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               %   CARLSBERG MERIDIAN CATALOGUES 1-11   %
               %        May 1984 - May 1998             %
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\def\MN{{\rm MNRAS }}       
\def\ApJSup{{\rm ApJS }}    
\def\AApSup{{\rm A\&AS }} 
\def\PhD{{\rm PhD thesis}} 
%
\def\ome{(O$-$E)}     
\def\eg{{\it e.g.}}   
\def\ie{{\it i.e.}}   
\def\cf{{\it cf.}}    
\def\etal{{\it et\,al.}}
%
\def\mv{$m_{\rm v}$}              
\def\mpg{m\lower0.8ex\hbox{pg}}   
\def\Vmax{V\lower0.8ex\hbox{max}} 
\def\Vc{V\lower0.8ex\hbox{c}}     
\def\logg{log$\,${\sans g}}       
\def\as{$\,^{\prime\prime}\,$}              % arc seconds symbol        
\def\ass{\,^{\prime\prime}\,}
\def\pas{${}^{\prime\prime}\mskip-9mu.\,$}  % arc seconds over a period 
\def\pass{{}^{\prime\prime}\mskip-9mu.\,}                               
\def\pam{${}^{\prime}\mskip-1mu.\,$}        % arc min over decimal point
\def\pdeg{${}^{\circ}\mskip-9mu.\,$}        % degrees over a period     
\def\ph{${}^{\rm h}\mskip-9mu.\,$}          % hour over decimal point   
\def\ps{${}^{\rm s}\mskip-7mu.\,$}          %  s over decimal point     
\def\pmag{${}^{\rm m}\mskip-9mu.\,$}        % m over decimal point      
\def\pmags{{}^{\rm m}\mskip-9mu.\,}                                     
\def\mag{\ifmmode^{\rm m }\else$^{\rm m}$\fi} % m space                 
%                                                                       
\def\simlt{\lower.5ex\hbox{$\; \buildrel < \over \sim \;$}}             
\def\simgt{\lower.5ex\hbox{$\; \buildrel > \over \sim \;$}}             
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\def\ss{\ifmmode^{\rm s}\else$^{\rm s}$\fi}                             
\def\deg{\ifmmode^\circ\else$^\circ $\fi}                               
\def\amin{\ifmmode^\prime\else$^\prime $\fi}  % arc min                 
%Right Ascension                                                        
\def\ra#1#2#3{#1\hh\ #2\mm\ #3\ss\ }                                    
%Declination                                                            
\def\dec#1#2#3{\ifmmode{#1}\else{$#1$}\fi\deg\ #2\amin\ #3\as\ }        
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\def\leseq{\>{\raise-.5ex\hbox{$<$} \atop \raise.1ex\hbox{$=$}}\>}      
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\documentstyle[11pt,twoside]{cmc11}                                      
\renewcommand{\catnumber}{1-11}                                            
\renewcommand{\catperiod}{May 1984 to May 1998}
\renewcommand{\catyear}{1999}                              
\begin{document}                                           
\cattitle                                                  
\firstpage                                                 
\tableofcontents                                           
\listoftables
%\listoffigures                                             
%                                                          
\summary{                                                  
This composite catalogue contains 180\,812 positions and magnitudes of 
176\,591 stars north of declination --40\deg, 155\,005 proper motions, and 
21\,944 positions and magnitudes of 184 Solar System objects obtained
with the Carlsberg Automatic Meridian Circle on La Palma during the period     
May 1984 to May 1998. It includes Carlsberg Meridian Catalogues Numbers 1 to
11 (CMC1-11); i.e. it comprises all the observations made with the 
scanning--slit micrometer since the beginning of operation on La Palma.
The positions of the stars are for the epoch of observation and the equinox    
J2000.0, and are referred to the new International Celestial Reference Frame.
The limiting  magnitude is \mv = 15\pmag4.
                                                                               
The catalogue mainly comprises observations and proper motions for the 
following programmes: 

\begin{tabular}{rl}
36\,000 & International Reference Stars \\
30\,000 & faint reference stars in a global net \\
18\,000 & reference stars in the fields of radio sources \\
17\,000 & stars in the Lick Northern Proper Motion catalogue \\
 5\,000 & reference stars for calibration of Schmidt plates \\
 2\,600 & stars in the Gliese catalogue of nearby stars \\
 5\,000 & stars in nearby OB associations \\
10\,500 & F-type stars within 100 pc \\
 9\,000 & G-type d\&g, K-type g stars within 300 pc \\
 2\,200 & Unbiased sample of K/M-type d stars \\
 19\,400 & Reference stars around Veron--Cetty galaxies \\
 4\,700 & GCVS stars, mainly 12$<$mag$<$14 \\
 7\,300 & NLTT stars, mainly 12$<$mag$<$14 \\
\end{tabular}

\noindent
and several smaller programmes, each having fewer than 2000 stars, which are
mainly aimed at galactic kinematics. Positions  and magnitudes of 12 nov\ae~ 
and 8 supernov\ae~which occurred in the years 1991 to 1998 are included.
The catalogue also contains observations of the following Solar System objects:
Callisto, Ganymede, Rhea, Titan, Iapetus, Hyperion, Uranus, Oberon, Neptune,   
Pluto, 173 minor planets, and comet P/Wild 2.                                                    
                                                                               
The mean error of a catalogue position in the zenith is 0\pas09 in right 
ascension and declination in CMC4-5-6, improving to 0\pas06 in CMC7-11. The 
accuracy in magnitude is 0\pmag05 in CMC4-10, improving to 0\pmag03 in CMC11.
The mean error of the proper motions, derived by combining the position in 
this catalogue with those at earlier epochs, is typically in the range 
0\pas003 to 0\pas004 per year.       
                                                                               
Cross-references are given to DM, AGK, SAO, HD and the Washington Double Star
(WDS) catalogues.  

The catalogue also contains 12\,216 mean annual observed positions of the FK5
stars used initially in CMC4-9 to transfer the instrumental system to the 
FK5 frame.

A compilation of all the meteorological data and nightly atmospheric
extinction for the years 1984-1998 is appended.
}{                                                                             
Este cat\'alogo m{\'u}ltiple contiene 180\,812 posiciones y  168\,989 
magnitudes de 176\,591 estrellas al norte de --40\deg, 155\,005 
movimientos propios y 21\,944 posiciones y magnitudes de 184 objetos 
del sistema solar, obtenidas con el C{\'i}rculo Meridiano Autom\'atico 
Carlsberg, en La Palma, desde Mayo de 1984 hasta Mayo de 1998. 
Incluye los Cat{\'a}logos Meridiano Carlsberg N\'umeros 1 a 11 (CMC1-11); es 
decir todas las observaciones hechas con el micr{\'o}metro de rendijas 
m{\'o}viles desde el principio de las operaciones en La Palma.
Las posiciones se publican para la \'epoca de observaci\'on, referidas 
al equinoccio J2000.0 y en el nuevo Sistema International de Referencia 
Celeste. La magnitud l\'{\i}mite es \mv=15\pmag4.

El cat\'alogo consta principalmente de observaciones de los siguientes 
programas: 

\begin{tabular}{rl}
36\,000 & estrellas de referencia internacional (IRS)\\
30\,000 & estrellas d\'ebiles de referencia en una red global\\
18\,000 & estrellas de referencia en campos de radio fuentes\\
17\,000 & estrellas del cat\'alogo Lick Northern Proper Motion \\
5\,000 & estrellas de referencia para calibraci\'{o}n de placas Schmidt\\
2\,600 & estrellas cercanas del cat\'alogo de Gliese \\
5\,000 & estrellas cercanas en  asociaciones O-B\\
10\,500 & estrellas F dentro de un radio de 100 pc\\
9\,000 & estrellas G y K dentro de un radio de 300 pc\\
2\,200 & estrellas de una muestra aleatoria de enanas K y M\\
19\,400 & estrellas de referencia en campos de galaxias en Veron-Cetty\\
4\,700 & estrellas de GCVS, principalmente en 12$<$mag$<$14\\
7\,300 & estrellas de NLTT, principalmente en 12$<$mag$<$14\\
\end{tabular}

\noindent y otros programas de menos de 2\,000 estrellas 
para estudiar la cinem\'atica gal\'actica. Contiene adem\'as posiciones y 
magnitudes de 12 novas y 8 supernovas aparecidas entre los a\~nos 1991 y 
1998. El cat\'alogo incluye observaciones de los objetos del sistema solar: 
Gan\'{\i}medes, Calixto, Rea, Tit\'an, Hiperi\'on, Japeto, Urano, Ober\'on, 
Neptuno, Plut\'on, 173 asteroides, y cometa P/Wild 2.

El error medio de una posici\'on del cat\'alogo en el cenit es 0\pas09 en      
ascensi\'on recta y declinaci\'on en los CMC4-5-6 y 0\pas06  
en los CMC7-11. En magnitud es de 0\pmag05 en los CMC4-10, y 0\pmag03 en
lo CMC11. El error medio de los movimientos 
propios, obtenidos combinando las posiciones de este cat\'alogo con los de 
\'epocas anteriores, es t\'{\i}picamente 0\pas003 a 0\pas004 por a\~no.
                                                                                
Se dan las referencias cruzadas con los cat\'alogos DM, AGK, SAO, HD y 
con los estrellas dobles WDS.

Tambi\'en se incluyen las posiciones medias anuales observadas de 12\,216 
estrellas del FK5 usadas para referir en primer lugar el sistema instrumental 
en los cat\'alogos CMC4-9 al sistema de referencia definido por el FK5.

Finalmente se a\~nade una recompilaci\'on de 
todos los datos meteorol\'ogicos y del extinci\'on atm\'osfera recogidos 
desde 1984 hasta 1998.}

\section{Introduction}\label{intro}                                            
This catalogue is the compilation of Carlsberg Meridian Catalogues Numbers 1
to 11 (CMC1-11), in the series observed with the 18 cm  
Carlsberg Automatic Meridian Circle on La Palma.  It comprises all
the observations made between May 1984 and May 1998 with the scanning--slit
micrometer. Catalogues CMC1-8 were issued separately in five printed volumes 
(CMC1-4 1989; CMC5 1991; CMC6 1992; CMC7 1993; CMC8 1994).  Catalogue CMC9
was issued on a CD-ROM in 1997. The space afforded by this CD-ROM was used
to re-issue CMC1-8 and combine them with CMC9. Similarly, CMC11 is now issued
on CD-ROM together with CMC1-10.  Although CMC10 was not published
separately -- being overtaken by CMC11 -- its separate identity has been 
maintained in the numbering sequence because the treatment of the observations
was slightly different from CMC11. The periods covered by these catalogues are 
set out in \S\ref{formation} Table~\ref{periods}. 
                                                                               
The operation of the instrument on La Palma was shared between Copenhagen     
University Observatory (CUO), the Royal Greenwich Observatory (RGO)  
Cambridge and the Real Instituto y Observatorio de la Armada en San Fernando   
(ROA).  The Copenhagen University Observatory is a department of The Niels     
Bohr Institute for Astronomy, Physics and Geophysics.                          
The three institutions set up a Management Committee to decide on the overall  
observing programme and other matters related to running the telescope.  In    
general, an individual  programme of stars took several years to complete 
and the results are published in a number of catalogues in the current     
series.                                                                        
                                                                               
The geodetic coordinates of the telescope on the WGS84 system were determined  
in 1993 using a GPS receiver.                                                  
The astronomical and geodetic coordinates are:                                 
                                                                               
\bigskip                                                                       
\[                                                                             
\mbox{Astronomical }\left\{                                                    
                    \begin{array}{l}                                           
                    17\deg \, 53\amin \, 07\pass8 \,\rm W\\[1.5ex]             
                    28\deg \, 45\amin \, 52\pass4 \,\rm N                      
                    \end{array}                                                
                    \right.                                                    
\qquad                                                                         
\mbox{Geodetic }\left\{                                                        
                    \begin{array}{l}                                           
                    17\deg \, 52\amin \, 56\pass70 \,\rm W\\[1.5ex]            
                    28\deg \, 45\amin \, 35\pass97 \,\rm N\\[1.5ex]            
                    {\rm Altitude}\,\,\, 2326\,{\rm m}                         
                    \end{array}                                                
                    \right.                                                    
\]                                                                             
                                                                               
\bigskip
All the observations in CMC1-11 were made with a photoelectric moving-slit
micrometer.  The original micrometer used in CMC1-4 was replaced by a new
micrometer in May 1988 and this was used for CMC5-11. A description of the
micrometer in use during CMC1-4 is given in Helmer \& Morrison (1985). The
refinements introduced with the new micrometer included reducing the length
of the slits with a diaphragm, thereby reducing the background noise, and
halving the scanning distance which allowed twice as many scans over an
object in the same time. The micrometer was also improved by fitting a
linear encoder.


Programme stars south of               
declination --20\deg \space were not observed in the small section of the slits
due to the somewhat poorer seeing at low altitudes.                            

These refinements led to an improvement of the accuracy (0\pas19 to 0\pas15)
for a single observation at the zenith. A further improvement to 0\pas12 was
achieved by smoothing observations from night to night (see 
Table~\ref{errorz}). 

Besides this development of the moving-slit micrometer, the following 
improvements were made to the system:
\begin{list}{}{}
 \item{August 1985:} An air circulation system was installed in the telescope 
  tube to remove internal refraction (H{\o}g \& Fabricius 1988).
 \item{January 1986:} An azimuth mark 130\,m to the south was observed hourly
  and the change in azimuth deduced from this mark was subtracted from the
  observations thereafter.
 \item{December 1986:} Another azimuth mark was introduced 50\,m to the north.
 \item{May 1988:} The new micrometer was introduced with a wider pass band 
  which is nearly rectangular between 4885 and 6160\,\AA. The previous
  micrometer had a pass band close to Johnson~V.
 \item{February 1989:} A new collimator alignment micrometer was brought into use,
  making possible determinations of the collimation-free reading
  and horizontal flexure (see Helmer\,\etal\,1991). Both the collimation and
  flexure were found to change smoothly during the night and the use of
  the alignment micrometer was discontinued after November 1994.
 \item{October 1991:} The divided circle was replaced by a new glass circle 
  manufactured by Heidenhain with {\it Diadur} division lines which gave 
  improved definition.
  The mean error for the reading of one diameter, as determined from the
  measurement of the diameter corrections, reduced from $\pm$0\pas05 to 
  $\pm$0\pas03.
 \item{August 1992:} The photoelectric circle-reading micrometers were replaced
  by CCD cameras. A quick circle reading made 2 seconds before the observation 
  starts enables the setting of the telescope to be given a final 
  adjustment, resulting in a setting error of less than 0\pas3. This permitted
  the use of the smallest part of the scanning slits, thereby increasing the 
  efficiency of the micrometer.
 \item{April 1995:} A new electronic control system for the telescope and
  micrometer was installed. New bearings were fitted to the diaphragm in the
  micrometer.
 \item{December 1996:} The clock system was replaced by a GPS receiver.
 \item{April 1997:} Remote operation was introduced using the Internet.
\end{list}

A full description of the improved micrometer and its operation can be found 
in \\ Helmer\,\etal (1991). 

 The limiting magnitude of the telescope increased as a result of these 
improvements. This is shown in Table~\ref{limitmag}.
\begin{table}
\begin{center}
\caption{Limiting magnitude of Catalogues.}
\label{limitmag}
\begin{tabular}{lc}
\hline
Catalogue & Limiting mag. (V) \\
\hline
CMC1-4 & 13.0  \\
CMC5-6 & 14.8  \\
CMC7-11 & 15.4  \\
\hline
\end{tabular}
\end{center}
\end{table}

Neutral density filters were used to reduce the magnitudes of the brightest
stars. These are listed in Table~\ref{filters}.

\begin{table}
\begin{center}
\caption{Neutral density filters.}
\label{filters}
\begin{tabular}{llll}
\hline
Catalogue & \multicolumn{2}{c}{Filters} \\
          & Brighter than 6.0 & Brighter than 2.0 \\
\hline
CMC1-4    & -----             & 6-mag          \\
CMC5      & 4-mag             & not observed   \\
CMC6-11   & 4-mag             & 8-mag          \\
\hline
\end{tabular}
\end{center}
\end{table}

The position of the clamp of the telescope is displayed in Table~\ref{clamp}.

\begin{table}
\begin{center}
\caption{Telescope clamp.}
\label{clamp}
\begin{tabular}{ccc}
\hline
Clamp  & \multicolumn{2}{c}{Dates} \\
       &  From         &    To  \\
\hline
West  & 1~May~1984     & 8~June~1987     \\
East  & 9~June~1987    & 21~February~1988 \\
West  & 16~May~1988    & 4~November~1990 \\
East  & 5~November~1990& 2~October~1991 \\
West  & 3~October~1991 & 27~May~1998 \\
\hline
\end{tabular}
\end{center}
\end{table}

                                                                 
\newpage                                                                 
The observation programme comprised five categories of objects: 
\begin{enumerate}                                                
 \item Stars belonging to stellar reference frame programmes, such as the FK5, 
       IRS and special reference stars around QSOs etc.;             
 \item Stars being re-observed primarily to improve the accuracy of their 
       proper motions which are required for stellar kinematics;
 \item Variable and high proper motion stars with poor positions;
 \item Bodies in the Solar System, comprising the outer planets, some of their 
       satellites, and minor planets whose positions are required for improving 
       their orbits.                                                         
 \item Calibration sources for determining the zenith point correction, level,
       azimuth, collimation and flexure. 
       
