\documentstyle[12pt]{article}
\title{The Preliminary Version of the Bibliographical Catalogue
	of Stellar Polarization }
\author{M. L. Belous{\footnotesize $^{1, 2}$}}
\date{}
\begin{document}
\maketitle
{\footnotesize $^{1 }$Institute of Astronomy of the Russian Academy of Sciences,
48 Pyatnitskaya st., Moscow 109017, Russia

$^{2 }$Sternberg Astronomical Institute, University of Moscow, Russia}
\vskip 0.4cm
\hrule
\vskip 1.2cm
\centerline{\large \bf ABSTRACT}
\vskip 0.5cm
	     Bibliographical Catalogue of Stellar Polarization (BCSP)
        will hold all the published data about stellar polarization 
        observations since 1977 up to now. The preliminary version of the 
        Catalogue presents its format and covers the period from 1977 to 1981.
        Due to bibliographic nature of the Catalogue, the main
        information it contains is not minute numerical data but basic
        polarization characteristics, original papers references and
        authors' conclusions about object polarization origin and
        behavior.
\vskip 0.8cm
\centerline{\large \bf INTRODUCTION}
\vskip 0.5cm
             The preliminary version of BCSP contains data about
        polarization measurements of more than 1600 galactic objects
        published in 1977 -- 1981. All the information included in the
        Catalogue has been taken from original papers published during
        this period. The main goal of the Catalogue is to present
        necessary bibliography to explorers studying a certain object
        and to give them some primary polarization data concerning with
        it.

\pagebreak
\centerline{\large \bf I. THE CATALOGUE STRUCTURE}
\vskip 0.5cm

             This computer readible version of the Catalogue consists of
        the files listed in Table 1.
\begin{center}
      \tablename{ 1. Data Files Format}
\end{center}
\begin{center}
      \vskip 0.3cm
      \begin{tabular}{|r|c|c|l|}
            \hline
            {\bf Name} & {\bf Record Length} & {\bf Records Number} & {\bf Description} \\
            \hline
            bcsp.doc & 76   &       473      & documentation file \\
            refs.dat & 96 &       193      &    bibliography 1   \\
            authors.bib & 96 &       193      &    bibliography 2   \\
            bcsp.dat & 139 &      1637     &   main data file \\
            nocoord.dat & 139 &       22      & supplementary data \\
            \hline
      \end{tabular}
\end{center}
\vskip 0.8cm
\centerline{\large \bf II. DETAILED CATALOGUE FILES DESCRIPTION}
\vskip 0.8cm
\begin{tabular}{p{3cm}p{9cm}}
      BCSP.DOC \vskip 0.3cm &  Catalogue documentation file. \vskip 0.3cm \\
      REFS.DAT \vskip 0.3cm &  Reference file (see sec. IX). \vskip 0.3cm \\
      AUTHORS.BIB \vskip 0.3cm &  Same as the previous, but the records are
       sorted corresponding to authors' names. \vskip 0.3cm \\
      NOCOORD.DAT \vskip 0.3cm & Objects which coordinates have been 
       un\-kno\-wn up to the date of this file creation (see sec. IV); the data
       are given in the same form as in the following file. \vskip 0.3cm \\
      BCSP.DAT \vskip 0.3cm &  Contains numerical data. The da\-ta are 
       pre\-sen\-ted in the form described in Table 2. \vskip 0.3cm  \\
\end{tabular}
\pagebreak
\begin{center}
      \tablename{ 2. Numerical Data File Description}
\end{center}
\begin{center}
      \vskip 0.3cm
      \begin{tabular}{|c|c|p{9cm}|}
            \hline
            {\bf Column} & {\bf Position} & {\bf Contents} \\
            \hline
            1 & 1 -- 14 & Object identifier (see sec. III) \\
            2 & 16 -- 22 & R. A. (2000.0): HH MM.m \\
            3 & 24 -- 29 & Decl. (2000.0): $<$sign$>$DD MM \\
            4 & 31 -- 42 & Spectral type (also see notes on coordinates and 
             spectra determination in sec. III) \\
            5 & 44 -- 52 & The degree of polarization, $p$ (see sec. IV) \\
            6 & 54 -- 81 & Information about the wa\-ve\-lengths used during
             observations (see sec. V) \\
            7 & 83 -- 87 & Characteristics of polarization nature and behavior 
             given by author(s) in the original paper (see sec. VI) \\
            8 & 89 -- 102 & Data on observational period (see sec. VII) \\
            9 & 104 -- 113 & Reference (A\&AA number) \\
            10 & 115 -- 124 & Object type \\
            11 & 126 -- 139 & Another object identifier (see sec. III) \\
            \hline
      \end{tabular}
\end{center}
\vskip 0.8cm
\centerline{\large \bf III. OBJECT IDENTIFIERS,}
\centerline{\large \bf COORDINATES AND SPECTRA}
\vskip 0.5cm

