\def\section#1{\\ \\ Section: #1} \def\subsection#1{\\ \\ subSection: #1} \def\subsubsection#1{\\ \\ subsubSection: #1} %Return-Path: guarinos@scsun.unige.ch %X400-Received: by mta chx400.switch.ch in /PRMD=switch/ADMD=arcom/C=CH/; % Relayed; Mon, 29 Nov 1993 09:19:40 +0100 %X400-Received: by /PRMD=SWITCH/ADMD=ARCOM/C=CH/; Relayed; % Mon, 29 Nov 1993 09:19:23 +0100 %X400-Received: by /PRMD=switch/ADMD=arcom/C=ch/; Relayed; % Mon, 29 Nov 1993 09:19:17 +0100 %Date: Mon, 29 Nov 1993 09:19:17 +0100 %X400-Originator: guarinos@scsun.unige.ch %X400-Recipients: francois@SIMBAD.u-strasbg.fr %X400-Mts-Identifier: [/PRMD=switch/ADMD=arcom/C=ch/;931129091917] %X400-Content-Type: P2-1984 (2) %Content-Identifier: 171 %From: GUARINOS Jacques %Message-Id: <171*/S=guarinos/OU=scsun/O=unige/PRMD=switch/ADMD=arcom/C=ch/@MHS> %To: francois@SIMBAD %In-Reply-To: <9311231254.AA18940@SIMBAD.u-strasbg.fr> %Subject: Re: Tes catalogues %Status: O % %\documentstyle{laamt} % LaTeX A&A Monotype Times Fonts \documentstyle{l-aa} % LaTeX A&A Standard Fonts %\documentstyle[referee,supertab]{l-aa} %\documentstyle[referee,supertab]{laamt} %\documentstyle{laalaanew_ref} % november 1991 %______________________________________ own macros % %______________________________________ might be important for figures %\renewcommand{\topfraction}{1} %\renewcommand{\bottomfraction}{1} %\renewcommand{\textfraction}{0} %______________________________________ general macros not defined in laamt \def\Msun{${\rm M}_\odot$~} \def\Msunit{$M_{\odot}$~} \def\M{$\dot{\rm M}$ ~} \def\Mit{$\dot M $ ~} \def\Rsun{${\rm R}_\odot$\ } \def\Msun{${\rm M}_\odot$\ } \def\Msunit{$M_{\odot}$~} \def\Lsun{${\rm L}_\odot$\ } \def\sun{$_\odot$ ~} \def\ssun{$\scriptstyle \odot$\ } \def\te{T$_{\rm eff}$~} \def\teit{$T_{eff}$~} \def\kms{$\!$km s$^{-1}$\ } \def\micron{$\mu$m~} \def\pr{$^{\prime}$~} %______________________________________ small symbols \def\sgeq{$\scriptstyle \geq$~} \def\sleq{$\scriptstyle \leq$~} \def\scong{$\scriptstyle \cong$~} \def\ssimeq{$\scriptstyle \simeq$~} \def\spm{$\scriptstyle \pm$~} %______________________________________ negative space \def\spa{$\!$~} %______________________________________ space in supertabular \def\tbsp{\rule{0pt}{3ex}} \def\tbsq{\rule[-0.5ex]{0pt}{3ex}} \newcommand{\AR}{{ARA\&A}~} \newcommand{\Afz}{{Afz}~ } \newcommand{\AJ}{{AJ}~ } \newcommand{\AZh}{{AZh}~} \newcommand{\AS}{{A\&A}~ } \newcommand{\AAS}{{A\&AS}~ } \newcommand{\AAR}{{A\&AR}~ } \newcommand{\ApJ}{{ApJ}~} \newcommand{\ApJS}{{ApJS}~} \newcommand{\ApSS}{{Ap\&SS}~} \newcommand{\BAAS}{{BAAS}~} \newcommand{\JAA}{{JA\&A}~} \newcommand{\MRAS}{{MNRAS}~} \newcommand{\Nat}{{Nat}~} \newcommand{\PASJ}{{PASJ}~} \newcommand{\PASP}{{PASP}~} \newcommand{\PASPC}{{PASPC}~} \newcommand{\QJRAS}{{QJRAS}~} \newcommand{\Sci}{{Sci}~} \newcommand{\SvA}{{SvA}~} \newcommand{\Acta}{{Acta astr.}~} \newcommand{\ActaS}{{Acta Astr. Sin.}~} \newcommand{\Ark}{{Ark. Astr.}~} \newcommand{\AstrN}{{Astr. Nachr.}~} \newcommand{\Austr}{{Austr. J. Phys.}~} \newcommand{\AustrS}{{Austr. J. Astrophys. Suppl.}~} \newcommand{\Chin}{{Chin. Astr.}~} \newcommand{\Comp}{{C.r. Acad. Sci. Paris}~} \newcommand{\IAUC}{{IAU Circ.}~} \newcommand{\Icarus}{{Icarus}~} \newcommand{\Irish}{{Irish astr. J.}~} \newcommand{\JRSC}{{J.R. astr. Soc. Can.}~} \newcommand{\MemR}{{Mem. R. astr. Soc.}~} \newcommand{\MemSocit}{{Mem. Soc. astr. ital.}~} \newcommand{\Mitt}{{Mitt. astr. Ges.}~} \newcommand{\Monafr}{{Mon. Notes astr. Soc. Sth. Afr.}~} \newcommand{\Obs}{{Observatory}~} \newcommand{\Philtrans}{{Phil. Trans. R. Soc. Lond. A}~} \newcommand{\ProcA}{{Proc. astr. Soc. Austr.}~} \newcommand{\RevMex}{{Rev. Mex. astr. astrofis.}~} \newcommand{\Vatic}{{Ric. astr. Specola astr. Vatic.}~} \newcommand{\ScAm}{{Scient. Am.}~} \newcommand{\Sky}{{Sky Telesc.}~} \newcommand{\SpcR}{{Space Sci. Rev.