\end{enumerate}                                                                
                                                                               
The strategy of the observing programme was                                    
such that these programmes could be carried out simultaneously, with           
their rates of completion being determined by pre-assigned priorities allotted 
by the Management Committee.  Details of the observing programme are given in  
\S\,\ref{number}.                                                               
                                                                               
In catalogues CMC1-9 the observations were initially reduced differentially 
with respect to the FK5 and later adjusted to the new International Celestial
Reference Frame (ICRF) using observations of stars common to the 
Hipparcos Catalogue (ESA, 1997).
CMC10-11 were observed differentially with respect to the Hipparcos Catalogue
which became available in a pre-release form in 1996.
The method was not completely differential because the nightly 
fitting to the reference catalogue involved only zero-point corrections in     
right ascension and declination, orientation of the telescope axis and         
a correction to the coefficient of refraction. Variations with time of the
pointing angles of the telescope were removed from the observations by         
measuring these angles at regular intervals throughout the night using         
the calibration light sources within and near the dome. 

Beginning with CMC7, zonal adjustments, consisting of a simple displacement of 
the segment of sky containing each star, were also applied in order to smooth 
out night-to-night variations introduced by unknown changes in the instrumental 
system and anomalous refraction. These adjustments gave a 10--20\% reduction 
in the internal mean error. Details of this procedure are given in 
\S\,\ref{zonal}.  Further improvements in accuracy in CMC10-11 were achieved
by observing differentially with respect to the Hipparcos Catalogue rather
than the FK5.
                                                                               
The positions on this CD-ROM for catalogues CMC1-11 supersede all previously 
printed and electronic versions which are available through the Centre de 
Donn\'ees Astronomiques de Strasbourg.  All the corrections in the errata lists
of those catalogues have been made in this CD-ROM compilation. A new match
of the catalogues with the Durchmusterung catalogues revealed many new pairings
which have been carried through to the CD-ROM. Besides these changes,
several hundred observations have been omitted here because they are astrometric 
doubles and this had been overlooked in the earlier compilations.
                                                                               
\section{Personnel}\label{personnel}
The telescope was operated by 27 different observers in the course of the
production of the catalogues CMC1-10. Beginning in May 1997 (during CMC11), 
the telescope was operated remotely by the three participating institutions 
in turn and no-one was present at the telescope. 
Table~\ref{observers} gives 
the main areas of effort for each observer. 

{\scriptsize
\begin{table}[t]                                                               
\caption{Observers and main areas of effort.}
\label{observers}
\tabcolsep3pt                                                                  
\begin{tabular}{l|c|c|c|c|c|c|c}  
\multicolumn{8}{c}{}\\
\hline
\bf Observer$^a$ & \bf Inst. &  \bf CMC &                             
\begin{tabular}{c}                                                             
\bf Observing\\                                                              
\bf and      \\                                                              
\bf differential \\                                                          
\bf reduction                                                                
\end{tabular}                                                                  
&                                                                              
\begin{tabular}{c}                                                             
\bf Formation\\                                                              
\bf of observing      \\                                                     
\bf list                                                                     
\end{tabular}                                                                  
&                                                                              
\begin{tabular}{c}                                                             
\bf Formation\\                                                              
\bf of     \\                                                                
\bf catalogue                                                                
\end{tabular}                                                                  
&                                                                              
\begin{tabular}{c}                                                             
\bf Software$/$\\                                                            
\bf hardware     \\                                                          
\bf development                                                              
\end{tabular}                                                                  
&                                                                              
\begin{tabular}{c}                                                             
\bf Daily     \\                                                             
\bf management                                                               
\end{tabular}\\                                                                
\hline                                                                         
\rule{0pt}{3.5ex}%                                                             
G~Ameyugo    & ROA & 4 & $\times$ &          &          &          &     \\
R~W~Argyle   & RGO &5-11& $\times$ & $\times$ &          & $\times$ &     \\ 
K~Augustesen & CUO &1-9& $\times$ &          &          &          &     \\
F~Beliz\'on  & ROA &8-11& $\times$ &          &          &          &     \\
M~E~Buontempo& RGO &1-11& $\times$ & $\times$ &          & $\times$ &\\[2.5ex]
F~Cano       & ROA &1-5& $\times$ & $\times$ &          &          &     \\
J~C~Coma     & ROA &2-5& $\times$ &          &          &          &     \\
O~H~Einicke  & CUO &1-11& $\times$ &          &          & $\times$ &     \\
P~Eldridge   & RGO &1-5& $\times$ & $\times$ &          &          &     \\
C~Enriqu\'ez & ROA &5-6& $\times$ &          &          &          &\\[2.5ex]
D~W~Evans    & RGO &5-11& $\times$ & $\times$ &          & $\times$ &     \\
C~Fabricius  & CUO &1-9& $\times$ &          & $\times$ & $\times$ &     \\
A~Fern\'andez& ROA & 5 & $\times$ &          &          &          &     \\
P~Gibbs      & RGO &1-5& $\times$ & $\times$ & $\times$ & $\times$ &     \\ 
F~Gutierrez  & ROA &3-4& $\times$ &          &          &          &\\[2.5ex]
H~Hansen     & CUO & 2 & $\times$ &          &          &          &     \\
L~Helmer     & CUO &1-11& $\times$ &          &          & $\times$ & $\times$\\
P~Herridge   & RGO &7-9& $\times$ &          &          & $\times$ &     \\
B~Jensen     & CUO &1-8& $\times$ &          &          &          &     \\
P~Jensen     & CUO &1-8& $\times$ &          &          &          &\\[2.5ex]
T~Knudsen    & CUO &1-11& $\times$ &          &          & $\times$ &     \\
L~V~Morrison & RGO &1-11& $\times$ &          & $\times$ & $\times$ & $\times$\\
J~L~Mui\~nos & ROA &1-11& $\times$ & $\times$ & $\times$ &          &     \\
R~H~D~Swifte & RGO & 1 & $\times$ &          &          & $\times$ &     \\
C~Thoburn    & RGO &1-4& $\times$ & $\times$ &          & $\times$ &\\[2.5ex]
M~Vallejo    & ROA &8-11& $\times$ &          &          &          &     \\ 
R~Villamil   & ROA &5-9& $\times$ &          &          &          &     \\
\hline                                                                     
\end{tabular}

$\null{^a}$ Until May 1997
\end{table} }
                                                                               
\section{Real-time selection and observation}\label{realtime}     
The selection of celestial and calibration objects was performed in real-time,  
according to a pre-assigned priority, from an input catalogue of more than 
300\,000 stars. Each star was normally observed on six different nights. 

The percentage of time spent on different categories of objects varied
slightly over the course of the observation of the eleven catalogues in this
compilation. The following are average values: 10\% on calibration objects,
73\% on programme stars, 15\% on FK5 or Hipparcos stars, except in CMC11 where
the percentage rose to $\sim$40\%, and 2\% on planets.  

The two observing slits were 4\as wide and 77\pas4 (1\,mm) long in the vertical 
direction, but only a section of one slit was uncovered at any one time during 
an observation. The possible section lengths were 12\pas4 (small), 23\pas6 
(medium) and 70\pas0 (long) vertically.  The small section was only available
from the time of the introduction of the new micrometer (May 1988). It was 
brought into regular use after the telescope setting had been refined in
August 1992.

When a star was observed for the first 
time the medium section was used, scanning some 14\as$\times$14\as of the 
sky. After August 1992, the subsequent observations were made using the more 
efficient small section where some 3\as$\times$3\as of the sky may be regarded
as fully scanned. Obviously this was only possible when the input position was 
known with some accuracy and the telescope could be set with great precision. 

If the input position of the star was poorly known, the longest section of the
slits was used for the first observation, provided it was not too faint to
obtain a reasonable signal-to-noise ratio. The availability of the HST
Guide Star Catalogue in 1992 greatly facilitated the identification and 
correction of the input positions of target stars.

The slit plate was driven at a constant velocity of 38\pas72\,s$^{-1}$ and
the integration time was fixed at 32\,ms. The velocity (${\nu}$) relative to 
the star in the forward scan was
$$ \nu = 38\pass72 - 15\ass\,{\rm cos}\,\delta\,{\rm cos}\,h, $$
and 
$$ \nu = 38\pass72 + 15\ass\,{\rm cos}\,\delta\,{\rm cos}\,h $$
in the reverse direction, where $h$ is the hour angle. The scanning
time was approximately 16\,s, 32\,s, 64\,s and 100\,s for stars brighter than 
9\pmag5(visual), stars from 9\pmag5 to 11\pmag0, stars from 11\pmag0 to 
14\pmag0 and stars fainter than 14\pmag0, respectively.
However, reference stars at zenith distances greater than 60\deg \space were 
observed for 32\,s, and those greater than 75\deg \space for 64\,s, 
irrespective of their magnitude.          
The actual time that the star spent in the slits (5\pas5 in the direction of
scan) depended on the scan length. For stars in the small section of the slits,
the time spent partially and completely in the slits was about half of the 
total scan times given above. For stars in the medium section, it was about a 
quarter, and for the long section, about an eighth.

Stars were observed up to 40\,s from the meridian. Due to the rather poor     
quality of the observations at large zenith distances, the selection of new   
programme stars south of declination --40\deg \space was restricted.          
                                                                              
After August 1992, the FK5 stars, and later, Hipparcos stars, were observed 
in the small slit section, 
except those at a zenith distance greater than 70\deg \space which were 
observed in the medium section. 
                                                                             
\section{Differential reduction to the FK5/ICRF}\label{difred}                               
                                                                             
  \subsection{Nightly reduction (general)}\label{nightly}                                            
The real-time reduction to micrometer coordinates of the photon counts for the 
stars was carried out as described in Helmer\,\etal\,(1991).
                                                                               
A preliminary, differential reduction to the FK5 system (CMC1-9) or to the
Hipparcos system (CMC10-11)                       
of the observations for each night was carried out the following day by the    
observer using interactive computer programs.  The differences between the     
calculated and observed apparent positions of the FK5/Hipparcos stars were 
used in a     
single least-squares adjustment for the whole night containing about           
eight to ten FK5 stars per hour, spread between zenith distances $\pm$84\deg.  
This increased to over 20 Hipparcos stars per hour in CMC10-11.
FK5/Hipparcos stars above +67\deg \space in declination were observed at 
either upper or lower culmination.
                                                                               
Magnitudes were derived by fitting the observations to about 50 photoelectric  
standards spread through the night. This increased to about 200 in CMC11.

The least-squares solutions in $\alpha, \delta$ and {\it m} were applied       
to the programme stars, and their mean places at J2000.0 were computed using   
the 1976 IAU system of astronomical constants, as described in the Supplement  
to the Astronomical Almanac 1984.  These preliminary mean places of the stars  
were compiled daily into a catalogue.  When the required number of mutually    
consistent observations was reached, the star was automatically omitted from   
the observing list.                                                            

   \subsection{Refraction}\label{refraction}
The astronomical refraction was taken from the Pulkovo Observatory Tables      
(4th edition). The temperature, pressure and humidity were read with each      
observation. The temperature used to enter the Pulkovo Tables was the average  
of three thermometers situated along the opening of the telescope enclosure.   
Table~\ref{deltaR} gives the differential                                      
correction to the Pulkovo refraction due the rectangular bandwidth 
(4885-6160\,\AA) of the detector system introduced with the new micrometer
in May 1988. These corrections were first applied in January 1990. The
previous detector system had a bandwidth close to Johnson~V and no correction
was applied to the Pulkovo Tables. 
\begin{table}[t]                                                               
\caption{Differential correction to the Pulkovo refraction.}
\label{deltaR}                                                                 
\begin{center}                                                                 
\begin{tabular}{c|c|l}                                                         
\multicolumn{3}{c}{}\\
\hline                                                                         
       \rule{0pt}{3ex}Type &  Coefft. of $$tan z$$ & \\[1.5ex]                 
\hline                                                                         
       \rule{0pt}{2.5ex}&    $\Delta R$ &\\                                    
                  O   &     +0\pas0860 &\\                                     
                  B   &     +0.0808  &\\                                       
                  A   &     +0.0741  &\\                                       
                  F   &     +0.0696  & --default value for stars\\             
                  G   &     +0.0649  & --used for all Solar System objects\\   
                  K   &     +0.0549  &\\                                       
                  M, R, N, S&  +0.0328  &\\ \hline                             
\end{tabular}                                                                  
\end{center}                                                                   
\end{table}                                                                    
                                                                               
This correction is particularly important for the reference stars which are observed 
at very large zenith distances. The correction was applied to all stars of     
known spectral type, beginning on 1 January 1990. Where the spectral type was 
unknown, the correction for type F was adopted. In these cases a correction to 
the declination may be added later when the spectral classification is known. 
A correction of         
\[                                                                             
\Delta \delta=(\Delta R-0\pass0696)\tan \,(\delta -                            
                                       28\deg\,45\amin\,52\pass4)              
\]                                                                             
should be {\bf added} to the declination.                                      
                                                                               
Before making the final differential solution used in this catalogue, several  
corrections were applied to the preliminary results obtained from the first 
solution. Small corrections were applied to right ascension and declination for
the differences from their assumed values of the scale and inclination of the 
micrometer which were determined regularly from observations of near-equatorial 
stars.                                         
                                                                               
No systematic differences were found in position or magnitude depending        
on whether a star was observed in the small or the medium section of           
the slits.                                                                     

  \subsection{Instrumental calibrations}\label{calib}
When available and reliable, the instrumental calibrations were interpolated   
to the time of observation and subtracted from the residuals of the reference
stars before the    
final least-squares adjustment was made. These calibrations consisted of the   
zenith point, level, collimation-free reading, horizontal flexure and north    
and south azimuth marks. They were measured at an interval of 0\ph5 during the 
first 1$1\over 2$ hours of the duty and at 1\ph5 thereafter.                   
The collimation and flexure, however, were only measured at 3\hh \space        
intervals because they were found to vary slowly.  The use of the collimators
to measure collimation and horizontal flexure was discontinued after 
29 November 1994. The collimation-free reading was then wholly determined from 
the least-squares adjustment to the reference stars. A constant value of 
$$  -0\pass50\,{\rm sin}\,z  $$
was adopted for the horizontal flexure in CMC6--CMC9, inclusive. Otherwise,
it was treated as an unknown. 
                                                                               
The stars were assigned the following weights in right ascension, declination  
and magnitude, depending on their zenith distances;                            
$\cos^{0.6} z,\ \cos^{0.9} z$ and $\cos z$, respectively. These are empirical 
relations derived from the scatter of the observations as a function of zenith 
distance.            
                                                                               
  \subsection{Nightly least--squares adjustment in RA, DEC}\label{adjust}
The solutions in right ascension comprised the Besselian constants {\it m}     
 and {\it n} as                                                                
unknowns, and often the collimation. The first and second derivatives with     
respect to time of the collimation, and the first derivatives of {\it m}       
 and {\it n} were used on about a third of the nights.                         
                                                                               
In declination the unknowns were always  constant corrections to the zenith 
point and refraction (separately, south and north). On roughly half of the 
nights the first and second derivatives with respect to time of the zenith 
point were also included.                                                      
                                                                               

   \subsection{Nightly least--squares adjustment in MAG}\label{mag}
In magnitude the unknowns were a constant ($D_o$) and colour term ($C_o$) in   
instrumental absorption, and a constant for extinction ($E_o$) at time         
$\theta _o$, and, when needed, its hourly rate of change ($E'$). For the time  
of observation, $\theta$, we have:                                             
\[                                                                             
m = m_{obs} + D_o + C_o (B-V) + [E_o + E' (\theta - \theta _o)]\sec z.         
\]                                                                             
The colour coefficient in instrumental sensitivity, $C_o$, was fixed at        
+0.036 in CMC5 and until 15 Feb 1990 in CMC6, and at +0.018 thereafter
(see \S\,\ref{juanV}).