             Object identifiers are mostly taken from the articles in
        which these objects are described. Stellar coordinates (Right
        Ascension and Declination 2000.0) and spectral type were
        directly included into the Catalogue, if they were in the
        article. But sometimes authors do not mention coordinates of
        well-known (or well-known to them) objects. So, it was
        necessary to interrogate Simbad database for these important
        data. The same was made if there were only 1950.0 coordinates
        in the original paper. It was possible to deal with most of the
        Catalogue objects like this.

             Several cases were more intricate. Certainly, Simbad
        database does not contain all the astronomical catalogues, so
        from time to time there appears an object unknown to Simbad in
        original paper. Then some attempts were made to find more
        cross-identifications. E. g., Simbad database contains some
        information about white dwarf LP $131-66$ except its other name,
        WD $1247+551$. In such cases identifiers known to Simbad are given in
        the Catalogue. The number of these objects is not more than one
        hundred.

             There are some catalogues (e. g., NIPSS --- Near Infrared
        Photographic Sky Survey) that are not completely incorporated in
        Simbad database. The coordinates of these objects were taken from
        literature (from where it was possible) and recalculated to the
        equinox of 2000.0. Only one or two dozens of such stars present
        in the Catalogue.

             In spite of all the efforts made there were several cases
        in which no source could be found to determine stellar
        coordinates. These objects are collected in file NOCOORD.DAT.
        Further attempts would be applied to get necessary data for
        them.

             If an object spectrum was not presented in the original
        paper, it was taken from Simbad (if it existed there, of
        course). Sometimes spectral classifications of an object from
        Simbad database and from the paper were different. Then the
        Simbad data were preferred except the cases when these two
        classifications were not too diverse.
\vskip 0.5cm

             Object identifiers are included in the catalogue twice:
        in positions 1 -- 14 (column 1) and 126 -- 139 (column 11).
        Everywhere it is possible column 1 contains preferably HD star
        designations.

\vskip 0.8cm
\centerline{\large \bf IV. THE DEGREE OF POLARIZATION }
\vskip 0.5cm

             Degree of linear polarization, $p$, was determined by
        authors during observations and was published in their papers.
        Sometimes authors presented Stokes parameters instead of
        polarization degree and position angle. In such cases it was
        easy to calculate $p$ from these data.

             All the values in this column are given in \%\%. Their
        decimal points are in position 47. The quantity of digits after
        decimal point is the same as in paper and is not reduced to a
        single format.

             This column (5) contains the degree of linear
        polarization only. If you want to know whether circular
        polarization was measured, please pay attention to flag in
        position 83 (see sec. VI). But in some papers only circular
        polarization measurements were presented. Then there is a
        degree of circular polarization in this column with its sign in
        position 44. For linear polarization the latter position
        is blank.

             A large amount of polarization measurements described in
        this Catalogue was multiwavelength. Nevertheless, column 5
        contains only single number. This number represents the most
        high polarization level measured by authors through all the
        observational period and through all the wavelengths. If the
        polarization behavior obeys the Serkowsky law (see sec. VII
        about it; pay attention at flag in position 85), it is not
        difficult to get the wavelength on which such a degree of
        polarization was observed. If not, explorers have more reasons
        to look through the original paper.

\vskip 0.8cm
\centerline{\large \bf V. WAVELENGTHS USED}
\centerline{\large \bf DURING OBSERVATIONS}
\vskip 0.5cm

             Column 6 contains the data about wavelengths used during
        objects observations. This column consists of many flags and
        numbers that do not present in every line. Table 3 presents the
        list of them.