}~} %______________________________________ end personnal macros % comment title...... \begin{document} \thesaurus{} \title{Distribution of interstellar matter in the galactic disk from visual extinction data} \subtitle{I. The catalogue of extinctions and distances} \author{J. Guarinos \inst{} } \offprints{} \institute{} \date{Received date, accepted date} \maketitle \begin{abstract} %______________________________________ Do not leave a blank line here! % % date %_____________________________________ Do not leave a blank line here! As a preliminary step towards a new study of the interstellar medium in the solar vicinity from visual interstellar extinction data, we built a large catalogue of stars with estimated visual extinction $A_{V}$ and distance, using reliable UBV data and MK types. Before this, we discarded the stars with wrong spectral classifications, the binary stars, the metal deficient stars, the variable stars and the chemically peculiar ones. While building the catalogue, a special attention was paid to the consistency between the spectroscopic and photometric data. The program designed for computing extinctions and distances is described in details in the corresponding paper (Astron. Astrophys. Suppl. Ser., submitted). For each star, this program performs a choice of the "best" MK type and the assignment of an absolute magnitude and of an intrinsic colour. All the observed data and derived parameters of the selected stars as well as of some of the discarded ones were put in computer-readable files which are distributed by the Centre de Donn\'ees astronomiques de Strasbourg (CDS). From more than 160\,000 objects with an MK type and about 90\,000 ones with UBV data, only 16\,300 stars remain in the final list, among which, 15449 stars have distances not larger than 3000 pc. These are the stars of the two files of our catalogue. The latter is much more homogeneous in spectral types than the catalogues previously used for drawing maps of the interstellar matter, especially regarding the repartition between O/B and A/F stars, allowing a more uniform spatial distribution of the sample of stars in the galactic disc near the Sun. \keywords{stars: distances -- stars: fundamental parameters -- dust, extinction -- solar neighbourhood -- catalogs} \end{abstract} % 14.Sep.'90: Demo-Vs. %________________________________________________________________ \section{Construction of a catalogue of interstellar extinctions and stellar distances} \subsection{Data sources} The V magnitudes and the $(B-V)$ and $(U-B)$ colour indices were given by the compilation of Mermilliod (1987). It contains 136\,700 entries, concerning 87\,300 stars. Each star may have several measurements of the V magnitude or of one or both of the colour indices. \par The MK types were provided by several catalogues. The most important in volume is the {\it University of Michigan Catalogue of Two-Dimensional Spectral Types for the HD Stars} (Houk \& Cowley 1975; Houk 1978; Houk 1982; Houk \& Smith-Moore 1988). It contains the MK types of 130\,400 southern stars. All the visual spectral classifications were performed by Houk, which makes this catalogue the most homogeneous available now. We discarded the spectral classifications inferred from under-exposed and superposed spectra: only the MK types inferred from quality 1 and 2 spectra were selected for the construction of our catalogue (Houk assigns four qualities to her spectra). \par The second most important source of our MK types was the {\it Catalogue of Selected Spectral Types in the MK System} (M. Jaschek 1978), which contains a selected MK type for about 30\,400 stars in the two hemispheres. M. Jaschek's and \mbox{Houk's} spectral classifications catalogues, whose intersection is not empty, are the largest such catalogues available now. In addition, they are very close to the original system of Morgan and Keenan. This is why, in spite of the better resolution achievable nowadays, we took the spectral types and luminosity classes from these two sources for the majority of our catalogue stars: We preferred homogeneity rather than precision. The {\it Third General Catalogue of MK Spectral Classification} (Buscombe 1977) and the Jensen's catalogue (1983) were also used when no reliable MK type was available in the two main sources. \section{The final catalogues} After the selection process, we got 16\,307 selected stars of all spectral types, all luminosity classes and all distances, gathered in a computer-readable file called "DistEx" (for {\bf Dist}ances