With the increase in observation of Hipparcos reference stars in CMC11, it was
possible to carry out a solution with greater temporal resolution. Rather than
include only a fixed linear change in extinction for the night, the
median of 10 successive observations was used to describe the temporal
variation in extinction.  This improved the standard error of the magnitude
from 0.05 to 0.03 for stars of V$\sim$9 near the zenith.

When computing the magnitudes for this catalogue, the value +0.5 was assumed   
for $B-V$ for all programme stars; whereas, for the reference stars, 
the individual values of $B-V$ were used.  The magnitude results are 
discussed in \S\,\ref{juanV}.                                                   
                                                                               
    \subsection{Zonal adjustment (CMC7-11)}\label{zonal}                            
The behaviour of the telescope and the atmosphere normally do not obey the     
simple model assumed in the differential reduction described in
\S\,\ref{nightly}.
As a result, the final residuals on any particular night for the reference
stars often show variations with respect to time and zenith distance. 
These are partly due to zonal errors in the FK5 prior to CMC10. 
Starting with CMC7, efforts were made to reduce the contribution of these 
temporal and spatial variations in the observations.
                                                                               
In designing a solution to this problem, care was taken not to alter           
the system of the catalogues. The method adopted in the final adjustment of
CMC8-11 is a slightly improved version of that used in CMC7.  It can be 
summarized as follows.                                        
                                                                               
Due to the method of reduction, programme stars were affected by the same 
regional distortions as reference stars. 
They formed a much denser net than the reference stars,
so their residuals could be used to obtain a better estimate of the regional
distortions. On any particular night, the residuals of the programme stars     
in the same segment or zone of the sky, will exhibit the same bias due to the  
imperfections of the simple model described in \S\,\ref{nightly}. The residual for 
each  star on a particular night is the difference between its position on  
that night and the mean of all its other observations which will normally      
be five in number, spread over  about two weeks. Most stars on any particular 
night will have nearly contemporaneous observations because as a  star is 
observed its priority is increased progressively until it has been completed. 
Provided that the regional distortions are more or less random from night-to-night, 
the mean position for each star will tend to average these out, and the 
residual from the mean on any particular night will reflect the regional 
distortion on that night. Distortions persisting over a week or more, 
originating from long-term deficiencies in the simple model, will be 
underestimated when only using programme stars. 

As the same FK5 stars were observed over several months, they tended to show the
long-term deficiencies as well as the night-to-night variations. Therefore, 
in CMC8 and CMC9, the residuals of the FK5 stars with respect to their mean 
positions were also included when calculating the regional distortions.
In CMC10 and CMC11 many different Hipparcos stars were observed as reference
stars and in general no particular star was observed repeatedly. So, the
observations of Hipparcos stars could not be used in this manner.
It must be emphasized that the FK5 positions themselves were
not used in this process --  only the difference between the individual
observations and their mean. Any star observed over months rather than
weeks would have the same effect. In summary, the inclusion of the FK5 
residuals should have helped to remove inconsistencies between two stars in
the same segment of the sky observed in different weeks, but it should not 
have altered the overall system of the catalogue.                                     
                                                                               
The nightly zonal correction for each star was calculated as the mean of the   
residuals of the surrounding programme stars in a strip 2\hh \space in right   
ascension by 60\deg \space in declination. Each star had to be brighter than   
12\mm \space and  have at least four good observations in position             
on other nights. A magnitude residual was computed when three good observations
were available on other nights. In contrast to CMC7, position and magnitude    
in CMC8-11 were dealt with separately in order to increase the number of 
contributing stars in deriving the positional corrections.                     
If the strip did not contain at least seven stars,                             
the right ascension was increased by steps of 1\hh \space and the  declination 
by 30\deg, up to a maximum of 5\hh$\times$150\deg. If still fewer than seven  
stars were found, no correction was calculated.                                
                                                                               
These zonal corrections were applied to all the programme stars, and new       
means and standard deviations (mean errors) were calculated. The mean errors 
for stars in the zenith between 9\mag \space and 11\mag \space were:            
                                                                               
\medskip                                                                       
\begin{center}                                                                 
\tabcolsep15pt                                                                 
 \begin{tabular}{l|c|c|c}                                                      
       &   R.A.   &   Dec.   & Mag. \\                                         
\hline                                                                         
\rule{0pt}{2.5ex}%
Before & 0\pas153 & 0\pas143 & 0\pmag049\\
After  & 0.118    & 0.125    & 0.048$^a$\\
\hline
\end{tabular}                                                                 

$^a$ Further improved to 0\pmag026, as described in \S\,\ref{mag}
\end{center}                                                                   
                                                                               
\medskip                                                                       
The improvement is clear in right ascension and declination, but not in 
magnitude. Nights which were bad photometrically were not included in the 
catalogue; so, significant zonal corrections are not to be expected in 
magnitude. A similar improvement was found for the scatter of the planet 
residuals with respect to the ephemerides.                                     

\subsection{Adjustment to the ICRF}\label{ICRF}
 \subsubsection{CMC1-9}
Whereas CMC10-11 were observed directly with respect to the ICRF via the 
Hipparcos Catalogue, CMC1-9 were necessarily observed with respect to the FK5. 
The positions in CMC1-9 were adjusted to the
ICRF by applying retrospectively systematic differences as a function of RA and 
Dec. These were evaluated as follows.

From a preliminary comparison of the Carlsberg reference frame with the ICRF
using positions of 63 extragalactic nebul{\ae} and 26 radio stars,
Argyle \etal\,(1996) found that the Carlsberg frame deviated from the
ICRF in RA in the range $\pm$0\pas05 and in Dec in the range $-$0\pas05 to
+0\pas12.  Later, with the availability of the Hipparcos Catalogue, which is
aligned to the ICRF to better than 1~mas, a more detailed study (unpublished)
was possible using almost 60\,000 stars (mainly IRS) common to the Carlsberg
and Hipparcos Catalogues. This density of comparison stars allowed a 5\deg~net of
systematic differences, ICRF$-$Carlsberg, to be evaluated. These were applied
to the positions of the stars and planets in CMC1-9. These systematic
differences were not applied to the observed positions of the FK5 stars which
are published in this CD-ROM.

\subsubsection{CMC10-11}
Although CMC10 and CMC11 were observed differentially with respect to the
Hipparcos Catalogue, a comparison made after the formation of these catalogues
revealed systematic differences of $\sim$30\,mas in RA and Dec. These varied
smoothly, approximately as sin\,2$z$, where $z$ is the zenith distance. This
may be the consequence of under-parameterising the nightly adjustment of the
observations to the ICRF, where only the simple Besselian constants were used.
These systematic errors were so clearly defined that it was decided to remove
them from CMC10 and CMC11. The resultant system of the positions should be
within 30\,mas of the ICRF.




\subsection{Planets and satellites}\label{plaandsat}                           
The method of reduction of the planets was similar to that of the stars, but   
with allowance for their motion and defect of illumination.                    
The corrections to the observed right ascension and declination for the        
defect of illumination were calculated from the following relations:           
                                                                               
\[                                                                             
\begin{array}{r@{\,=\,}l}                                                      
\Delta \alpha \cos \delta & 
+0.75\,s\sin\left({\displaystyle\frac{i}{2}}\right)\sin Q\\
[2ex]\Delta \delta             & 
+0.75\,s\sin\left({\displaystyle\frac{i}{2}}\right)\cos Q,  
\end{array}                                                                    
\]                                                                             
where $s$ is the true semi-diameter, $i$ the phase angle and $Q$ the position  
angle of the greatest defect of illumination. The coefficient, 0.75, is taken  
from Lindegren (1977).                                                         
                                                                               
The final nightly zonal solutions obtained from the stars were applied         
to the planet positions, thus reducing them to the same reference frame. In    
common with the programme stars, a constant value of $B-V=+0.5$ was assumed in 
calculating the colour correction in magnitude discussed in \S\,\ref{nightly}.


Corrections for parallax were applied to the apparent topocentric declinations 
of the Solar System objects in order to produce apparent geocentric positions,
except in the case of Geographos, where the topocentric position was retained
because the parallax of the preliminary orbit was not known with sufficient
accuracy. 
                                                                               
\section{Formation of the catalogue}\label{formation}                          

About 1\,047\,000 observations of 176\,600 stars carried out in 36\,000 hours of 
operation on 3634 nights between 1 May 1984 and 27 May 1998 have been compiled 
into this catalogue. The details are given in Table~\ref{periods}. 

\begin{table}
\begin{center}
\caption{Catalogue observation periods.}
\label{periods}
\begin{tabular}{c|rr|c|c|c}
\multicolumn{6}{c}{}\\
\hline
Catalogue & \multicolumn{2}{c|}{Period}          & Hours~of & Nights & Nights \\
&\multicolumn{1}{c}{From}&\multicolumn{1}{c|}{To}& operation&  used  &rejected\\
          &           &                &          &                 & for~mag.\\
\hline
CMC1-4    & 1~May~84             & 21~Feb~88      & 8872     & 955    & 111 \\
CMC5      &16~May~88             &  1~Jan~90      & 3892     & 415    &  61 \\
CMC6      & 3~Jan~90             & 31~Dec~90      & 2478     & 254    &  57  \\
CMC7      & 1~Jan~91             &  5~Aug~92      & 4479     & 466    &  69  \\
CMC8      &19~Aug~92             & 19~Dec~93      & 3415     & 364    &  77  \\
CMC9      & 1~Jan~94             &  5~Apr~95      & 3562     & 365    &  55  \\
CMC10     & 2~May~95             &  9~Dec~96      & 4564     & 446    &  65  \\
CMC11     &13~Dec~96             & 27~May~98      & 4710     & 369    & 100  \\
\hline
\end{tabular}
\end{center}
\end{table}

On average, each star received six independent observations of its position
and magnitude. About 2000 stars were observed in more than one Catalogue.  
The observations in each catalogue were processed independently in the following
manner. Before forming the unweighted means of the observed  positions, bad
observations were eliminated. Those with badly defined stellar images were 
excluded. If the image was not completely within the scanned part
of the sky, the observation was rejected.  Observations were also rejected if  
the images were very spread, thus making it difficult to determine the centre. 
If the real-time reduction process of the scans of the image found a mean 
error in either the $x$ or $y$ 
coordinate of 1\pas15 or more, both the right ascension and declination were   
rejected.  Similarly, the magnitude was rejected if the internal mean          
error was greater than 0\pmag25.  About 4\% of the observations were     
excluded due to these criteria.                                                
                                                                               
In magnitude, as much as 27\% of the nights in a Catalogue were rejected 
because they were not good enough photometrically (see Table~\ref{periods}).
                                                                               
In the final stage of examination, observations with residuals exceeding three
times the mean error (see Table~\ref{errorz}) of a single observation were 
rejected. As a result of this process, about 1\% of the observations in right 
ascension and declination, and 4\% in magnitude were rejected.
                                                                               
Observations of double stars where more than one component entered the slits   
were rejected if the resulting error in the position was greater than          
0\pas1.  In this latest compilation which includes CMC1-9, further checks 
were made against the Washington Double Star catalogue, and as a result 
some stars were rejected which had been issued in 1997 on the CD-ROM
comprising CMC1-9. The component codes were also revised for a number of stars.

Where stars were observed in more than one Catalogue, their independent mean
positions are given in order of the epoch of observation.

                                                                               
%\begin{figure}[p]                                                              
% \vspace{20cm}                                                                 
% \caption{Internal mean error of one observation as a function of declination, 
%          and the zenith mean error as a function of magnitude.}               
% \label{merror}                                                                
%\end{figure}                                                                   
                                                                               
\section{Accuracy of the catalogue}\label{accuracy}                            

The internal mean errors of the observations were calculated from the scatter  
of the observations about their unweighted means.  These were averaged in      
5\deg \space ranges of declination. The mean error for one observation
as a function of zenith distance (z) for stars brighter than ${m=11}$ are 
listed in Table~\ref{errorz}. The accuracy of the observations has improved
with time due to improvements in instrumentation (listed in \S\,\ref{intro}) and
in reduction methods (see \S\,\ref{difred}).  In particular, the introduction
of the new micrometer in May~1988 led to the improvement in CMC5-6, and the  
zonal adjustment (\S\,\ref{zonal}) produced an improvement in CMC7-9. Further 
improvements were obtained in CMC10-11 with the introduction of the Hipparcos 
Catalogue.

\begin{table}
\begin{center}
\caption{Mean error of a {\bf single observation} as a function of zenith distance
        (z) for stars brighter than ${m=11}$.}
\label{errorz}                                                              
\begin{tabular}{l|c|c|c|c}
\multicolumn{5}{c}{}\\
\hline
                              &           CMC1-4              &
                                          CMC5-6            &
                                          CMC7-9            &
					  CMC10-11          \\
\hline
${\epsilon_\alpha}$\,cos\,$\delta$ & 0\pas19\,sec$^{0.7}$z     &
                                     0\pas15\,sec$^{0.7}$z     &
                                     0\pas12\,sec$^{0.7}$z     &
				     0\pas12\,sec$^{0.5}$z    \\
${\epsilon_\delta}$                & 0\pas18\,sec$^{1.1}$z     &
                                     0\pas15\,sec$^{1.1}$z     &
                                     0\pas13\,sec$^{1.1}$z     &
				     0\pas12\,sec$^{1.0}$z    \\
${\epsilon_m}$                     & 0\pmag05\,sec$^{1.0}$z    &
                                     0\pmag05\,sec$^{1.0}$z    &
                                     0\pmag05\,sec$^{0.6}$z    &
				    0\pmag045\,sec$^{0.5}$z   \\
\hline
\end{tabular}
\end{center}
\end{table}
                                                                               
The mean error of a single observation as a function of magnitude, reduced to the
zenith, is given in Table~\ref{errorm}.
\begin{table}
\begin{center}
\caption{Zenith mean error of a {\bf single observation} as a function of magnitude.}
\label{errorm}
\begin{tabular}{l|c|c|c}
 \multicolumn{4}{c}{}\\
\hline                             
                                   &CMC1-4$^a$
                                   &CMC5-6$^b$             
                                   &CMC7-9           \\
\hline

${\epsilon_\alpha}$\,cos\,$\delta$ & 0\pas19+${(m-11)\times0.05}$ 
                                   & 0\pas15+${(m-12)\times0.05}$ 
                                   & 0\pas12+e$^{(m-17.0)\times0.8}$ \\
${\epsilon_\delta}$                & 0\pas19+${(m-11)\times0.05}$ 
                                   & 0\pas15+${(m-12)\times0.05}$ 
                                   & 0\pas12+e$^{(m-17.0)\times0.8}$ \\
${\epsilon_m}$                     & 0\pmag05+${(m-9)\times0.025}$ 
                                   & 0\pmag05+${(m-12)\times0.05}$ 
                                   & 0\pmag05+e$^{(m-16.3)\times0.8}$ \\
\hline
&\multicolumn{1}{l}{${^a; \epsilon_\alpha, \epsilon_\delta, m>11; 
                                           \epsilon_m, m>9}$}  
        &\multicolumn{1}{l}{${^b; m>12}$} & \\
\end{tabular}
\begin{tabular}{l|c|c}
 \multicolumn{3}{c}{}\\
\hline                             
                                   &CMC10
                                   &CMC11            \\             
\hline

${\epsilon_\alpha}$\,cos\,$\delta$ & 0\pas12+e$^{(m-18.3)\times0.8}$
                                   & 0\pas12+e$^{(m-18.3)\times0.8}$ \\
${\epsilon_\delta}$                & 0\pas12+e$^{(m-18.3)\times0.8}$ 
                                   & 0\pas12+e$^{(m-18.3)\times0.8}$ \\
${\epsilon_m}$                     & 0\pmag04+e$^{(m-23.0)\times0.4}$ 
                                   & 0\pmag03+e$^{(m-22.0)\times0.4}$ \\ 
\hline
\end{tabular}
\end{center}
\end{table}                                                                    

