris cluster: its members, distance, space motion and evolution           
\PRFTABLE                                                                       
\vfill\eject                                                                    
\PROTABLE                                                                       
121& White, G.& Epping, Australia& Radio stars\TINOTE{1}\\                      
202& White, N.E.& Noordwijk& Properties of X-ray sources                        
discovered by Einstein, Exosat and Rosat\TINOTE{2}\\                            
16& Wielen, R.& Heidelberg& Proper motions of open star clusters\\              
17& Wielen, R.& Heidelberg& Parallaxes of LHS stars\\                           
18& Wielen, R. & Heidelberg& Proper motions of pulsating variable               
stars\\                                                                         
136& Wing, R.F.& Columbus,\,USA& Absolute magnitudes of                         
Mira variables and carbon stars\\                                               
4& Xu Tong-Qi& Shanghai, China& Rotation of the Earth since 1957\\              
5& Xu Tong-Qi& Shanghai, China& Comparison between the optical and              
radio positions of radio stars\\                                                
53& Yasuda, H.& Tokyo, Japan& Confirmation of a fundamental system              
in the fainter magnitude ranges\\                                               
46& Yoshii, Y.& Tokyo, Japan& Kinematics of extremely                           
metal-deficient red giants\\                                                    
51& Zappal\`a, V.& Torino& Physical observations of asteroids\\                 
141& Zeeuw, P.T. de& Princeton,\,USA& Structure and evolution of OB             
associations                                                                    
\PRFTABLE                                                                       
                                                                                
\begin{flushleft}                                                               
\TINOTE{1} Original proposal withdrawn and replaced by this proposal\\          
\TINOTE{2} Proposal deleted (no data)                                           
\end{flushleft}                                                                 
                                                                                
\vfill\eject                                                                    
                                                                                
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\CENTER{\LARGE\bf Acknowledgements}                                             
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
                                                                                
\small                                                                          
                                                                                
The work of the participants of the INCA Consortium is                          
supported and funded by national agencies through their respective              
institutes. The lists of funding authorities and main participating             
institutes are given, for each country, at the beginning of this                
volume.                                                                         
                                                                                
\medskip                                                                        
The work performed in Australia, dealing with radio stars and                   
the Hipparcos/Hubble Space Telescope link, is supported by the                  
Australia Telescope National Facility of CSIRO. G.L. White was                  
supported in part by an Australian National Research Fellowship. The            
use of ~`Starlink', and of the other facilities at the Anglo-Australian         
Observatory, are acknowledged.                                                  
                                                                                
\medskip                                                                        
The work performed in Belgium deals mainly with double and                      
multiple star systems. J. Dommanget is particularly indebted for                
financial support to the Fonds de la Recherche Fondamentale Collective          
(Bruxelles) under convention 2.9009.79 for the period 1979-87, and the          
Fonds National de la Recherche Scientifique, Cr\'edits aux Chercheurs,          
under conventions No.~1.5.388.88F for the period 1988-90 and                    
1.5.179.91F for the period 1991-93. The Commission des Communaut\'es            
Europ\'eennes provided a grant (No.~SC1-0057) for the period 1989-90.           
                                                                                
\medskip                                                                        
The work performed in Denmark, dealing with new astrometric and                 
photometric observations, and the participation in the operation of the         
Carlsberg Automatic Meridian Circle, is supported by the Danish Space           
Board, the Danish Natural Science Research Council and the Carlsberg            
Foundation.                                                                     
                                                                                
\medskip                                                                        
The work performed in France (mainly new astrometric                            
observations and measurements, work on variable stars and minor planets         
and satellites, mission simulations, production of the successive               
versions of the Input Catalogue, and coordination of the Consortium) is         
supported by the Centre National d'Etudes Spatiales (CNES), the Centre          
National de la Recherche Scientifique (CNRS), the Institut National des         
Sciences de l'Univers (INSU), and, through the support of each                  
participating Observatory and of the Bureau des Longitudes, the                 
Minist\`ere de l'Education Nationale (MEN). The Minist\`ere de                  
l'Education Nationale is also acknowledged for special support for              
observations with the automatic meridian circle at the Bordeaux                 
Observatory. The SIMBAD project is supported by INSU. The Centre                
National d'Etudes Spatiales is also acknowledged for grants for                 
operating the two data bases: SIMBAD, and INCA. The host of the two             
data bases was the Computer Centre of Paris-Sud University (Paris-Sud           
Informatique) from 1985 to 1990, and its director, J.B. Johannin, is            
especially acknowledged for his constant support. Acknowledgements are          
also due to the Minist\`ere de l'Education Nationale, de la Jeunesse et         
des Sports, the Minist\`ere de la Recherche et de la Technologie, and           
the Minist\`ere des Affaires Etrang\`eres, for their support through a          
European research network.                                                      
                                                                                