and {\bf Ex}tinctions) available from the author on request. Among these stars, there are members of other galaxies (the small and large magellanic clouds) as well as stars belonging to globular clusters and whose metal-deficiency escaped from the selection process. In order to keep only the members of our galaxy having reliable enough distances, we selected the stars which have been given a distance of less than \mbox{3\,000~pc}. They are 15\,449 in number. This set of data, the Catalogue of Extinctions and Distances Derived from UBV data (CEDDU) is the main output of the work presented in this paper. It has been stored in two computer-readable files. So were the sets of data concerning some stars which were discarded during the selection process. The latter need new observations and are interesting candidates for further spectroscopic studies in the optical and in the UV, with higher resolution. \par All these catalogs and related technical informations can be obtained from the Centre de Donn\'ees astronomiques de Strasbourg (CDS), 11 rue de l'Universit\'e, F--67\,000 Strasbourg, France. \subsection{Content of the Catalogue of Extinctions and Distances Derived from UBV data (CEDDU)} CEDDU contains 15\,449 stars of all spectral types, all luminosity classes and with distances not larger than \mbox{3\,000~pc}. The informations on them are stored in two files, having both a record length of 132 bytes. The first one, CEDDU1, displays a selection of observational data along with all the derived and computed parameters, such as absolute magnitude, intrinsic colour $(B-V)_{\rm o}$, interstellar extinction $A_{V}$ and heliocentric distance. The second file, CEDDU2, contains the complete set of observational data. Both files are sorted in ascending galactic longitudes. \par For each star, CEDDU1 displays the following data: \begin{enumerate} \item Bytes 1-12: The identifier (either a HD number or a DM number). \item Bytes 14-35: The MK type written in a standard format. \item Byte 36: A letter indicating the source of the MK type: \begin{itemize} \item "H" indicates that the MK type comes from the {\it Michigan Spectral Catalogue} (Houk \& Cowley 1975; Houk 1978; Houk 1982; Houk \& Smith-Moore 1988). \item "J" indicates that the MK type comes from the {\it Catalogue of Selected Spectral Types in the MK System} (M. Jaschek 1978). \item "B" indicates that the MK type was found in the {\it Third General Catalogue of MK Spectral Classification (Buscombe 1977)}. \item "K" indicates that the MK type was found in the catalogue of Jensen (1983). \item Finally, for a very small number of stars, the MK type was found in the list of spectral classifications provided by SIMBAD. These MK types are indicated by "S". \end{itemize} \item Bytes 39-44: The apparent magnitude V in the UBV system. This value is the average of all the non-deviating measurements provided by the {\it Photoelectric Photometric Catalogue} (Mermilliod 1987). \item Bytes 46-51: The $(B-V)$ colour index in the UBV system. This value is the average of all the non-deviating measurements provided by the {\it Photoelectric Photometric Catalogue} (Mermilliod 1987). \item Bytes 53-58: The $(U-B)$ colour index in the UBV system. This value is the average of all the non-deviating measurements provided by the {\it Photoelectric Photometric Catalogue} (Mermilliod 1987). \item Bytes 62-66: The absolute magnitude of the star. The absolute magnitude determination is described in section 3.3.2. of the paper. \item Bytes 68-71: A string of 4 characters indicating the source of the table which provided the absolute magnitudes (see section 3.3.2): \begin{itemize} \item "GRMK" indicates that the absolute magnitude comes from the Grenier et al. (1985) MK/M$_{V}$ correspondence table for magnitude-limited samples. \item "CGMK" indicates that the absolute magnitude comes from the Corbally and Garrison (1984) MK/M$_{V}$ correspondence table. \item "SKMK" indicates that the absolute magnitude comes from the Schmidt-Kaler (1982) MK/M$_{V}$ correspondence table. \item "SKMQ" indicates that the absolute magnitude comes from the Schmidt-Kaler (1982) $(B-V)_{\rm o}$-Luminosity class/M$_{V}$ correspondence table. In this case, the intrinsic colour $(B-V)_{\rm o}$ necessary for the use of this table has been computed through a photometric method exposed in section 3.3.1. (see Garc\'\i a, Clari\'a and Levato 1988). \end{itemize} \item Bytes 75-79: The intrinsic colour $(B-V)_{\rm o}$. \item Bytes 81-84: A string of either 2 or 4 characters indicating how the intrinsic colour was determined (see section 3.3.1): \begin{itemize} \item "MQ" indicates that the photometric method described in section 3.3.1 was used to compute $(B-V)_{\rm o}$. This method, an update of the one proposed by Johnson \& Morgan (1953), is explained by Garc\'\i a et al. (1988). \item "SK" indicates that the intrinsic colour comes from the MK/$(B-V)_{\rm o}$ correspondence table (Schmidt-Kaler 1982). \item "SK--n", where n is an integer whose value is either 1 or 2, indicates that a correction of n sub-types towards the blue has been performed on the spectral type, before using the MK/$(B-V)_{\rm o}$ correspondence table (Schmidt-Kaler 1982). \item For 10 stars, a correction of 1 sub-type towards the blue has been performed on the spectral type, before using the updated Q method described by Garc\'\i a et al. (1988). "MQ--1" corresponds to these stars. \end{itemize} \item Bytes 87-91: The interstellar extinction $A_{V}$, in magnitudes. It has been calculated as explained in section 3.3.1. \item Bytes 94-97: The heliocentric distance $d$, in parsecs. \item Bytes 100-103: The $X$-coordinate in the galactic plane, in parsecs: \mbox{$X~=~d~\cos{b}~\sin{l}$}, where $l$ and $b$ are the galactic latitude and longitude. \item Bytes 105-109: The $Y$-coordinate in the galactic plane, in parsecs: \mbox{$Y~=~-d~\cos{b}~\cos{l}$}, where $l$ and $b$ are the galactic latitude and longitude. \item Bytes 111-115: The $Z$-coordinate or height above the galactic plane, in parsecs: \mbox{$Z~=~d~\sin{b}$}, where $b$ is the galactic latitude. \item Bytes 119-124: The galactic longitude $l$. \item Bytes 126-131: The galactic latitude $b$. \end{enumerate} \par CEDDU2 provides a more complete information on photometric and spectroscopic observational data, along with the equatorial coordinates (for equinox 2000). Its content is the following: \begin{enumerate} \item Bytes 1-12: The identifier (either a HD number or a DM number). \item Bytes 14-45: The MK type written in a same standard format as in CEDDU1, with all the spectrum peculiarities (if there are). Their source is identical to that of the MK type. \item Byte 46: A letter indicating the source of the MK type, as in CEDDU1. \item Bytes 49-56: The right ascension (equinox 2000). \item Bytes 59-66: The declination (equinox 2000). \item Bytes 69-74: The galactic longitude. \item Bytes 76-81: The galactic latitude. \item Bytes 83-88: The apparent magnitude V in the UBV system. This value is the average of all the non-deviating measurements provided by the {\it Photoelectric Photometric Catalogue} (Mermilliod 1987). \item Bytes 89-91: The number of measurements with which the apparent magnitude V was calculated. \item Bytes 93-98: The rms of the apparent magnitude V. \item Bytes 100-105: The $(B-V)$ colour index in the UBV system. This value is the average of all the non-deviating measurements provided by the {\it Photoelectric Photometric Catalogue} (Mermilliod 1987). \item Bytes 106-108: The number of measurements with which the $(B-V)$ colour index was calculated. \item Bytes 110-115: The rms of the $(B-V)$ colour index. \item Bytes 117-122: The $(U-B)$ colour index in the UBV system, if available. This value is the average of all the non-deviating measurements provided by the {\it Photoelectric Photometric Catalogue} (Mermilliod 1987). \item Bytes 123-125: The number of measurements with which the $(U-B)$ colour index was calculated. \item Bytes 127-132: The rms of the $(U-B)$ colour index. \end{enumerate} Among the 15\,449 stars of CEDDU, 11\,911 are closer than \mbox{120~pc} from the galactic plane ($-120~{\rm pc}~\leq~Z~\leq~120~{\rm pc}$). Note that the proportion of stars for which the $(U-B)$ colour index is available is approximately 82 \%. \subsection{Contents of the appendices} \subsubsection{Stars