A catalogue position is the mean of several independent observations, so the   
accuracy is better than that of a single transit given by the expressions 
in Table~\ref{errorm}. It is assumed that the accuracy of a position based on 
$n$ observations can be expressed as                                                            
\bigskip                                                                       
\[                                                                             
\epsilon_n = \sqrt{a^2 + b^2/n},                                               
\]                                                                             
where $a$ is the asymptotic mean error and  $b$ is the internal mean error given
in Table~\ref{errorm}. Taking the values of $a$ from Morrison\,\etal\,(1990), 
we derive the expressions listed in Table~\ref{errorc} for the external mean
error of a catalogue position as a function of the number of observations $n$, 
zenith distance $z$  and magnitude $m$.
\begin{table}
\begin{center}
\caption{Mean error of a catalogue position as a function of number of 
   observations $n$, zenith distance $z$ and magnitude $m$.}
\label{errorc}
{\footnotesize
\begin{tabular}{l|c|c}
\multicolumn{3}{c}{}\\
\hline
   & ${\epsilon_\alpha\,{\rm cos}\,\delta}$ & ${\epsilon_\delta}$ \\
\hline
      CMC1-4$^a$    & ${ \left\{                    
                    0\pass035^2+{\displaystyle\frac{1}{n}} 
                  \left[                                     
               0\pass19+(m-11)\times0.05\vphantom{\frac{1}{1}}                 
                  \right]^2                                                    
                    \sec^{1.2}z                                           
             \right\}^{\frac{1}{2}}}$   &
        ${  \left\{                                                            
                    0\pass049^2+{\displaystyle\frac{1}{n}}                   
                  \left[                                                       
              0\pass19+(m-11)\times0.05\vphantom{\frac{1}{1}}            
                  \right]^2                                                    
                    \sec^{1.8}z                                                
             \right\}^{\frac{1}{2}}}$ \\ 
      CMC5-6$^b$    & ${  \left\{  
                    0\pass035^2+{\displaystyle\frac{1}{n}}                     
                  \left[                                                       
              0\pass15+(m-12)\times0.05\vphantom{\frac{1}{1}}            
                  \right]^2                                                    
                    \sec^{1.2}z                                                
             \right\}^{\frac{1}{2}}}$  &
         ${   \left\{                                                          
                    0\pass049^2+{\displaystyle\frac{1}{n}}                     
                  \left[                                                       
              0\pass15+(m-12)\times0.05\vphantom{\frac{1}{1}}            
                  \right]^2                                                    
                    \sec^{2.2}z                                                
             \right\}^{\frac{1}{2}}}$  \\                                       
CMC7-9 & ${   \left\{                                                          
                    0\pass035^2 + {\displaystyle\frac{1}{n}}                   
                  \left[                                                       
              0\pass12+{\rm e}^{(m-17.0)\times0.8}\vphantom{\frac{1}{1}}       
                  \right]^2                                                    
                    \sec^{1.4}z                                                
             \right\}^{\frac{1}{2}}}$  &
          ${   \left\{                                                         
                    0\pass049^2+{\displaystyle\frac{1}{n}}                     
                  \left[                                                       
                    0\pass12+{\rm e}^{(m-17.0)\times0.8}\vphantom{\frac{1}{1}} 
                  \right]^2                                                    
                    \sec^{2.2}z                                                
             \right\}^{\frac{1}{2}}}$  \\
CMC10-11 & ${   \left\{                                                          
                    0\pass035^2 + {\displaystyle\frac{1}{n}}                   
                  \left[                                                       
              0\pass12+{\rm e}^{(m-18.3)\times0.8}\vphantom{\frac{1}{1}}       
                  \right]^2                                                    
                    \sec^{1.0}z                                                
             \right\}^{\frac{1}{2}}}$  &
          ${   \left\{                                                         
                    0\pass049^2+{\displaystyle\frac{1}{n}}                     
                  \left[                                                       
                    0\pass12+{\rm e}^{(m-18.3)\times0.8}\vphantom{\frac{1}{1}} 
                  \right]^2                                                    
                    \sec^{2.0}z                                                
             \right\}^{\frac{1}{2}}}$  \\
\hline  
\end{tabular} }
\end{center}
{\footnotesize ${^a; m>11}$ \hspace{5mm} ${^b; m>12}$}
\end{table}                                                                    
                          
Table~\ref{error11} gives the mean error of a catalogue position calculated
from the expressions in Table~\ref{errorc} for a star of magnitude 11 having
six observations, which is the customary number.
\begin{table}
\caption{Mean error of a catalogue position for a star of $m$=11 with $n$=6.}  
\label{error11}
\begin{center}                                                                 
\begin{tabular}{c|cc|cc|cc|cc}                                                 
\multicolumn{9}{c}{}\\
\hline                                                                         
$z$\rule{0pt}{3ex}                                                             
        &\multicolumn{2}{c|}{ 0\deg}                                           
        &\multicolumn{2}{c|}{30\deg}                                           
        &\multicolumn{2}{c|}{60\deg}                                           
        &\multicolumn{2}{c}{68\pdeg8}\\[1.5ex]                                 
$\delta$&\multicolumn{2}{c|}{+29\deg}                                          
        &\multicolumn{2}{c|}{$-1\deg,+59\deg$}                                 
        &\multicolumn{2}{c|}{$-31\deg,+89\deg$}                                
        &\multicolumn{2}{c}{$-40\deg$}  \\[1.5ex]                              
\hline                                                                         
\hline                                                                         
   \rule{0pt}{2.5ex}                                                           
      &$\epsilon_\alpha$&$\epsilon_\delta$                                     
      &$\epsilon_\alpha$&$\epsilon_\delta$                                     
      &$\epsilon_\alpha$&$\epsilon_\delta$&                                    
      $\epsilon_\alpha$&$\epsilon_\delta$\\[1ex]                               
\hline                                                                         
\rule{0pt}{3ex}CMC1-4                                                            
    &0\pas09&0\pas09&0\pas09&0\pas10&0\pas13&0\pas17&0\pas16&0\pas24\\         
CMC5-6   &0.07 &0.08 &0.08 &0.09 &0.11 &0.14 &0.13 &0.19\\                  
CMC7-9   &0.06 &0.07 &0.07 &0.08 &0.09 &0.12 &0.11 &0.17\\               
CMC10-11 &0.06 &0.07 &0.06 &0.08 &0.08 &0.11 &0.09 &0.15\\                
\hline
\end{tabular}                                                                  
\end{center}                                                                   
\end{table}                                                                    
Table~\ref{error13} gives the mean error of a catalogue position calculated
from the expressions in Table~\ref{errorc} for a star of magnitude 13 having
six observations.
\begin{table}
\caption{Mean error of a catalogue position for a star of $m$=13 with $n$=6.}
\label{error13}
\begin{center}                                                                 
\begin{tabular}{c|cc|cc|cc|cc}                                                 
\multicolumn{9}{c}{}\\
\hline                                                                         
$z$\rule{0pt}{3ex}                                                             
        &\multicolumn{2}{c|}{ 0\deg}                                           
        &\multicolumn{2}{c|}{30\deg}                                           
        &\multicolumn{2}{c|}{60\deg}                                           
        &\multicolumn{2}{c}{68\pdeg8}\\[1.5ex]                                 
$\delta$&\multicolumn{2}{c|}{+29\deg}                                          
        &\multicolumn{2}{c|}{$-1\deg,+59\deg$}                                 
        &\multicolumn{2}{c|}{$-31\deg,+89\deg$}                                
        &\multicolumn{2}{c}{$-40\deg$}  \\[1.5ex]                              
\hline                                                                         
\hline                                                                         
   \rule{0pt}{2.5ex}                                                           
      &$\epsilon_\alpha$&$\epsilon_\delta$                                     
      &$\epsilon_\alpha$&$\epsilon_\delta$                                     
      &$\epsilon_\alpha$&$\epsilon_\delta$&                                    
      $\epsilon_\alpha$&$\epsilon_\delta$\\[1ex]                               
\hline                                                                         
\rule{0pt}{3ex}CMC1-4                                                            
    &0\pas10&0\pas11&0\pas11&0\pas12&0\pas15&0\pas19&0\pas18&0\pas25\\         
CMC5-6   &0.09 &0.10 &0.10 &0.11 &0.13 &0.18 &0.15 &0.25\\                       
CMC7-9   &0.07 &0.08 &0.08 &0.09 &0.11 &0.15 &0.14 &0.21\\                       
CMC10-11 &0.07 &0.07 &0.07 &0.08 &0.09 &0.12 &0.10 &0.16\\                       
\hline
\end{tabular}                                                                  
\end{center}                                                                   
\end{table}                                                                    

The external mean error of a catalogue magnitude for stars having four or more 
observations was obtained by comparing the magnitudes of stars having          
photoelectric standards in the catalogue of Nicolet (1978) for CMC1-9 and 
Hipparcos for CMC10-11.  The stars were     
limited to those brighter than \mv = 11 because it can be seen from 
Table~\ref{errorm} that the mean error of individual observations increases for
stars fainter than this limit.  The average resultant external mean error of 
stars brighter than about \mv=11.0 is 0\pmag045 in CMC1-10 and 0\pmag040
in CMC11 and it is independent of 
declination. For stars fainter than this the mean errors rise in accordance 
with the expressions in Table~\ref{errorm}.
                                                                               
\section{Number and distribution of observations}\label{number}                

Tables~\ref{starobser} and \ref{solarsys} list the main programmes and numbers 
of observations in this compilation catalogue. About 2000 stars have more than 
one entry in this compilation. Sometimes the same star was re-observed under 
another number because it was not realized initially that the imprecise input 
positions referred to the same star. In some cases stars were re-observed 
deliberately, either to investigate some problem with the first observation, 
or to improve the accuracy of the position. Non-stellar objects are listed
in Table~\ref{nonstellar}, and nov\ae~and supernov\ae~in Table~\ref{nova}.

The minor planets fall into several categories regarding their frequency of        
observation. Those being monitored for brightness variations, leading to
the establishment of phase relations, were observed nightly.
Minor planets requiring improvements in their orbits for observation by
the Infrared Space Observatory were also observed nightly.
Those included in the H{\sc ipparcos} satellite programme were observed 
weekly in order to provide a long-term baseline extending beyond the duration 
of the space mission. Minor planets having their masses determined from
mutual perturbations were scheduled every tenth night.

The distribution of the stars with magnitude is bimodal, reflecting the 
large survey programmes: IRS and Lick NPM with a median around 9\,mag,  
and the faint and special reference stars around 12\,mag. There is a 
general progression from brighter to fainter stars between CMC1-4 and
CMC9 as a result of the completion of the IRS in the early years and
the improvements in instrumentation which made the observation of fainter
stars possible.

\begin{table}
\caption{Programmes and number of observations of stars.}
\label{starobser}                                                              
\begin{center}                                                                 
{\footnotesize
\begin{tabular}{@{}c@{}}                                                       
\rule{0pt}{3ex}\large\bf Stars \\[1ex]                                         
\hline                                                                         
\begin{tabular}{lrrr}                                                          
\rule{0pt}{3ex} CMC1-11&
                \multicolumn{1}{c}{R.A.}&                                      
                \multicolumn{1}{c}{Dec.}&                                      
                \multicolumn{1}{c}{ Mag.} \\[1ex]                              
\hline                                                                         
\rule{0pt}{2.5ex}%                                                             
Number of observations  & 1047966   & 1047016  & 822121 \\[.5ex]
Number of stars         &  176591   &  176591  & 168989 \\[.5ex]
\end{tabular}\\[1.5ex]                                                         
\begin{tabular}{l|r|r|c}
\hline                                                                         
&\multicolumn{1}{|c|}{No. of stars}&\multicolumn{1}{|c|}{No. of stars}&
                                               \multicolumn{1}{c}{Percentage}\\
\multicolumn{1}{c}{\bf Programmes}&\multicolumn{1}{|c|}{in programme}&
              \multicolumn{1}{|c|}{observed}&\multicolumn{1}{c}{completed}\\
%\omit\hfill\bf Programmes\hfill\vline &&&&&&&\\                                 
\hline
{\bf Reference frame}  &&&\\
International Reference Stars: mainly in Hipparcos Catalogue           & 35886
                                                           & 34632 & 97\\
Faint reference stars, 10$<$V$<$12: mainly AC; density 1 per sq deg    & 35600
                                                           & 33276 & 93\\
General Catalogue of 33342 stars (Boss)                                & 24296
                                                           & 15634 & 64\\
Reference stars in radio source fields: mainly ICRF                    & 11397
                                                           & 10061 & 88\\
Hipparcos Catalogue, V$>$11                                            & 2096
                                                           &  1783 & 85\\
Radio stars                                                            &   280
                                                           &   238 & 85\\
Problematical AGK stars                                                &  857
                                                           &   687 & 80\\
&&&\\
{\bf Position and proper motion} &&&\\
Gliese catalogue of nearby stars and CNS3 (12$<$V$<$14)  &  2808 &  2436 & 87\\
Luyten (NLTT, 12$<$V$<$14, ${\mu>0\pass3}$)&  2955 &  2427 & 82 \\
Luyten (NLTT, 12$<$V$<$14, ${0\pass18<\mu<0\pass3}$)&  7508 & 4988 & 66 \\
Variable stars (GCVS, 12$<$V$<$14)            &  3383 & 3029 & 90 \\
Lick NPM catalogue                       & 33053 & 18053 & 55 \\
&&&\\
{\bf Proper motion} &&&\\
F-type stars within 100 pc               & 10544 &  9631 & 91 \\
G-type d\&g, K-type giants within 300 pc &  9243 &  8778 & 95 \\
Nearby O-B associations                  &  6555 &  5693 & 87 \\
Sample of A5-G0 stars in N. Gal. Pole    &  3098 &  2985 & 96 \\
Unbiased sample of K/M dwarfs            &  2241 &  2179 & 97 \\
High-vel./ metal-poor stars              &  1277 &  1090 & 85 \\
Disk and halo dwarfs                     &   899 &   870 & 97 \\
Gould Belt stars                         &  1142 &   781 & 68 \\
Peculiar F/K stars                       &  1564 &  1096 & 70 \\
Wide binaries in Galactic Pole           &   624 &   579 & 93 \\            
&&&\\
{\bf Special reference stars for -} &&&\\
ESA {\it Giotto} mission to Comet Grigg-Skjellerup   &  1061 & 1057 & 99 \\
NASA {\it Galileo} flyby of Asteroid 243 Ida          &  2030 & 1321 & 65 \\
Schmidt fields for STScI GSC1.2 (equatorial band)    & 12547 & 11893 & 95 \\
Stars 10$<$V$<$13 within 20 arc min of Veron-Cetty galaxies &  - 
                                                             & 19434 &  - \\
Stars in fields of Seyfert galaxies                 & 583  & 516 & 89 \\
Prediction of occultations by Neptune               &  604 & 343 & 57 \\
Prediction of occultations by Pluto                 & 716  & 388 & 54 \\
&&&\\
{\bf Nov\ae\,\&\,Supernov\ae}     &  -   &  20  &  - \\
&&&\\
{\bf Non-stellar objects}         &   -  & 24   &  - \\
\hline                                                                         
\end{tabular} 
\end{tabular} }
\end{center}                                                                   
\end{table}