\medskip                                                                        
The work performed in Germany deals mainly with astrometric                     
compilation and analysis, measurement of cluster stars and double star          
positions and the preparations for the linking of the Hipparcos                 
reference frame to the radio/extragalactic frame. The work of the               
Astronomisches Rechen-Institut Heidelberg is mainly financed by the             
Ministerium f\"ur Wissenschaft und Kunst (MWK), Stuttgart, of the Land          
Baden-W\"urttemberg (Kapitel 1497). Additional support is provided by           
the Bundesministerium f\"ur Forschung und Technologie (BMFT), Bonn, of          
the Federal Republic of Germany, through the Deutsche Forschungs- und           
Versuchsanstalt f\"ur Luft-und Raumfahrt (DFVLR), K\"oln, under Project         
No. 01000421 (Project Leader: R. Wielen). The work at Hamburg                   
Observatory is financed by BMFT under Project No. 100013-8 (Project             
Leader: Ch. de Vegt). The work at the University of Bonn is financed            
by BMFT under Project No. 0100023-6 (Project Leader: P.~Brosche).               
                                                                                
\medskip                                                                        
The work performed in The Netherlands at Sterrewacht Leiden,                    
dealing with new astrometric measurements and photometric observations,         
is supported by Leiden University, in turn supported by the Ministerie          
voor Onderwijs en Wetenschappen.                                                
                                                                                
\medskip                                                                        
The work performed in Spain by the Real Instituto y                             
Observatorio de la Armada and by the Universitat de Barcelona, dealing          
with new astrometric and photometric observations, variable stars and           
minor planets, and the participation in the operation of the Carlsberg          
Automatic Meridian Circle, is funded by the Comisi\'on Interministerial         
de Ciencia y Tecnolog\'{\i}a (CICYT), Direcci\'on General de                    
Investigaci\'on Cient\'{\i}fica y T\'ecnica (DGICYT) and Estado Mayor de        
la Armada. For the period 1981-85, financial support was provided by            
the Comisi\'on Nacional de Investigaci\'on del Espacio (CONIE). The             
Comissi\'o Interdepartamental de Recerca i Innovaci\'o Tecnol\`ogica            
(CIRIT) is also acknowledged.                                                   
                                                                                
\medskip                                                                        
The work performed in Switzerland, dealing with new photometric                 
observations, photometric data compilation, and mission simulations, is         
financed by the Universit\'es de Gen\`eve and Lausanne, and the Fonds           
National Suisse de la Recherche Scientifique.                                   
                                                                                
\medskip                                                                        
The work performed in the United Kingdom, dealing with new                      
astrometric measurements and observations, the linking of the Hipparcos         
reference frame to the radio/extragalactic reference frame and double           
star observations, the participation in the operation of the Carlsberg          
Automatic Meridian Circle, and travel funds, is supported and funded by         
the United Kingdom Science and Engineering Research Council (SERC).             
The support of the Royal Greenwich Observatory for the measurements of          
positions of faint stars in the Cape Zone, and of Cambridge University          
for the work on double stars and the reference frame link, is also              
acknowledged.                                                                   
                                                                                
\medskip                                                                        
The work performed in the United States of America by the                       
Hubble Space Telescope Astrometry Team in preparation of the link of            
the Hipparcos reference frame to the radio/extragalactic reference              
frame, through the use of the Hubble Space Telescope Fine Guidance              
Sensors, is supported by the Astronomy Department of the University of          
Texas and NASA (NASA contract NAS 8-32906 and NASA grant NAGW-233).             
                                                                                
\medskip                                                                        
The work performed by the world-wide network of observers and                   
the American Association of Variable Star Observers (AAVSO), under the          
direction of Dr J.A. Mattei, before and during the Hipparcos mission,           
and the support of this work by NASA (NASA grant NAGW-1493), is                 
acknowledged.                                                                   
                                                                                
\bigskip\bigskip                                                                
Acknowledgements are particularly due to the staff of the                       
Centre de Donn\'ees Astronomiques de Strasbourg, Observatoire de                
Strasbourg, for their constant and efficient help in the creation and           
operation of the INCA Data Base, stemming from the SIMBAD Data Base and         
mainly operated using its basic software.                                       
                                                                                