\vskip 0.5cm
{\small
\begin{center}
      \tablename{ 3. Wavelengths Usage Flags}
\end{center}
\vskip 0.3cm
\begin{tabular}{|c|p{11cm}|}
      \hline
      {\bf Position} & {\bf Contains} \\
      \hline
      54 & \#, if there was an unfiltered object measurement, and blank 
       otherwise; \\
      55 -- 61 & Names of Johnson --- Morgan system filters used during 
       observations, and blank, if these filters were not used; \\
      63 -- 64 & Number of other (medium- and narrowband) used filters. If 
       this number was more then 20, there is ``$>$'' sign in position 64; \\
      66 -- 67 & The units used to describe medium- and narrowband filters
       (wavelengths intervals can be measured in units of meters, centimeters,
       millimeters, micrometers, nanometers, angstr\"oms, gigahertzs,
       megahertzs or kiloelectronvolts); \\
      69 -- 74 & One of the medium- or narrowband filters bordering the 
       wavelengths interval measured by authors (in units described before); \\
      76 -- 81 & The other bordering filter. \\
      \hline
\end{tabular}
}
\vskip 0.5cm
{\em Example:}\hspace{2cm}{\sf \#BR \hspace{0.8cm}5 um\/ 1.6 \hspace{0.4cm}   2.2}

             means that this star was measured unfiltered ({\sf \#}), then two
        Johnson --- Morgan system filters ({\sf B} and {\sf R}) were used, and
        besides there were measurements in {\sf five} bands between {\sf 1.6}
        and {\sf 2.2} micrometers ({\sf um}).
\vskip 0.8cm
\centerline{\large \bf VI. REMARKS}
\centerline{\large \bf ON OBJECT POLARIZATION BEHAVIOR}
\centerline{\large \bf AND NATURE}
\vskip 0.5cm

             After observations, authors often make efforts to
        investigate the nature of its polarization basing on the
        behavior of the object during the observational period. If
        such an information presents in original paper, it is
        incorporated in the Catalogue's column 7 using the format described
        in table 4.

\vskip 0.5cm
{\small
      \begin{center}
            \tablename{ 4. Author Remarks Coding}
      \end{center}
      \vskip 0.3cm
      \begin{tabular}{|c|c|p{10cm}|}
      \hline
      {\bf Position} & {\bf Flag} & {\bf Explanation} \\
      \hline
      83 & \multicolumn{2}{|l|}{circular polarization measurements of the
       cor\-res\-pon\-di\-ng ob\-ject~\dots} \\
      \cline{2-3}
      & 0 & \dots were not carried out; \\
      & 1 & \dots were carried out and the degree of circular polarization presents
       in the paper; \\
      & 2 & \dots were carried out but the circular polarization was not detected; \\
      & 3 & \dots did not allow to make clear conclusion; \\
      & 4 & \dots present in the paper, but the author do
       not make any conclusion \\
      \hline
      84 & \multicolumn{2}{|l|}{time variability of observing object
        po\-la\-ri\-za\-ti\-on~\dots} \\
      \cline{2-3}
      & 0 & \dots was not explored; \\
      & 1 & \dots was explored but was not detected; \\
      & 2 & \dots was detected; \\
      & 3 & \dots is not clear; different interpretations are possible; \\
      & 4 & \dots was explored and all the data are in the paper, but the author
       do not make any conclusion; \\
      & 5 & \dots was detected during a part of the observational period and
       definitely was not detected during the other one \\
      \hline
\end{tabular}
\pagebreak
\vskip 0.5cm
\begin{center}
\tablename{ 4 (Continued). Author Remarks Coding}
\end{center}
\begin{tabular}{|c|c|p{10cm}|}
\hline
{\bf Position} & {\bf Flag} & {\bf Explanation} \\
\hline
     85 & \multicolumn{2}{|l|}{wavelength dependence of linear po\-la\-ri\-za\-ti\-on~\dots} \\
     \cline{2-3}
     & 0 & \dots was not explored; \\
     & 1 & \dots was found to be standard (Serkowsky law); \\
     & 2 & \dots was unusual; \\
     & 3 & \dots was not clear enough to allow the author to make any conclusion; \\
     & 4 & \dots was explored and all the data are in the paper, but the author do
      not make any conclusion; \\
     & 5 & \dots was found to fit another law (not Serkowsky); \\
     & 6 & \dots was found to fit Serkowsky law during a part of the observational
      period and definitely not to fit it during the other one; \\
     & 7 & \dots was found to be typical for the class of objects the exploring
      star belongs to \\
     \hline
86 & \multicolumn{2}{|l|}{spatial distribution of polarization in the
                                       re\-gi\-on of the ob\-ject~\dots} \\
\cline{2-3}
& 0 & \dots was not explored; \\
& 1 & \dots was explored and was published as a map without numerical data; \\
& 2 & \dots was explored and was published as a map with numerical data; \\
& 3 & \dots was explored, and besides the author investigated the dependence
            between polarizations of the object and its environment \\
\hline
87 & \multicolumn{2}{|l|}{the author's conclusion of the po\-la\-ri\-za\-ti\-on
                               na\-tu\-re~\dots} \\
\cline{2-3}
& 0 & \dots is absent; \\
& 1 & \dots is that the polarization nature is interstellar; \\
& 2 & \dots is that a part of object polarization is intrinsic; \\
& 3 & \dots is that he hardly can say anything about the polarization
            nature of the object; \\
& 4 & \dots is that during a part of the observational period the object
            polarization was definitely of interstellar origin, but during
            the other one some intrinsic component was detected \\
\hline
\end{tabular}
}
\pagebreak
\vskip 1.8cm
\centerline{\large \bf VII. OBSERVATIONAL PERIOD}
\centerline{\large \bf DESCRIPTION}
\vskip 0.8cm