%%%%%%%%%%%%%%%%%% Previous version given in CMC9 %%%%%%%%%%%%%%%%%%%%%%%%
%\begin{table*}[ht]                                                             
%\caption{Programmes and number of observations of stars.}
%\label{starobser}                                                              
%\begin{center}                                                                 
%{\footnotesize
%\begin{tabular}{@{}c@{}}                                                       
%\rule{0pt}{3ex}\large\bf Stars \\[1ex]                                         
%\hline                                                                         
%\begin{tabular}{lrrr}                                                          
%\rule{0pt}{3ex} CMC1-9&
%                \multicolumn{1}{c}{R.A.}&                                      
%                \multicolumn{1}{c}{Dec.}&                                      
%                \multicolumn{1}{c}{ Mag.} \\[1ex]                              
%\hline                                                                         
%\rule{0pt}{2.5ex}%                                                             
%Number of observations  & 831336   &  830400  &  680058 \\[.5ex]               
%Number of stars         & 138603   &  138603  &  135734 \\[.5ex]               
%\end{tabular}\\[1.5ex]                                                         
%\begin{tabular}{l|r|rrrrrr}                                                     
%\hline                                                                         
%&\multicolumn{1}{|c|}{No. of}&\multicolumn{6}{c}{Number of stars in --}\\ 
%\omit\hfill\bf Programmes\hfill\vline &&&&&&&\\                                 
%&\multicolumn{1}{|c|}{stars}            & CMC1-4 &  CMC5 & CMC6 & CMC7 & CMC8 
%                                                                      & CMC9\\
%\hline                                                                         
%{\bf Reference frame}  &&&&&&&\\                                                
%International Reference Stars   & 35895 & 21328 &  3883 &  3162 & 2925 & 1956
%                                                                       &  561\\
%Faint reference stars           & 35600 &    -  &  2258 &  4143 & 9447 & 7546
%                                                                       & 5034\\
%General Catalogue               & 24296 &  8957 &  1963 &  1153 & 1574 & 1872
%                                                                       &  639\\
%Reference stars in radio fields & 11394 &  6829 &  1158 &  1040 &  736 &  689
%                                                                       &  867\\
%PZT stars                       &  1957 &   797 &   132 &   155 &  189 &  142
%                                                                       &   41\\
%Radio stars                     &   313 &   203 &    72 &    28 &   15 &    8
%                                                                       &    -\\
%Gliese catalogue of nearby stars&  2808 &   412 &   365 &    98 &  315 &  413
%                                                                       &  466\\
%&&&&&&&\\                                                                       
%{\bf Proper motion} &&&&&&&\\                                                   
%Lick NPM catalogue              & 33052 &  2563 &   861 &   776 & 2015 & 3725
%                                                                       & 2092\\
%F-type stars within 100 pc      & 10550 &  9209 &   718 &   100 &   11 &    8
%                                                                       &    -\\
%G-type d\&g, K-type g $<$300 pc &  9243 &  5665 &  2271 &   786 &  489 &   20
%                                                                       &    -\\
%Nearby O-B associations         &  5629 &  2548 &  1082 &   751 &  281 &  636
%                                                                       &  326\\
%Sample of A5-G0 stars in NGP    &  3098 &   399 &  1234 &   889 &  374 &  134
%                                                                       &    -\\
%Unbiased sample of K/M dwarfs   &  2241 &    -  &  1242 &   535 &  381 &   23
%                                                                       &    -\\
%High-vel./ metal-poor stars     &  1277 &   302 &   197 &   345 &  225 &   21
%                                                                       &    -\\
%Disk and halo dwarfs            &   899 &    -  &       &   329 &  504 &   27
%                                                                       &    -\\
%Luyten (NLTT, ${11<V<14, \mu>0\pass3}$)&  2955 &-  &  -  &     - &    - &    -
%                                                                       &  777\\
%Variables (GCVS, ${12<V<14}$)    &  3383 &    -  &    -  &     - &    - &    -
%                                                                       & 1048\\
%&&&&&&&\\                                                                       
%{\bf Special reference stars for -} &&&&&&&\\
%Giotto/Comet Grigg-Skjellerup   &  1061 &    -  &    -  &    -  & 1033 &   -
%                                                                       &   -\\ 
%Galileo/Asteroid 243 Ida        &  2030 &    -  &   -   &    -  & 1074 &  226
%                                                                       &    -\\
%Veron-Cetty galaxies            &  4209 &    -  &    -  &    -  &    - &    -
%                                                                       & 2205\\
%Schmidt fields (equatorial band)& 12547 &    -  &    -  &    -  &   -  &    -
%                                                                       & 5844\\
%&&&&&&&\\
%{\bf Nov\ae\,\&\,Supernov\ae}     &  15   &    -  &    -  &     -  &   3 &  5 
%                                                                       &  7  \\ 
%&&&&&&&\\
%{\bf Non-stellar objects}         &   25 & 1   & 7       & 4     &   10    & 3 
%                                                                       & 1 \\
%\hline                                                                         
%\end{tabular} 
%\end{tabular} }
%\end{center}                                                                   
%\end{table*}                                                                    

\begin{table}
\caption{List of non-stellar objects in CMC1-11.}
\label{nonstellar}                                                              
\begin{center}                                                                 
\rule{0pt}{3ex}\large\bf Non-stellar objects \\[1ex]
{\footnotesize
\begin{tabular}{ll|ll|ll}
\hline                                                                         
\rule{0pt}{3ex} CMC No.&
                \multicolumn{1}{c|}{Name}&                                      
                CMC No.&
                \multicolumn{1}{c|}{Name}&                                      
                CMC No.&
                \multicolumn{1}{c}{Name} \\[1ex]                              
\hline
 408181     & 3C 273B     & 604912 & Mark~421   & 714318 & PG1634+706\\
 605671     & 3C 273B     & 605513 & PG1211+143 & 716343 & Q1807+698\\
 809567     & 3C 273B     & 609616 & SS~433     & 716702 & Q1821+643\\
            &             &        &            &        &          \\
 504665     & MS07546+39  & 701487 & NGC~1068   & 800771 & M\,31   \\
 505011     & PG0844+349  & 708322 & Mark~1298  & 801455 & Mark~359 \\
 506082     & Mark~421    & 708527 & WAS~26     & 806953 & Mark~79 \\
 507138     & Mark~231    & 711095 & PG1351+64  &        &         \\
 508442     & Mark~478    & 711527 & PG1411+442 & 903323 & Q0422+004\\
 510047     & Mark~501    & 711816 & Mark~1383  & \\
 510463     & PG1718+481  & 712788 & AP~Lib     & \\
\hline               
\end{tabular} }
\end{center}
\end{table}

\begin{table}
\caption{List of nov\ae~and supernov\ae.}
\label{nova}
\begin{center}
\rule{0pt}{3ex}\large\bf Nov\ae~\& Supernov\ae \\[1ex]
{\footnotesize
\begin{tabular}{ll|ll|ll|ll}
\hline                                                                         
\rule{0pt}{3ex} CMC No.&
                \multicolumn{1}{c|}{Name}&                                      
                CMC No.&
                \multicolumn{1}{c|}{Name}&                                      
                CMC No.&
                \multicolumn{1}{c|}{Name}&                                      
                CMC No.&
                \multicolumn{1}{c}{Name} \\[1ex]                              
\hline
  807251 & N~Pup~1991      & 908250 & SN~1993J     & 911862 & SN~1994I  &
                                                    1001331 & N~Cass~1995\\
  803614 & SN~1992A        & 813501 & N~Aql~1993   & 909030 & SN~1994AE &
                                                    1017345 & N~Aql~1995\\
  718963 & N~Cyg~1992      & 817814 & N~Cas~1993   & 915764 & N~Oph~1994&
                                                    1016156 & N~Sgr~1996\\ 
  715036 & N~Sco~1992      & 812327 & N~Oph~1993   & 908039 & SN~1995D & 
                                                    1110802 & N~Sco~1997\\
  716727 & N~Sgr~1992~No.2 & 910850 & SN~1994D     & 907458 & SN~1995E &
                                                    1105767 & SN~1998S\\
\hline                                                                         
\end{tabular} }
\end{center}                                                                   
\end{table}                                                                    
                                                                               

\begin{table}
\begin{center}                                                                 
\caption{Number of observations of Solar System objects.}                      
\label{solarsys}                                                               
{\footnotesize 
\begin{tabular}{@{}c@{}||@{}c@{}}                                              
\multicolumn{2}{c}{\rule{0pt}{4ex}\large\bf Solar System CMC1-11} \\[2ex]       
\hline                                                                         
\begin{tabular}{rlrrr}                                                         
\rule{0pt}{3ex}&&\multicolumn{1}{c}{R.A.}&                                     
                   \multicolumn{1}{c}{Dec.}&                                   
                   \multicolumn{1}{c}{ Mag.} \\[1ex]                           
\hline                                                                         
\multicolumn{5}{c}{\bf Major planets\rule{0pt}{2.5ex}} \\[.5ex]                
                  &Uranus  & 883 & 883 & 483  \\                               
                  &Neptune &1106 &1106 & 645  \\                               
                  &Pluto   & 380 & 380 & 269  \\                               
\hline                                                                         
\multicolumn{5}{c}{\bf Satellites\rule{0pt}{2.5ex}} \\[.5ex]                   
                  &Callisto& 440 & 440 & 264 \\                               
                  &Ganymede& 218 & 218 & 165  \\                               
                  &Rhea    &  12 &  12 &   8  \\                               
                  &Titan   & 400 & 400 & 236  \\                               
                  &Iapetus & 231 & 231 & 187  \\                               
                  &Hyperion&  87 &  87 &  38  \\                               
                  &Oberon  & 147 & 147 &  63  \\
\hline                                                                         
\multicolumn{5}{c}{\bf Minor planets\rule{0pt}{2.5ex}}  \\[.5ex]               
1 &  Ceres       & 340    & 340    & 273 \\
2 &  Pallas      & 372    & 372    & 298 \\
3 &  Juno        & 342    & 342    & 287 \\
4 &  Vesta       & 264    & 264    & 217 \\
5 &  Astraea     & 207    & 207    & 170 \\
6 &  Hebe        & 336    & 336    & 288 \\
7 &  Iris        & 344    & 344    & 286 \\
8 &  Flora       & 388    & 388    & 322 \\
9 &  Metis       & 232    & 232    & 202 \\
10 & Hygiea      & 530    & 530    & 428 \\
11 & Parthenope  & 192    & 192    & 151 \\
12 & Victoria    & 257    & 257    & 199 \\
13 & Egeria      & 265    & 265    & 204 \\
14 & Irene       & 207    & 207    & 162 \\
15 & Eunomia     & 309    & 309    & 248 \\
16 & Psyche      & 464    & 464    & 356 \\
17 & Thetis      & 161    & 161    & 107 \\
18 & Melpomene   & 303    & 303    & 248 \\
19 & Fortuna     & 304    & 304    & 243 \\
20 & Massalia    & 265    & 265    & 212 \\
21 & Lutetia     & 238    & 238    & 185 \\
22 & Kalliope    & 432    & 432    & 348 \\
23 & Thalia      & 229    & 229    & 182 \\
24 & Themis      & 153    & 153    & 107 \\
27 & Euterpe     & 193    & 193    & 162 \\
28 & Bellona     & 209    & 209    & 157 \\
29 & Amphitrite  & 285    & 285    & 228 \\
30 & Urania      & 188    & 188    & 146 \\
31 & Euphrosyne  & 151    & 151    & 94  \\
32 & Pomona      &   4    &   4    &   1 \\
34 & Circe       & 366    & 366    & 273 \\
35 & Leukotha    & 312    & 312    & 221 \\
37 & Fides       & 171    & 171    & 137 \\
38 & Leda        & 349    & 349    & 245 \\
39 & Laetitia    & 243    & 243    & 201 \\
40 & Harmonia    & 326    & 326    & 262 \\
42 & Isis        & 207    & 207    & 136 \\
44 & Nysa        & 278    & 278    & 222 \\
\end{tabular}                                                                  
&                                                                              
\begin{tabular}{rlrrr}                                                         
\rule{0pt}{3ex}&&\multicolumn{1}{c}{R.A.}&                                     
                   \multicolumn{1}{c}{Dec.}&                                   
                   \multicolumn{1}{c}{ Mag.} \\[1ex]                           
\hline                                                                         
\multicolumn{5}{c}{\bf Minor planets (cont.)\rule{0pt}{2.5ex}}  \\[.5ex]       
45 &Eugenia                 &   152     &      152   &        108   \\ 
46 &Hestia                   &  102     &      102   &         62   \\ 
49 &Pales                     &  40     &       40   &         18   \\ 
50 &Virginia                &   271     &      271   &        182   \\ 
51 &Nemausa                 &   310     &      310   &        247   \\ 
52 &Europa                  &   237     &      237   &        203   \\  
55 &Pandora                 &   428     &      428   &        337   \\  
57 &Mnemosyne               &    22     &       22   &         14   \\  
63 &Ausonia                 &   193     &      193   &        146   \\  
65 &Cybele                  &    73     &       73   &         39   \\  
66 &Maja                    &   241     &      241   &        147   \\  
67 &Asia                    &    14     &       14   &         10   \\  
68 &Leto                    &   194     &      194   &        155   \\  
69 &Hesperia                &    16     &       16   &          6   \\  
70 &Panopaea                &    20     &       20   &          6   \\  
72 &Feronia                 &   208     &      208   &        161   \\  
74 &Galatea                 &   302     &      302   &        217   \\  
75 &Eurydike                &   315     &      315   &        210   \\  
76 &Freia                   &     5     &        5   &          2   \\  
77 &Frigga                  &   359     &      359   &        232   \\  
82 &Alkmene                 &   277     &      277   &        192   \\  
84 &Klio                    &    31     &       31   &         22   \\  
87 &Sylvia                  &   293     &      293   &        198   \\  
88 &Thisbe                  &   282     &      282   &        224   \\  
89 &Julia                   &   116     &      116   &         82   \\  
91 &Aegina                  &    16     &       16   &         11   \\  
93 &Minerva                 &     6     &        6   &          3   \\  
97 &Klotho                  &   260     &      260   &        205   \\  
101& Helena                 &    21     &       21   &         12   \\  
107& Camilla                &    29     &       29   &         17   \\  
109& Felicitas              &     13    &        13  &           4  \\  
110& Lydia                  &     28    &        28  &          18  \\  
111& Ate                    &     24    &        24  &          15  \\  
113& Amalthea               &     19    &        19  &          11  \\  
114& Kassandra              &    283    &       283  &         190  \\  
115& Thyra                  &    149    &       149  &         112  \\  
117& Lomia                  &    306    &       306  &         207  \\  
119& Althaea                &    291    &       291  &         225  \\  
121& Hermione               &     11    &        11  &           6  \\  
124& Alkeste                &     20    &        20  &          18  \\  
126& Velleda                &     19    &        19  &          12  \\  
129& Antigone               &    226    &       226  &         182  \\  
133& Cyrene                 &     12    &        12  &           3  \\  
136& Austria                &      4    &         4  &           2  \\  
140& Siwa                   &     24    &        24  &          10  \\  
147& Protogeneia            &     15    &        15  &           5  \\  
159& Aemilia                &     30    &        30  &          14  \\  
165& Loreley                &     20    &        20  &          12  \\  
170& Maria                  &     10    &        10  &           4  \\  
171& Ophelia                &     20    &        20  &           4  \\  
192& Nausikaa               &    171    &       171  &         127  \\  
196& Philomela              &    257    &       257  &         214  \\  
   &                        &           &            & (cont.)      \\
\omit\rule{0pt}{8pt}&&&&                                                
\end{tabular}\\                                                                
\hline                                                                         
\end{tabular} }
\end{center}
\end{table}
\vspace{5cm}
\begin{center}
{\footnotesize
\begin{tabular}{@{}c@{}||@{}c@{}}                                              
\hline                                                                         
\begin{tabular}{rlrrr}                                                         
\rule{0pt}{3ex}&&\multicolumn{1}{c}{R.A.}&                                     
                   \multicolumn{1}{c}{Dec.}&                                   
                   \multicolumn{1}{c}{ Mag.} \\[1ex]                           
\hline                                                                         
\multicolumn{5}{c}{\bf Minor planets (cont.)\rule{0pt}{2.5ex}}  \\[.5ex]
197& Arete           &            23    &        23  &           9 \\
201& Penelope        &            18    &        18  &          11 \\
207& Hedda           &             3    &         3  &           1 \\
216& Kleopatra       &           126    &       126  &          99 \\
219& Thusnelda       &           199    &       199  &         134 \\
221& Eos             &             8    &         8  &           7 \\
224& Oceana          &             4    &         4  &           1 \\
229& Adelinda        &             3    &         3  &           0 \\
230& Athamantis      &           162    &       162  &         130 \\
233& Asterope        &           251    &       251  &         165 \\
242& Kriemhild       &             4    &         4  &           3 \\
243& Ida             &            33    &        33  &          26 \\
250& Bettina         &            28    &        28  &          17 \\
251& Sophia          &            10    &        10  &           3 \\
253& Mathilde        &            45    &        45  &          27 \\
255& Oppavia         &             1    &         1  &           0 \\
256& Walpurga        &             1    &         1  &           0 \\
263& Dresda          &             4    &         4  &           1 \\
271& Penthesilea     &             2    &         2  &           1 \\
277& Elvira          &             6    &         6  &           2 \\
287& Nephthys        &            15    &        15  &           7 \\
289& Nenetta         &             6    &         6  &           3 \\
294& Felicia         &            18    &        18  &          15 \\
305& Gordonia        &             8    &         8  &           3 \\
308& Polyxo          &           281    &       281  &         193 \\
313& Chaldaea        &            25    &        25  &          12 \\
314& Rosalia         &            10    &        10  &           2 \\
324& Bamberga        &           261    &       261  &         212 \\
337& Devosa          &           191    &       191  &         132 \\
339& Dorothea        &             4    &         4  &           1 \\
341& California      &            11    &        11  &           4 \\
343& Ostara          &             2    &         2  &           2 \\
347& Pariana         &             4    &         4  &           1 \\
348& May             &            14    &        14  &          10 \\
349& Dembowska       &           288    &       288  &         236 \\
351& Yrsa            &             7    &         7  &           4 \\
354& Eleonora        &           186    &       186  &         144 \\
356& Liguria         &             6    &         6  &           3 \\
357& Ninina          &             7    &         7  &           4 \\
366& Vincentina      &            13    &        13  &           6 \\
389& Industria       &            31    &        31  &          18 \\
\end{tabular}                                                                  
&                                                                              
\begin{tabular}{rlrrr}                                                         
\rule{0pt}{3ex}&&\multicolumn{1}{c}{R.A.}&                                     
                   \multicolumn{1}{c}{Dec.}&                                   
                   \multicolumn{1}{c}{ Mag.} \\[1ex]                           
\hline                                                                         
\multicolumn{5}{c}{\bf Minor planets (cont.)\rule{0pt}{2.5ex}}  \\[.5ex]       
401& Ottilia             &         2   &          2  &           2  \\
410& Chloris             &       232   &        232  &         142  \\
415& Palatia             &        18   &         18  &           9  \\
423& Diotima             &       294   &        294  &         229  \\
433& Eros                &        51   &         51  &          26  \\
445& Edna                &        10   &         10  &           7  \\
447& Valentine           &         9   &          9  &           2  \\
451& Patientia           &       219   &        219  &         154  \\
454& Mathesis            &        23   &         23  &          17  \\
465& Alekto              &         2   &          2  &           1  \\
471& Papagena            &       268   &        268  &         203  \\
489& Comacina            &        10   &         10  &           4  \\
491& Carina              &        12   &         12  &           4  \\
492& Gismonda            &         1   &          1  &           1  \\
494& Virtus              &        24   &         24  &          13  \\
511& Davida              &       242   &        242  &         191  \\
532& Herculina           &       221   &        221  &         170  \\
534& Nassovia            &        10   &         10  &           2  \\
540& Rosamunde           &         8   &          8  &           7  \\
547& Praxedis            &         4   &          4  &           1  \\
570& Kythera             &       189   &        189  &         125  \\
579& Sidonia             &         9   &          9  &           3  \\
589& Croatia             &        15   &         15  &           8  \\
598& Octavia             &         6   &          6  &           3  \\
628& Christine           &        22   &         22  &          15  \\
631& Philippina          &        29   &         29  &          14  \\
661& Cloelia             &         7   &          7  &           4  \\
670& Ottegebe            &        15   &         15  &           7  \\
701& Oriola              &         4   &          4  &           3  \\
704& Interamnia          &       252   &        252  &         189  \\
714& Ulula               &        15   &         15  &           4  \\
720& Bohlinia            &        19   &         19  &          11  \\
721& Tabora              &        63   &         63  &          27  \\
739& Mandeville          &        10   &         10  &           2  \\
757& Portlandia          &        14   &         14  &          10  \\
786& Bredichina          &        15   &         15  &          10  \\
804& Hispania            &        14   &         14  &           8  \\
976& Benjamina           &         8   &          8  &           4  \\
1539& Borrelly           &          8  &           8 &            6 \\
1605& Milankovitch       &          2  &           2 &            1 \\
1620& Geographos         &         16  &          16 &           13 \\
4179& Toutatis           &          9  &           9 &            9 \\
    & P/Wild 2           &         23  &          23 &           13 \\
\omit\rule{0pt}{8pt}&&&&                                                       
\end{tabular}\\                                                                
\hline                                                                         
\end{tabular} } 
\end{center}                                                                   

