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\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!
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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}