\medskip                                                                        
The support of the Centre National d'Etudes Spatiales (CNES) in                 
mission simulations, through the assistance of personnel and the use of         
the Toulouse computer, the host of the complete simulation chain, is            
gratefully acknowledged.                                                        
                                                                                
\medskip                                                                        
The Guide Star Catalog Team of the Space Telescope Science                      
Institute (STScI), Baltimore, and particularly B. McLean, is gratefully         
acknowledged for the efficiency with which they answered requests about         
certain stars left without measurements at the end of the INCA                  
Consortium's ground-based observing programmes.                                 
                                                                                
\medskip                                                                        
The Royal Greenwich Observatory and the Hamburg Observatory are                 
acknowledged for the use of the CPC2 Catalogue prior to publication, as         
a joint contribution from these observatories.                                  
                                                                                
\medskip                                                                        
Many observers, in various observatories, undertook extensive                   
measurement programmes related to the Hipparcos Input Catalogue                 
preparation (astrometric observations and measurements, photoelectric           
observations, special observations of double and multiple systems).             
The work performed and the support they received from their respective          
institutions is gratefully acknowledged. The support of the management          
and staff of the European Southern Observatory (ESO), of the Carlsberg          
Automatic Meridian Circle (operated jointly by the Copenhagen                   
University Observatory, the Royal Greenwich Observatory and the Real            
Instituto y Observatorio de la Armada en San Fernando) and of the               
Bordeaux automatic meridian circle, is especially acknowledged.                 
                                                                                
\medskip                                                                        
For the work on variable stars, and especially large-amplitude                  
variable stars requiring the use of ephem\-erides for their efficient           
observation by Hipparcos, acknowledgements are due to the AAVSO and             
AFOEV staff and observers, to O.~Gascuel and J. Quinqueton of CRIM              
(Centre de Recherches en Informatique de Montpellier), to E. Diday of           
INRIA (Institut National de Recherche en Informatique et Automatique),          
and especially to A. Sch\"utz, P.E. Davies and A.J.C.~McDonald of ESOC          
(European Space Operations Centre).                                             
                                                                                
\medskip                                                                        
Numerous individuals participated in the preparation of the                     
link of the Hipparcos reference frame to an extragalactic reference             
system. Full acknowledgements to the participating institutes have been         
given in ESA-SP 1111, Vol. II.                                                  
                                                                                
\medskip                                                                        
For the preparatory work on minor planets and satellites, and                   
also for the eph\-eme\-rides of major planets, the Bureau des Longitudes        
(Paris) is particularly acknowledged.                                           
                                                                                
\bigskip\bigskip                                                                
The INCA Consortium acknowledges the careful work of reviewing                  
the astronomical proposals submitted to ESA by the Scientific Selection         
Committee and especially to the Committee's Chairman, Professor                 
A.~Blaauw, for his enthusiastic involvement in the work of the                  
Consortium.                                                                     
                                                                                
\medskip                                                                        
The staff of the ESTEC Hipparcos Project Team (under Project                    
Managers L. Emiliani and H. Hassan), in particular M.~Schuyer, R.D.             
Wills, S. Vaghi and R. Bonnefoy, are thanked for the many helpful               
exchanges throughout the preparation of the Hipparcos Input Catalogue.          
The staff of the ESA Operations Centre (ESOC), and in particular                
A.~Sch\"utz, were responsible for the implementation of the Hipparcos           
Input Catalogue, and their work under the Ground Segment Manager, J.            
van der Ha, and the Spacecraft Operations Manager, D. Heger, was an             
important contribution to the proper functioning of the Hipparcos Input         
Catalogue after the satellite launch.                                           
                                                                                
\medskip                                                                        
The INCA Steering Committee, on behalf of the entire INCA                       
Consortium, would like to use this opportunity to give recognition to           
the impetus given to the Hipparcos project in its early phases by the           
late Professor W. Fricke, and to the effective support he brought to            
the work of preparation of the Input Catalogue.                                 
                                                                                
\medskip                                                                        
The INCA Team Leader wants to highlight her deep appreciation                   
for the dedication shown by the Hipparcos Project Scientist in ESA, Dr          
M.A.C. Perryman, and in particular for his unremitting and stimulating          
interest in all parts of the work performed in the INCA Consortium and          
of all its connections with other parts of the Hipparcos work.                  
                                                                                
\end{document}                                                                  
                                                                                
                                                                                