\section{Proper motions}\label{pm}                                             

The positions of stars in CMC1-11 were combined with observations at previous 
epochs in order to derive their proper motions. This work was divided into two
main categories which evolved with time as the PPM catalogue (R\"oser \&
Bastian 1993) and the machine-readable version of the Astrographic Catalogue
(AC) became available.

The first category of proper motion applied to stars which are brighter
than V$\sim$11 and were thus to be found in the PPM catalogue.
The PPM proper motions were improved by combining the CAMC
position with the covariance matrix in the PPM, employing the method given by 
Eichhorn (1974, section 3.2.2). The PPM positions are given at equinox 
J2000.0 in the FK5 system.

The PPM was not available for CMC1-4, and in
this case the early epoch positions were taken directly from the GC, Cape
Astrographic, First and Second Cape Photographic, Yale Photographic, AGK2, AGK3
and a few smaller catalogues.  The positions in these catalogues were adjusted
to the FK4 system, where this had not already been done, and then to the FK5.
The systematic corrections (FK5-FK4) for the epoch of each catalogue were evaluated
from a routine kindly supplied by Heiner Schwan of the Astronomisches          
Rechen-Institut, and applied to the extracted star positions.  These systematic
corrections did not include the changes of position and rotation resulting from
the transformation to the 1976 IAU System.                                     
For the non-PPM stars the CAMC positions at equinox J2000.0 in the 1976 IAU 
system were transformed to the previous system at B1950.0 using the procedure 
given by Yallop\,\etal\,(1989).  The positions so derived at B1950.0 were 
adjusted to the epoch of observation by subtracting the proper motion resulting 
from the difference in rotation between the frames of reference in the 1976 IAU
system and the previous system.  The CAMC positions were thus referred to the  
same reference frame as the catalogues used in deriving the proper motions.    
Finally, these proper motions were transformed to the equinox J2000.0.

The revised proper motions for some stars were found to be discordant with 
those in the PPM. The positions of these stars were taken from the AGK2 and 
AGK3 and compared with the CMC5-9. In most cases the AGK3 position was found 
to be discrepant, and in a few cases where the Astrographic Catalogue position 
was also available, both the AGK2  and AGK3 positions were found to be 
discrepant. 

The second category of proper motion applied to stars fainter than V$\sim$11
for which only the AC could readily supply positions at previous epochs for the
bulk of these stars.  By courtesy of Siegfried R\"oser of the 
Astronomisches Rechen-Institut, Heidelberg, the AC first became available for 
CMC5 and CMC6, but only for the northern hemisphere. Both hemispheres were
available for CMC7-CMC9. These AC positions were in the system of the FK5.
For CMC10-CMC11 the AC\,2000 (Urban \etal, 1998) became available. This version of
the AC was referred to the system of the Hipparcos Catalogue. These positions
were used directly with CMC10-CMC11 which were also referred to the system
of the Hipparcos Catalogue. In general, each star has two or three independent
positions in the AC.
                                                                               
                                                                               
The catalogue positions were weighted according to their mean errors at epoch  
of observation.  A mean error of 0\pas3 in right ascension and declination was 
adopted for the Astrographic Catalogue. The mean errors for the other 
catalogues were taken directly from the published positions. The estimates of 
the mean errors of the CAMC positions were calculated from the expressions given 
in Table~\ref{errorc}.                                     
                                                                               
The mean errors of the proper motions were estimated from the weights assigned 
to the input positions. Comparison of the proper motions with provisional
values from the H{\sc ipparcos} results shows that these internal errors are
underestimated by about 50\%. So, whereas the average internal errors given in 
the catalogue lie in the range $\pm$0\pas002 to $\pm$0\pas003 per year, the 
average external errors lie in the range $\pm$0\pas003 to $\pm$0\pas004 per 
year.

The $\sim$21\,600 stars with no determination of proper motion fall into 
the following categories: (a) stars fainter than V$\sim$11 in CMC1-4 where 
the AC was not available, and in CMC5-6 south of the equator where, again, 
the AC was not available; (b) stars fainter than the limit of 
the AC for which no accurate first epoch positions were readily available.
                                                                               
For the reasons given above, the coverage and accuracy of the proper motions has
improved with time from CMC1-4 to CMC11. Thus, the proper motion
of a star in this compilation which has more than one entry is likely to be 
more accurate in the latest catalogue.

A comparison with stars common to the Hipparcos Catalogue, shows that
in proper motion the systematic errors lie mainly in the range 
$\pm$1.5\,mas\,yr$^{-1}$, with only a few small areas reaching 
$\pm$3.0\,mas\,yr$^{-1}$.

\section{Comparison with standard catalogues and ephemerides}\label{compara}   

\subsection{Hipparcos Catalogue}
The aim has been to obtain positions differentially with respect to the ICRF,
using the Hipparcos Catalogue as the realization of that frame in the optical
waveband. The adjustment of the observations and catalogues to the ICRF is
described in \S\,\ref{ICRF}. As a result of these procedures, the system of
this catalogue should be within 30\,mas of the ICRF at the epoch of the 
observations and for about ten years thereafter. Beyond that, systematic
errors of the proper motions will vitiate this accuracy.

Below --40\deg \space in declination, corresponding to a zenith distance of 
70\deg \space to the south, and similarly below the pole in the north, the 
CAMC system runs off uncontrollably from the ICRF in declination. This is 
probably due to errors in modelling  refraction at these low altitudes.  
For this reason the catalogue is limited to a declination of --40\deg, apart
from the FK5 stars observed during CMC1-9, which are given down to
a declination of --60\deg.

\subsection{JPL DE405, satellite and minor planet ephemerides}\label{jpl}
The observed positions of the major planets (referred to the ICRF) have 
been compared with the Jet Propulsion Laboratory Development Ephemerides 405 
(DE405) (Morrison \& Evans, 1998). The 
offsets of Ganymede and Callisto from Jupiter were calculated from the         
Connaissance des Temps (1985-1994) and those of Oberon from Uranus from the
Supplement to the CdT. (1990-1994). The ephemerides of the orbits of the      
satellites of Saturn were kindly supplied by D.B.\,Taylor (Taylor \& Shen, 
1988).

The opposition means of the observations discussed by Morrison \& Evans (1998)
generally lie within 0\pas05 of the ephemerides, except in the declination of
Jupiter (derived from the observations of Callisto and Ganymede), which shows
a fluctuation of amplitude 0\pas1 with the synodic period of Jupiter (12\,yr).
This looks like a frame--tie problem.  However, the most recent VLBI
observations of {\it Galileo} preclude this interpretation because they fit
very well to DE405.  The CAMC positions
of Uranus and Neptune, which were in the same region of the sky during the
observational period of this catalogue, show a coherent pattern relative to
DE405.  From this we conclude that there are systematic errors in the CAMC
observations which reach $\sim$0\pas1.
                                                                               
The minor planets were compared with ephemerides generated from recent         
integrations carried out by Annick Bec-Borsenberger, Bureau des Longitudes,    
Paris.  Again, the errors conform to those for a single observation
given in Table~\ref{errorz} and Table~\ref{errorm}.
The CAMC magnitudes of many of the minor planets have been analysed to
determine slope parameters and absolute magnitudes Piironen\,\etal\,(1996).

\subsection{Johnson $V$}\label{juanV}                                          
Since $B-V$ is generally not known for the stars in this catalogue, a value of 
$B-V =+0.5$ was adopted for ALL stars and Solar System objects when applying the
colour correction to the observed magnitude. This colour correction to the
magnitude changed with alterations to the filters and
micrometer over the period of this compilation. The colour correction was
derived for each catalogue by comparing the values in these catalogues with
photoelectric standards. The expressions for reducing the magnitudes published 
in this compilation catalogue to Johnson $V$ are:
$$ V_{\rm J} = V_{\rm CMC1-4} - 0.015 + [-0.071-0.011({\rm Year}-1984.0)]
                                                                   \,(B-V-0.5)$$
$$ V_{\rm J} = V_{\rm CMC5} - 0.022 + 0.036\,(B-V-0.5)$$
$$ V_{\rm J} = V_{\rm CMC6} - 0.005 + 0.036\,(B-V-0.5) \;\;{\rm (Jan\,3~to~
                                                                     Feb\,15)}$$
$$ V_{\rm J} = V_{\rm CMC6} - 0.005 + 0.018\,(B-V-0.5) \;\;{\rm (Feb\,16~to~ 
                                                                     Dec\,31)}$$
$$ V_{\rm J} = V_{\rm CMC7} - 0.011 + 0.018\,(B-V-0.5)$$
$$ V_{\rm J} = V_{\rm CMC8} + 0.018\,(B-V -0.5)$$
$$ V_{\rm J} = V_{\rm CMC9} + 0.018\,(B-V -0.5)$$
$$ V_{\rm J} = V_{\rm CMC10} - 0.010 + 0.013\,(B-V-0.5)$$
$$ V_{\rm J} = V_{\rm CMC11} + 0.002 + 0.024\,(B-V-0.5)$$

In CMC10 it was found that the neutral density
filters employed in the observation of brighter stars, as described in 
Table~\ref{filters}, were not quite linear. This was also found in CMC11.
Corrections to remove these non--linearities were applied in CMC10 and CMC11,
but not in the earlier catalogues in the series. The maximum systematic error
in CMC1-9 due to the neglect of this effect is +0.02~mag near V=2 and V=6. 

The periods covered by the catalogues are listed in Table~\ref{periods}.

\newpage
\section{Explanation and file formats}\label{explanation}
\subsection{Star Catalogue CMC1-11 -- decimal version -- {\it star1.dat}}

Record format -- 2 records per star (in ascending order of
right ascension, except for observations of the same star, where epoch of 
observation takes precedence).

\begin{center}
Record length = 80 char

\vspace{2mm}
\begin{tabular}{r|ll}
 \hline
Format  &              Quantity    & Unit \\
\hline
I7      & CMC serial number               & Volume$\times$100000+serial No.\\
I9      & RA (J2000.0, Epoch of date)     & $10^{-7}\,$hour \\
I9      & Dec(J2000.0, Epoch of date)     & $10^{-6}\,$degree \\
I4      & V magnitude (CAMC)\,$^a$        & $10^{-2}\,$mag \\
A1      & var.=V; approx.=Y or I; 12.=X or R& \\
I4      & Epoch of RA                     & $10^{-2}\,$year (--1900)\\
1X      &                                 &                          \\
I4      & Epoch of Dec                    & $10^{-2}\,$year (--1900)\\
3I2     & No. of obs. RA, Dec, Mag        &  \\
2F5.2   & Parallax factors in RA \& Dec   & \\
1X      &                                 & \\
I7,I6   & CAMC proper motion \& error RA  & $10^{-5}$ s/year  \\
        & Set to 999990 and 0 if not determined & \\
I6,I3   & CAMC proper motion \& error Dec & $10^{-4}$ \as/year  \\
        & Set to 999990 and 0 if not determined & \\
2X      &            & \\
\hline
A2      & Spectral type  & \\
I9      & DM=N$\times$10000000+Zone$\times$100000+Number & \\
        & N=$\pm$1: BD +89 to --22 deg   & \\
        & N=--2: CoD --23 to --45 deg      & \\
        & N=--3: CPD                      & \\
        & N=$\pm$4: DM assigned by CDS       & \\
I1      & DM double component number  & \\
I6      & SAO &\\
I6      & GC & \\
I8      & AGK & \\
I7      & HD &\\
A14     & WDS           & Final letter(s)\\
9X      &               & = comp$^{\rm n}$ obsd.\\
I10     & Internal CAMC number & \\
8X      &     & \\
\hline
\end{tabular}
\end{center}

{\footnotesize ~$^a$ Where the CAMC did not measure the mag, an approximate value
  from other sources is given to a precision of 0.1 mag (Y or I in next col.).
  Stars fainter than $\sim$12 with unknown mag are given as 12. (X or R in
  next col.).}

\newpage
\subsection{Star Catalogue CMC1-11 -- sexagesimal version -- 
                                           {\it star2.dat \& star2*.dat}}
\begin{explanation}                                                            
\item[Column 1:]              Serial number=volume$\times$100000 + serial 
                                               number+double comp$^n$.
                        
