\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}