             These data taken from the original paper are written in
        the following form. There is the date when observations began
        in positions 92 -- 102: year, month abbreviation and day (the
        latter two present if they are given in the paper). Flag in
        position 90 allows to determine the observational period (see
        Table 5).

\vskip 0.5cm
\begin{center}
      \tablename{ 5. Observational Periods Flags}
\end{center}
\begin{center}
\vskip 0.3cm
\begin{tabular}{|c|p{12cm}|}
      \hline
      {\bf Flag} & {\bf Period \dots} \\
      \hline
      0 & \dots is not specified by the author (the year can be taken from
       the paper only); \\
      1 & \dots is not more than 24 hours; \\
      2 & \dots is between a day and a month; \\
      3 & \dots is between a month and a year; \\
      4 & \dots is more than a year \\
      \hline
\end{tabular}
\end{center}
\vskip 0.5cm

             Sometimes observations were carried out nonsystematically
        during a long period but in a form of several shorter periods.
        In such a case there is an asterisk (*) in position 89.
\vskip 1cm
{\em Example:}\hspace{2cm}{\sf *1 \hspace{0.4cm} 1977 \hspace{0.4cm} AUG
               \hspace{0.4cm} 17 }

             means that there were several observational periods (each
        not more than a day) since August 17, 1977.

             For single set of observations, position 89 is blank.
\vskip 0.8cm
\centerline{\large \bf CONCLUSION}
\vskip 0.5cm
             Bibliographical Catalogue of Stellar Polarization
        (preliminary version) presents data about polarimetric
        measurements of more than 1600 stars during the period of 1977
        -- 1980 through all the electromagnetic spectrum from X- to
        radio wavelengths published in astronomical literature. The main
        goal of the Catalogue is to inform explorers about polarimetric
        measurements of objects they are interested in and to quote
        necessary references. So there are not many numerical data in
        the Catalogue. For example, there are no position angles of
        polarization data in it. But the information containing in
        several flags enclosed to each object reference allows to find
        out whether definite paper contains data necessary to the
        explorers' research.

             This work is the preliminary publication of the Catalogue
        only. The final version will contain data about polarization
        measurements from 1977 up to date in the same form.
\vskip 0.8cm
\centerline{\large \bf ACKNOWLEDGEMENTS}
\vskip 0.5cm
             I wish to thank Dr. O. Yu. Malkov for his kind support
        and gentle supervising in this research.

             I thank Prof. C. Jaschek, Prof. A. A. Boyarchuk, Dr. J.
        Krautter and Dr. H. Schwarz for their valuable advices on
        the Catalogue's content and structure.

             I am also grateful to Dr. M. E. Prokhorov for his aid in
        several pulsars identifications and to Dr. F. Ochsenbein for
        his helpful advices in Simbad usage.

             This research has made use of the Simbad database,
        operated at CDS, Strasbourg, France.


\end{document}