\item[Columns 2-4 \& 5-7:]    Right ascension (\hh\,\mm\,\ss) and declination 
                              (\deg\,\amin\,\as) for equinox J2000.0
                              and epoch of observation.
\item[Columns 8 \& 11:]       Number of observations in position
                              and magnitude.
\item[Column 9:]              Mean epoch of observation in right ascension and
                              declination.
\item[Column 10:]       Observed magnitude (V CAMC). No magnitude was         
                        determined for 7602 stars.  For these stars the
                        magnitude was either taken (to one decimal place) from
			an input catalogue or it was assigned a nominal
			magnitude of 12.  If the star is present in 
                        the General Catalogue of Variable Stars, the faintest 
                        observed magnitude is given, followed by a ``V''.     
                        The individual observed magnitudes for these stars
                        may be given in the file {\it varmag.dat}. 
\item[Columns 12 \& 13:] Annual proper motion in right ascension (s/yr) and 
                        declination (\as/yr) in the J2000.0 frame. A blank 
                        indicates that no position at an earlier epoch was 
                        found in the catalogues which were searched.  The proper
                        motion was derived independently for each entry of
                        the star (see \S\,\ref{pm}).       
\item[Column 14:]       DM number: BD +89 to --22 \& CD --23 to --45.        
                       A few exceptions to this rule south of the zone --22 
                       are marked by a C (Cordoba Durchmusterung) or a P    
                       (Cape Durchmusterung).  The digit immediately after  
                       the zone number is the component code. The minus sign
                       immediately after the degree zone indicates that the 
                       DM number has been assigned in the CSI.              
\end{explanation}                                                           

%\newpage
Record format -- 1 record per star (in ascending order
of right ascension, except for entries of the same star, where the epoch
of observation takes precedence.)

\begin{center}
Record length = 80 char

\vspace{2mm}
\begin{tabular}{r|ll}
 \hline
Format  &              Quantity    & Unit \\
\hline
I7            & CMC serial number & Volume$\times$100000+serial No.  \\
A3            & Double star component       &             \\
I2,I3,F7.3    & RA (J2000.0, Epoch of date) & h\,m\,s \\
1X            &                             &  \\
A1,I2,I3,F6.2 & Dec (J2000.0, Epoch of date)& \deg\,\amin\,\as \\
1X            &                             &   \\
I2            & Number of observations      & \\
1X            &                             &  \\
F5.2          & Epoch of observation        & year ($-$1900) \\
1X            &                             &   \\
A5            & V magnitude (CAMC)          & \\
A1            & V=var.                      & \\
I2            & No. of obs. in mag.         &  \\
F8.4          & CAMC proper motion in RA    & s/year (blank= no pm)\\
F7.3          & CAMC proper motion in Dec   & \as/year (blank= no pm) \\
1X            &                             &  \\
A11           & DM number                   & \\
\hline
\end{tabular}
\end{center}

\newpage
\subsection{CMC1-11 stars with $\mu>0\pass18$/yr -- mainly NLTT -- 
                                                      {\it nltt.dat}}
\begin{explanation}                                                            
\item[Column 1:]              Serial number=volume$\times$100000 + serial 
                                               number+double comp$^n$.
                        
\item[Columns 2-4 \& 5-7:]    Right ascension (\hh\,\mm\,\ss) and declination 
                              (\deg\,\amin\,\as) for equinox J2000.0
                              and epoch of observation.
\item[Columns 8 \& 11:]       Number of observations in position
                              and magnitude.
\item[Column 9:]              Mean epoch of observation in right ascension and
                              declination.
\item[Column 10:]       Observed magnitude (V CAMC). No magnitude was         
                        determined for some of the stars.  For these stars the
                        magnitude was either taken (to one decimal place) from
			an input catalogue or it was assigned a nominal 
			magnitude of 12.  If the star is present in 
                        the General Catalogue of Variable Stars, the faintest 
                        observed magnitude is given, followed by a ``V''.     
                        The individual observed magnitudes for these stars
			may be given in the file {\it varmag.dat}. 
\item[Columns 12 \& 13:] Annual proper motion in right ascension (s/yr) and 
                        declination (\as/yr) in the J2000.0 frame. The proper
                        motion was derived independently for each entry of
                        the star (see \S\,\ref{pm}).  Where the	proper motion 
			could not be calculated, because no position at an 
			earlier epoch was found in the catalogues which were 
			searched, the proper motion was taken from the NLTT. 
			These are indicated by an asterisk immediately
			following the proper motion in declination.
			
\item[Column 14:]       The star identification given in the NLTT. Where BD/CD
                        is not available, the following are used: Oxf=Oxford AC,
                        Grw=Greenwich AC, \\U=Upgren, R=Ross, L=Luyten No. in
			Bruce PM Survey, LP=Luyten-Palomar Survey. An asterisk
			indicates that a note is given in the NLTT ``notes''
			file.

                        ``Not NLTT'' means that the CAMC proper motion is
			greater than 0\pas179 per year, but the star was not
			found in the NLTT.  In many cases the true value of the
			proper motion is probably less than the 0\pas18 limit
			of the NLTT.
\end{explanation}                                                           

\newpage
Record format -- 1 record per star (in ascending order
of right ascension, except for entries of the same star, where the epoch of
observations takes precedence.)

\begin{center}
Record length = 84 char

\vspace{2mm}
\begin{tabular}{r|ll}
 \hline
Format  &              Quantity    & Unit \\
\hline
I7            & CMC serial number & Volume$\times$100000+serial No.  \\
A3            & Double star component       &             \\
I2,I3,F7.3    & RA (J2000.0, Epoch of date) & h\,m\,s \\
1X            &                             &  \\
A1,I2,I3,F6.2 & Dec (J2000.0, Epoch of date)& \deg\,\amin\,\as \\
1X            &                             &   \\
I2            & Number of observations      & \\
1X            &                             &  \\
F5.2          & Epoch of observation        & year ($-$1900) \\
1X            &                             &   \\
A5            & V magnitude (CAMC)          & \\
A1            & V=var.                      & \\
I2            & No. of obs. in mag.         &  \\
F8.4          & CAMC proper motion in RA    & s/year \\
F7.3          & CAMC proper motion in Dec   & \as/year \\
A1            & NLTT proper motion flag     &  \\
A15           & NLTT identifier             & \\
\hline
\end{tabular}
\end{center}

\newpage
\subsection{Variable stars in CMC1-11 -- {\it varpos.dat}}
\begin{explanation}                                                            
\item[Column 1:]              Serial number=volume$\times$100000 + serial 
                                               number+double comp$^n$.
                        
\item[Columns 2-4 \& 5-7:]    Right ascension (\hh\,\mm\,\ss) and declination 
                              (\deg\,\amin\,\as) for equinox J2000.0
                              and epoch of observation.
\item[Columns 8 \& 11:]       Number of observations in position
                              and magnitude.
\item[Column 9:]              Mean epoch of observation in right ascension and
                              declination.
\item[Column 10:]       Minimum observed magnitude (V CAMC).          
                        The individual observed magnitudes for these stars
			may be
                        given in the file {\it varmag.dat}. Note that the 
			number of observations of magnitude (col.11) is the 
			number of consistent observations used in forming the 
			mean magnitude. Since these stars are variable, the 
			number of observations may be given as zero, when in 
			fact there are observations in {\it varmag.dat}. Where 
			no observations of magnitude were made, the magnitude 
			was either taken (to one decimal place) from an input 
			catalogue or it was assigned a nominal magnitude of 12.
			Note also that nights with just a few clouds were
			not normally flagged as non-photometric, so some false
			faint magnitudes could be expected.
\item[Columns 12 \& 13:] Annual proper motion in right ascension (s/yr) and 
                        declination (\as/yr) in the J2000.0 frame. A blank 
                        indicates that no position at an earlier epoch was 
                        found in the catalogues which were searched.  The proper
                        motion was derived independently for each entry of
                        the star (see \S\,\ref{pm}).       
\item[Column 14:]       GCVS identifier.
\end{explanation}                                                           

\newpage
Record format -- 1 record per star (in ascending order of right ascension, except
for entries of the same star, where the epoch of observation takes precedence.)

\begin{center}
Record length = 80 char

\vspace{2mm}
\begin{tabular}{r|ll}
 \hline
Format  &              Quantity    & Unit \\
\hline
I7            & CMC serial number & Volume$\times$100000+serial No.  \\
A3            & Double star component       &             \\
I2,I3,F7.3    & RA (J2000.0, Epoch of date) & h\,m\,s \\
1X            &                             &  \\
A1,I2,I3,F6.2 & Dec (J2000.0, Epoch of date)& \deg\,\amin\,\as \\
1X            &                             &   \\
I2            & Number of observations      & \\
1X            &                             &  \\
F5.2          & Epoch of observation        & year ($-$1900) \\
1X            &                             &   \\
A5            & V magnitude (CAMC)          & \\
A1            & V=var.                      & \\
I2            & No. of obs. in mag.         &  \\
F8.4          & CAMC proper motion in RA    & s/year (blank= no pm)\\
F7.3          & CAMC proper motion in Dec   & \as/year (blank= no pm)\\
1X            &                             &  \\
A11           & GCVS identifier             & \\
\hline
\end{tabular}
\end{center}

\newpage
\subsection{Positions of nov\ae~and supernov\ae~in CMC1-11 -- {\it novapos.dat}}
\begin{explanation}                                                            
\item[Column 1:]              Serial number=volume$\times$100000 + serial 
                                               number+double comp$^n$.
                        
\item[Columns 2-4 \& 5-7:]    Right ascension (\hh\,\mm\,\ss) and declination 
                              (\deg\,\amin\,\as) for equinox J2000.0
                              and epoch of observation.
\item[Columns 8 \& 11:]       Number of observations in position
                              and magnitude.
\item[Column 9:]              Mean epoch of observation in right ascension and
                              declination.
\item[Column 10:]       Minimum observed magnitude (V CAMC).          
                        The individual observed magnitudes for these stars are
                        given in the file {\it novamag.dat}. 
\item[Columns 12 \& 13:] (Annual proper motion -- blank)
\item[Column 14:]       Nova/Supernova identifier.
\end{explanation}                                                           

Record format -- 1 record per star (in ascending order of right ascension)

\begin{center}
Record length = 80 char

\vspace{2mm}
\begin{tabular}{r|ll}
 \hline
Format  &              Quantity    & Unit \\
\hline
I7            & CMC serial number & Volume$\times$100000+serial No.  \\
A3            & Double star component       &             \\
I2,I3,F7.3    & RA (J2000.0, Epoch of date) & h\,m\,s \\
1X            &                             &  \\
A1,I2,I3,F6.2 & Dec (J2000.0, Epoch of date)& \deg\,\amin\,\as \\
1X            &                             &   \\
I2            & Number of observations      & \\
1X            &                             &  \\
F5.2          & Epoch of observation        & year ($-$1900) \\
1X            &                             &   \\
A5            & V magnitude (CAMC)          & \\
A1            & V=var.                      & \\
I2            & No. of obs. in mag.         &  \\
16X           &                             & \\
A11           & N/SN identifier             & \\
\hline
\end{tabular}
\end{center}

\newpage
\subsection{Reference stars in CMC1-11, 10$<$V$<$14, within 20\,\amin~of 
Veron-Cetty galaxy positions -- {\it veronc81.dat, veronc82.dat, veronc83.dat}}

{\it veronc81.dat}: Quasars (brighter than  absolute magnitude $-23$).\\
{\it veronc82.dat}: Confirmed, probable or possible BL Lac objects.\\
{\it veronc83.dat}: Active Galaxies (fainter than absolute magnitude $-23$).\\

\begin{explanation}                                                            
\item[Column 1:]              Serial number=volume$\times$100000 + serial 
                                               number+double comp$^n$.
                        
\item[Columns 2-4 \& 5-7:]    Right ascension (\hh\,\mm\,\ss) and declination 
                              (\deg\,\amin\,\as) for equinox J2000.0
                              and epoch of observation.
\item[Columns 8 \& 11:]       Number of observations in position
                              and magnitude.
\item[Column 9:]              Mean epoch of observation in right ascension and
                              declination.
\item[Column 10:]       Observed magnitude (V CAMC). Where no magnitude was
                        determined for stars, the magnitude was either taken 
			(to one decimal place) from an input catalogue or it 
			was assigned a nominal magnitude of 12.  If the star 
			is present in the General Catalogue of Variable Stars, 
			the faintest observed magnitude is given, followed by 
			a ``V''. The individual observed magnitudes for these 
			stars may be given in the file {\it varmag.dat}. 
\item[Columns 12 \& 13:] Annual proper motion in right ascension (s/yr) and 
                        declination (\as/yr) in the J2000.0 frame. A blank 
                        indicates that no position at an earlier epoch was 
                        found in the catalogues which were searched.  The proper
                        motion was derived independently for each entry of
                        the star (see \S\,\ref{pm}).       
\item[Columns 14 \& 15:] RA and Dec offsets in arc min of the CAMC star 
                         position from the galaxy, in the sense
			 CAMC {\it minus} Veron-Cetty.
%\item[Column 16:]       Identifier of galaxy in Veron-Cetty.
\item[Column 16:]       Identifier of galaxy in Veron-Cetty \& Veron (1998). 
\end{explanation}                                                           

\newpage
Record format -- 1 record per star (in ascending order of right 
ascension of galaxy, and right ascension of star within entries for a galaxy).

\begin{center}
Record length = 96 char

\vspace{2mm}
\begin{tabular}{r|ll}
 \hline
Format  &              Quantity    & Unit \\
\hline
I7            & CMC serial number & Volume$\times$100000+serial No.  \\
A3            & Double star component       &             \\
I2,I3,F7.3    & RA (J2000.0, Epoch of date) & h\,m\,s \\
1X            &                             &  \\
A1,I2,I3,F6.2 & Dec (J2000.0, Epoch of date)& \deg\,\amin\,\as \\
1X            &                             &   \\
I2            & Number of observations      & \\
1X            &                             &  \\
F5.2          & Epoch of observation        & year ($-$1900) \\
1X            &                             &   \\
A5            & V magnitude (CAMC)          & \\
A1            & V=var.                      & \\
I2            & No. of obs. in mag.         &  \\
F8.4          & CAMC proper motion in RA    & s/year (blank= no pm)\\
F7.3          & CAMC proper motion in Dec   & \as/year (blank= no pm) \\
I4            & Offset in RA                & \amin \\       
I4            & Offset in Dec               & \amin \\
1X            &                             &  \\
A19           & Galaxy identifier           & \\
\hline
\end{tabular}
\end{center}

\newpage
\subsection{Observed positions of FK5 stars - {\it fk5u.dat \& fk5l.dat}}
Two files contain 12\,216 mean observed positions of the FK5 stars used nightly
to transfer the instrumental system of CMC1-9 to the FK5. The circumpolar stars
were observed at upper and lower culminations and these are given in two
separate files: upper - 11365 positions; lower - 851 positions.

The system defined by these positions is that of the original versions of
CMC1-9, before they were adjusted to the ICRF, as described in \S\,\ref{ICRF}.
The system was not exactly that of the FK5, as explained in \S\,\ref{nightly}, 
\S\,\ref{zonal} and \S\,\ref{ICRF}. In each year about 20 observations were 
made on the average of each FK5 star. The accuracy of these annual mean 
positions can be calculated from the expressions in Table\,\ref{errorc}. They 
tend towards the asymptotic errors of 0\pas035 and 0\pas049 found by 
Morrison\,\etal\,(1990). 

Format of FK5 star files (upper and lower culminations, in ascending order
of right ascension)

\begin{center}
Record length = 55 char

\vspace{2mm}
\begin{tabular}{r|ll}
 \hline
Format  &              Quantity   & Unit \\
\hline
I7      & CMC serial number & Volume$\times$100000+FK5$\times$10
                                                         +comp$^{\rm n}$\\
I9      & RA (J2000.0, Epoch of date) & $10^{-7}\,$hour \\
I9      & Dec(J2000.0, Epoch of date) & $10^{-6}\,$degree \\
I4      & V magnitude (CAMC)          & $10^{-2}\,$mag \\
A1      & V=var.                      & \\
I4      & Epoch of RA                 & $10^{-2}\,$year (--1900)\\
1X      &                             &                          \\
I4      & Epoch of Dec                & $10^{-2}\,$year (--1900)\\
3I2     & No. of obs. RA, Dec, Mag    &  \\
2F5.2   & Parallax factors in RA \& Dec & \\
\hline
\end{tabular}
\end{center}

\vspace{1cm}
\subsection{Observed magnitudes of variable stars -- {\it varmag.dat}}

The individual magnitudes of stars that are known to be variable are listed
in file {\it varmag.dat}. The FK5 variables are included in this list.

Format of variable star file (in alphabetical order of constellation, star name
and Julian Date within star entries.

\begin{center}
Record length = 40 char

\vspace{2mm}
\begin{tabular}{r|l}
 \hline
Format  &              Quantity    \\
\hline
   I8  &   CMC number = Volume$\times$100000+serial number \\
       &   or FK5 number\\
   1X  &        \\
  A11  &   Variable star name \\
   1X  &        \\
 F12.4 &  Julian Date of observation \\
   2X  &          \\
  F5.2 &  Observed magnitude (V CAMC) \\   
\hline
\end{tabular}
\end{center}

\newpage
\subsection{Observed magnitudes of nov\ae~and supernov\ae~-- {\it novamag.dat}}

The magnitudes of 12 nov\ae~and 8 supernov\ae~observed in the years 
1991 to 1998 are given in the file {\it novamag.dat}.