with negative colour excesses} Our selection process isolated 390 stars for which the estimated $E_{B-V}$ is negative, even after a two spectral sub-types shift towards the blue. These stars were put in dedicated computer-readable files. The data equivalent to those of CEDDU1 are stored in the file exneg1, except that: \begin{itemize} \item The absolute magnitude has not been calculated and is, therefore, missing, as well as its source. \item The interstellar extinction $A_{V}$ is replaced by the colour excess E$_{B-V}$ and shifted by one byte towards the right. \item The distance $d$, $X$, $Y$ and $Z$ have not been calculated. \item The galactic longitude and latitude are missing. \end{itemize} The file exneg2 has the same type of content as CEDDU2, with the same organisation. \subsubsection{Apparent very close stars with heavy reddening} Our program discarded 62 stars because it computes an extinction above 0.5 with a distance below \mbox{20~pc} for them. These stars were put in dedicated computer-readable files. The data equivalent to those of CEDDU1 are stored in the file avlar1, except that: \begin{itemize} \item The distance $d$, $X$, $Y$ and $Z$ are shifted towards the right: They are written between bytes 96 and 120. \item The galactic longitude and latitude are missing. \end{itemize} The file avlar2 has the same type of content as CEDDU2, with the same organisation. \subsubsection{Apparent very far stars with low reddening} Our program discarded 98 stars because it computes an extinction of less than \mbox{0.2~mag/kpc} along the portion of sightline which goes across the galactic disk (with an assumed thickness of \mbox{120~pc}) and a distance of more than \mbox{1~kpc}. It is possible that these stars really exhibit a very low extinction. They were removed from the catalogue only because their extinction is considered as statistically abnormal. The data equivalent to those of CEDDU1 are stored in the file asmal1, except that: \begin{itemize} \item The distance $d$, $X$, $Y$ and $Z$ are shifted towards the right: They are written between bytes 96 and 120. \item The galactic longitude and latitude are missing. \end{itemize} The file asmal2 has the same type of content as CEDDU2, with the same organisation. \begin{thebibliography}{} \bibitem{}Buscombe, W. : 1977, {\it MK Spectral Classifications; Third General Catalogue}, Northwestern University, Evanston. \bibitem{}Corbally, C. J., Garrison, R. F. : 1984, in {\it The MK Process and Stellar Classification}. Proceedings of a workshop, Toronto (Canada), june 1983. R. F. Garrison Ed. p. 277. \bibitem{}Garc\'\i a, B., Clari\'a, J. J., Levato, H. : 1988, {\it Astrophys. Sp. Sci.} {\bf 143}, 317. \bibitem{}Grenier, S., G\'omez, A. E., Jaschek, C., Jaschek, M., Heck, A. : 1985, {\it Astron. Astrophys.} {145}, 331. \bibitem{}Guarinos, J. : {\it Astron. Astrophys. Suppl. Ser.}, submitted. \bibitem{}Houk, N. : 1978, {\it Michigan Catalogue of Two-Dimensional Spectral Types for the HD Stars}, Volume 2, University of Michigan, Ann Arbor, Michigan. \bibitem{}Houk, N. : 1982, {\it Michigan Catalogue of Two-Dimensional Spectral Types for the HD Stars}, Volume 3, University of Michigan, Ann Arbor, Michigan. \bibitem{}Houk, N., Cowley, A. P. : 1975, {\it University of Michigan Catalogue of Two-Dimensional Spectral Types for the HD Stars}, Volume 1, University of Michigan, Ann Arbor, Michigan. \bibitem{}Houk, N., Smith-Moore, M. : 1988, {\it Michigan Catalogue of Two-Dimensional Spectral Types for the HD Stars}, Volume 4, University of Michigan, Ann Arbor, Michigan. \bibitem{}Jaschek, M. : 1978, {\it Bull. Inform. CDS}, {\bf 15}, 121. \bibitem{}Jensen, K. S. : 1983, {\it Spectral Classifications in the MK System for HD Stars in the 25$^{o}~<~\delta~<~30^{o}$ Zone}, catalogue distributed by the CDS under number III/75. \bibitem{}Johnson, H. L., Morgan, W. W. : 1953, {\it Astrophys. J.} {\bf 117}, 313. \bibitem{}Mermilliod, J.-C. : 1987, {\it Astron. Astrophys. Suppl. Ser.} {\bf 71},413. \bibitem{}Schmidt-Kaler, T. : 1982, in {\it Landolt-B\"ornstein}, Vol. VI/2b, K. Schaifers, H. H. Voigt Eds., Springer-Verlag. p. 1. \bibitem{} \bibitem{} \end{thebibliography} \end{document}