Format of record (in order of discovery year)

\begin{center}
Record length = 45 char

\vspace{2mm}
\begin{tabular}{r|l}
 \hline
Format  &              Quantity    \\
\hline
   I8  &   CMC number = Volume$\times$100000+serial number \\
   2X  &        \\
  A15  &   Nova/Supernova name \\
   1X  &        \\
 F12.4 &  Julian Date of observation \\
   1X  &                \\
  F6.2 &  Observed magnitude (V CAMC) \\
\hline
\end{tabular}
\end{center}

\subsection{Observed magnitudes of suspected variables -- {\it suspect.dat}}

The magnitudes of a few stars were observed for suspected variability.
The magnitudes are listed in the file {\it suspect.dat}.

Format of record (in order of right ascension and Julian Date within star
entries)

\begin{center}
Record length = 45 char

\vspace{2mm}
\begin{tabular}{r|l}
 \hline
Format  &              Quantity    \\
\hline
   I8  &   CMC number = Volume$\times$100000+serial number \\
   2X  &        \\
  A15  &   Star identification \\
   1X  &        \\
 F12.4 &  Julian Date of observation \\
   1X  &                \\
  F6.2 &  Observed magnitude (V CAMC) \\
\hline
\end{tabular}
\end{center}

\newpage
\subsection{Observations of planets, satellites and minor planets -- {\it
planet.dat}}

Format of planet record 

\begin{center}
Record length = 83 char

\vspace{2mm}
\begin{tabular}{r|l}
 \hline
Format  &              Quantity    \\
\hline
   1X  &       \\
   I7  &   CAMC object code    \\
   4X  &        \\
   A4  &   Minor planet number or blank \\
   2X  &        \\
  A12  &   Planet, satellite or minor planet name  \\
   2X  &        \\
 F14.6 &  Julian Date(TT)$^a$ where TT = UT1 + (TAI--UT1) + 32\ps184    \\
       &  UT1 = time of transit; TAI--UT1 is taken by interpolation\\
       &  from 5--day values published by the Bureau Central de \\
       &  l'IERS, Observatoire de Paris\\
   A1  &  An * indicates an observation with an internal error \\
       &  greater than 0\pas75 and less than 1\pas15        \\
   2X  &          \\
2I3,F7.3&  Apparent geocentric$^b$ RA (h\,m\,s) for equinox of date, \\
       &   referred to the 1976 IAU reference system \\
   2X  &          \\
A1,I2,I3,F6.2& Apparent geocentric$^b$ Declination (\deg\,\amin\,\as) for equinox\\
       &   of date, referred to the 1976 IAU reference system \\
   2X  &           \\
   F5.2&   Observed magnitude (V CAMC) or blank   \\   
\hline
\end{tabular}
\end{center}

$^a$ The time argument in the printed volumes of CMC1-3 is TAI, and not TDT as
stated.

$^b$ Except Geographos, which is topocentric.

\newpage
\subsection{Meteorological data -- {\it *.met}}

The Carlsberg Automatic Meridian Circle carried out regular meteorological
observations in the period 13~May 1984 to 27~May~1998 and the records 
are more or less continuous in that period. The devices used to measure
temperature, pressure, humidity, wind speed and direction are as follows:
\begin{list}{}{}
\item{\bf Temperature}\\
     Analog Devices AD590K\\
     Range: --55$^\circ$ C to +150$^\circ$ C\\
     Calibrated accuracy: 0.1$^\circ$ C\\
     Situation: mast head; 6 metres above ground until 1991 May 16,\\
     then 10.5  metres above ground
\item{\bf Pressure}\\
     Ysi Sostman, 2014--19.2/25.7 HA--3--WH aneroid type\\
     barometer\\
     Range: 650--870 mb\\
     Resolution: 0.1 mm Hg\\
     Hysteresis: $\le$0.1 mm Hg\\
     Situation: inside telescope enclosure (started 1 August 1984)
\item{\bf Humidity}\\
     Lambrecht KG, type 800 N 100 hair hygrometer\\
     Range: 0--100$\%$ relative humidity\\
     Resolution: 2$\%$\\
     Situation: inside the telescope enclosure until 1987 October 17\\
     ~~~~~~when it was moved to the outside north--facing wall of\\
     ~~~~~~the telescope enclosure
\item{\bf Wind speed}\\
     From 1984 May:
      \begin{list}{}{}
      \item{} Malling, system 881.01 and 875 anemometer\\
            Range: 0--30 m/s\\
            Accuracy: 1 m/s
      \end{list}
     From 1988 January:
      \begin{list}{}{}
      \item{} Vaisala WAA 12 anemometer\\
            Range: 0--75 m/s\\
            Accuracy: $\pm$ 1$\%$ below 20 m/s;~~ $\pm$ 2$\%$ above 20 m/s
      \end{list}      
    Situation: mast head; 6 metres above ground until 1991 May 16,\\
            ~~~~~~then 10.5  metres above ground\\
    {NB: Until December 1994, wind speed averaged over several\\ 
            ~~~~~~seconds and therefore insensitive to sudden gusts}
\item{\bf Wind direction}\\
     Aanderaa, model 2053 (vane type)\\
     Range: 0$^\circ$ -- 360$^\circ$\\ 
     Accuracy: 5$^\circ$ \\
     Situation: mast head; 6 metres above ground until 1991 May 16,
     then 10.5  metres above ground
\end{list}

For the years 1984, 1985 and 1986 meteorological readings are only available 
at 30 minute intervals. From 1987 January, the meteorological sensors were 
read automatically by a dedicated Olivetti PC. Readings were then made at 
5~minute intervals throughout the day and night regardless of whether observing 
was in progress. Beginning in 1994 December, all readings were made at 20\,s 
intervals and then averaged over 5~minutes. The 5-min averages of wind velocity 
are thus less prone to erratic fluctuations caused by gusts than single 
readings at 5~minute intervals.

No readings were available when any one of the computers was ``down'', or a 
sensor became faulty, or during periods of routine maintenance or when the 
telescope was being modified -- for example when fitting the new micrometer or
the new circle reading system etc. In particular, there are no meteorological
data for the following periods: 
\begin{list}{}{}
\item{}1984 September 25 to October 8: data were inadvertently deleted
                                                from the computer file
\item{}1985 December 9 to December 31: technical fault
\item{}1986 January 1 to January 11: telescope out of operation due to 
                                                         technical fault
\item{}1986 March: no wind direction data because the transducer was broken
                                                          by heavy icing
\item{}1986 September 12 to September 22: telescope out of action due to
                                                         technical fault
\item{}1986 December 18 to December 31: telescope was closed down for this 
                                                                    period
\item{}1988 February: breaks in the data due to the fitting of the new 
                                                               micrometer
\item{}1988 May to August 10: no wind direction values between north and
              north--east because direction indicator was faulty
\item{}1994 January: gaps in the data because some of the sensors broke free
            from the top of the meteorological mast due to severe 
                                                  icing and strong winds
\item{}1995 April: gaps in the meteorological data because a new telescope
            control system was installed and operation was restricted
\item{}1995 September 14 to 1995 November 16: no wind direction values due 
            to a fault in the wind direction device
\item{}1995 November 16 to 1996 March 7: A/D converter produced `noisy'
                                                             background.
\end{list}

\newpage
The meteorological data are given in 26 six-monthly files. The number of records
in each file is as follows:

\begin{center}
\begin{tabular}{lr}
1984~Jun--Dec & 3541 \\
1985~Jan--Dec & 5974 \\
1986~Jan--Dec & 7285 \\
1987~Jan--Jun & 47349 \\
1987~Jul--Dec & 45810 \\
1988~Jan--Jun & 50637 \\
1988~Jul--Dec & 46556 \\
1989~Jan--Jun & 50672 \\
1989~Jul--Dec & 51706 \\
1990~Jan--Jun & 51974 \\
1990~Jul--Dec & 49363 \\
1991~Jan--Jun & 50008 \\
1991~Jul--Dec & 49571 \\
1992~Jan--Jun & 51884 \\
1992~Jul--Dec & 51606 \\
1993~Jan--Jun & 50622 \\
1993~Jul--Dec & 52740 \\
1994~Jan--Jun & 50640 \\
1994~Jul--Dec & 51173 \\
1995~Jan--Jun & 49121 \\
1995~Jul--Dec & 53010 \\
1996~Jan--Jun & 50989 \\
1996~Jul--Dec & 49001 \\
1997~Jan--Jun & 50548 \\
1997~Jul--Dec & 51899 \\
1998~Jan--May & 42033 \\
\end{tabular}
\end{center}

\newpage
Format of meteorological data record

\begin{center}
Record length = 60 char

\vspace{2mm}
\begin{tabular}{r|l}
 \hline
Format  &              Quantity    \\
\hline
    1X     &     \\
    I4      &     Year    \\
    1X      &        \\
    I2      &     Month       \\
    1X      &         \\
    I2      &     Day     \\
    1X      &         \\
    I2      &     Hours~~UT     \\
    1X      &         \\
    I2      &     Minutes~~UT    \\
    1X      &         \\
    I2      &     Seconds~~UT    \\
    2X      &         \\
  F5.1     &     Pressure in millibars   \\
    2X       &         \\
  F6.1     &     Outdoor temperature in $^\circ$C   \\
    2X      &         \\
    I2      &     Wind speed in metres/second     \\
    1X      &         \\
    I3      &     Wind direction: North is 0$^\circ$; East is 90$^\circ$    \\
    1X      &         \\
    I3      &    Percentage relative humidity: measured inside the dome until\\ 
            &    17 October 1987; outdoors thereafter \\
    1X      &         \\
  F6.1     &     Temperature inside the dome in $^\circ$C     \\
    1X      &         \\
   5I1      &     Acceptance flags for pressure, temperature, humidity,    \\
            &     wind speed and wind direction:     \\
            &     ~~~~~if 0 -- reading ignored      \\
            &     ~~~~~if 1 -- reading accepted     \\
            &     ~~~~~if temperature flag set to 2, then temperature is     \\
            &     ~~~~~the indoor temperature as the outside value was     \\
            &     ~~~~~unacceptable        \\
            &     ~~~~~Inside temperature and acceptance flags are not available \\
            &     ~~~~~for the period June 1984 to December 1986.     \\     
\hline
\end{tabular}
\end{center}

\newpage
\subsection{Atmospheric extinction in Johnson V -- {\it ext8498.dat}}

The extinction in Johnson V was determined nightly from the photoelectric 
registration of standard stars. The parameters used in determining the 
nightly extinction were as follows:
\begin{list}{}{}
\item{} Extinction: coefficient of sec(zd) determined by least--squares 
  adjustment to calibration stars observed during the course of 
  a night: the equation of condition also includes a constant term for
  the zeropoint of the instrumental system -- see \S\ref{nightly} 
\item{} Spectral band: Johnson V
\item{} Calibration stars: CMC1-9 Nicolet (1978); CMC10-11 (Hipparcos)
\item{} Magnitude range:
     \begin{list}{}{}
     \item{} $2<{\rm m}_{v}<7$ from 1984 May to 1990 January
     \item{} $2<{\rm m}_{v}<14$ from 1990 January
     \end{list}
\item{} Zenith distance: down to 83\deg~N and S
\item{} Number of stars per night: $\sim$50, but ranges between 20 and 80
           until CMC11, when it increased to $\sim$200\\
\end{list}

Apart from gaps due to non-photometric nights, there are gaps in the extinction
values due to other causes in the following periods:
\begin{list}{}{}
\item{} 1988 February: fitting of the new micrometer and photo-multiplier\\
        1989 November to 1990 January: prolonged poor weather and technical 
                                                                  problems\\
        1992 August: installation of a new circle reading system\\
        1993 July: computer fault preventing observation
\end{list}

The eruption of the volcano, Mount Pinatubo in the Philippine Islands, in 1991
June produced up to 0.1 magnitudes of extinction between 1991 September and
the beginning of 1993 when its influence declined.

The extinction values and their hourly rate of change (where significant)
for the period 1984 May to 1998 May are listed in file {\it ext8498.dat}.

\newpage
Format and description of the extinction data record

\begin{center}
Record length = 61 char

\begin{tabular}{r|l}
\hline
Format  &  Unit  \\
\hline
  1X   &         \\
  I4   &  Year   \\
  1X   &         \\
  I2   &  Month  \\
  1X   &         \\
  I2   &  Day    \\
  2X   &         \\
  I2   &  Hours UT  \\
  1X   &         \\
  I2   &  Minutes UT \\
  5X   &         \\
  F4.2 &  Extinction in V (mag)   \\
  6X   &         \\
  F5.3 &  Extinction mean error   \\
  3X   &         \\
  F6.3 &  Hourly rate of change of extinction  \\
  3X   &         \\
  F5.3 &  Mean error of rate of change  \\
  3X   &         \\
  I3   &  Number of stars in solution\\
\hline
\end{tabular}
\end{center}

\newpage
\section*{Acknowledgements}\label{ack}                                          
The CAMC is operated under an international agreement between Denmark, Britain 
and Spain on the island of La Palma by Copenhagen University Observatory, Royal
Greenwich Observatory{\footnote {On the dissolution of the RGO in October 1998,
the staff in the CAMC project were transferred to the Institute of Astronomy,
Cambridge, where they continued to be funded by the Particle Physics \&
Astronomy Research Council.}}
and the Real Instituto y Observatorio de la Armada in the
Spanish Observatorio del Roque de los Muchachos of the Instituto de            
Astrof\'{\i}sica de Canarias.                                                  
                                                                               
We thank the Danish Natural Science Research Council for covering the travel   
expenses of Danish observers and for funding the development of a prototype    
CCD camera for the circle reading.                                             
                                                                               
We wish to thank the Carlsberg Foundation for paying the construction and      
installation of the CCD circle reading cameras (Project 90-0676/40).           
                                                                               
The RGO personnel are funded by the Particle Physics \& Astronomy Research     
Council of the United Kingdom.                                                 
                                                                               
We thank the Spanish Navy for its cooperation in the project through the Real  
Instituto y Observatorio de la Armada and the Direcci\'on General de           
Investigaci\'on Cient\'{\i}fica y T\'ecnica for their support (Proyecto 
PB90-039, PB94-1283).
                                                                               
The Centre de Donn\'ees Astronomiques de Strasbourg supplied the Catalogue of  
Stellar Identifications and some of the astrometric catalogues which were used 
in cross-referencing and in calculating the proper motions.                    
                                                                               
Prior to 1996 Siegfried R\"oser of the Astronomisches Rechen-Institut in Heidelberg          
supplied the positions of stars in the Astrographic Catalogue. The positions   
in the Astrographic Catalogue in the southern sky was made possible through    
the key-punched version kindly made available by the Sternberg Institute,      
Moscow.                                                                        
                                                                               
Annick Bec-Borsenberger of the Bureau des Lon\-gi\-tu\-des, Paris, kindly      
supplied the ephe\-me\-ri\-des for the minor planets. Since 1997 the
ephemerides of Solar System objects have been obtained from the JPL
{\it Horizons On--Line Ephemeris System} {\tt
http://ssd.jpl.nasa.gov/cgi-bin/eph} interface at their Web site.
                                                                               
We also wish to express our gratitude to the Instituto de Astrof\'{\i}sica de  
Canarias for the assistance given to the project.                              
                                                                               
\newpage                                                                       
\begin{thebibliography}{99}                                                    
\bibitem{1}  
   Argyle, R.W., Einicke, O.H., Pilkington, J.D.H., Morrison, L.V.,
   Jones, D.H.P.,
   Fabricius, C. \& Helmer, L. 1996. {\sl Comparison of the Carlsberg optical
   reference frame with the International celestial reference frame.}
   A\&A, {\bf 312}, 1031.
\bibitem{2}{\sl Carlsberg Meridian Catalogue La Palma No. 4.
  Observations of positions of stars and planets: May 1984 to February 1988}.
  (CMC4), 1989. Copenhagen University Observatory, Royal Greenwich Observatory
  and Real Instituto y Observatorio de la Armada en San Fernando.
\bibitem{3}
  {\sl Carlsberg Meridian Catalogue La Palma No. 5.
  Observations of positions of stars and planets: May 1988 to December 1989}.
   (CMC5), 1991. Copenhagen University Observatory, Royal Greenwich Observatory
  and Real Instituto y Observatorio de la Armada en San Fernando.
\bibitem{4}
   {\sl Carlsberg Meridian Catalogue La Palma No. 6.
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\end{thebibliography}
\end{document}
