Baltic Astronomy, vol. 21, , 2012 THE NEW VERSION OF THE BINARY STAR DATABASE (BDB)

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1 Baltic Astronomy, vol. 21, , 2012 THE NEW VERSION OF THE BINARY STAR DATABASE (BDB) P. Kaygorodov 1, B. Debray 2, N. Kolesnikov 3, D. Kovaleva 1 and O. Malkov 1,3 1 Institute of Astronomy, Russian Acad. Sci., 48 Pyatnitskaya, Moscow , Russia; pasha@inasan.ru 2 Institut UTINAM, CNRS UMR 6213, Observatoire de Besançon, Université de Franche-Comté, 41 bis Avenue de l Observatoire, F Besançon, Cedex, France; debray@obs-besancon.fr 3 Faculty of Physics, Moscow State University, Leninskie Gory, Moscow GSP-1, Russia; malkov@inasan.ru Received: 2012 February 13; accepted: 2012 May 18 Abstract. The Binary star database contains data on about stellar systems of multiplicity 2 to 22, taken from a large variety of published catalogues for all types of binary stars: visual, orbital, astrometric, interferometric, spectroscopic, photometric, eclipsing, etc. Positional, kinematic, photometric, spectroscopic, orbital and astrophysical parameters are provided when available. The database can be queried by identifier, coordinates, catalogue and stellar/orbital parameters (including binary type) of objects. Lists of objects can be submitted as well. Also, the database provides links to some other online services, both of general purpose and on binary stars. A pilot version of BDB can be accessed at Key words: 1. INTRODUCTION binaries: general database virtual observatory Binary stars are very numerous: apparently more than a half of the Milky Way stars are not single ones, but belong to binary or multiple star systems. Our knowledge of accurate stellar masses, radii and other fundamental astrophysical parameters is based exclusively on data derived for some types of binary stars. Analysis of observational data for various types of binary stars allows us to obtain a general understanding of star formation processes and evolutionary scenario for binary as well as single stars. Construction of catalogues / databases of binary stars has a long history. Compilations of data for binary stars have been published for visual (WDS, Washington Double Star catalogue, interferometric (INT4, eclipsing (CEV, Catalogue of Eclipsing Variables, Malkov et al. 2006), spectroscopic (SB9, and other types of binaries. However, a comprehensive study of stellar populations should not be limited

2 310 P. Kaygorodov, B. Debray, N. Kolesnikov, D. Kovaleva, O. Malkov to a particular type of binary stars: e.g., to properly restore the star formation history, all types of binaries, from common proper motion s to close binaries with a degenerate component, should be analyzed. Also, a parametrization of components and orbits of binary stars cannot be limited to a particular type of observational data. Properties of components of eclipsing binaries can be derived only if radial velocity curves of the components are observed as well. To calculate masses of visual binary components, orbital parameters should be combined with photocentric-orbit observational data and system parallax. Components of a spectroscopic binary can be parametrized only if the is astrometrically or interferometrically resolved. Thus, existent data on different observational types of binaries, kept in various data centers / catalogues / databases scattered around the world, should be collected and united (or linked). The widely used SIMBAD astronomical database provides basic data, crossidentifications and bibliography for astronomical objects outside the solar system. However, the SIMBAD and many other useful databases are oriented primarily to single objects. The list of basic data for binary stars contains additional parameters, such as semi-major axis and eccentricity. Also, cross-identification of components in multiple systems sometimes cannot be based just on coordinate matching, and needs more careful approaches. Therefore, a compilation of a database combining observational data and cross-identifications for all types of binaries is extremely worthwhile. Initially, the Binary star database (BDB) was constructed in Besançon Observatory ( It contained the CCDM and WDS1996 catalogues of visual binaries, a list of eclipsing binaries and three photometric (UBV, Stromgren, Geneva) catalogues. In 2008, it was decided to move BDB to the Institute of Astronomy (Moscow), where the database was significantly reconstructed and renovated. Main BDB objectives and ideas of BDB management were discussed in Malkov et al. (2009). The BDB scheme and BDB data sources are described in Sections 2 and 3, respectively. Usage of the BDB is discussed in Section 4. In Section 5, we mention our main lines of development for the database. 2. BDB SCHEME BDB stores all data from the original catalogues as is, but some supplementary data is also generated, based on the catalogued content. This data is used mostly for search and cross-identification. There are several internal tables in the database, containing supplementary data: components table; s table; systems table; ID s table. Records of the Components table contain information about components of s and systems: coordinates, magnitude and photometric band, spectral type, radial velocity, parallax, proper motion. A star can have more than one record in this table if information about it is drawn from several catalogues. Some record fields can be empty if there is no corresponding data in the catalogues. The Pairs table contains data on s. Here is a specific ing, usually s of single stars but sometimes higher-order ings within hierarchical systems. Each record in this table holds information about the : relative coordinates (θ and ρ) with epoch of observation, period, semi-major axis, inclination,

3 / :.-)*+, "#$%&' (! }~ klmnopqrstuvwxyz{j ^_àbcdefghi ]\ The new version of the Binary star database (BDB) 311 Cross-ID table original data catalogue catalogue catalogue file #1 file file file #3 file line #1 line #2 ID's table (CCDM) file #2 file # ID System (WDS) ID System (WDS) ID System (WDS) ID System (WDS) WDS WDS WDS s table P=... P=... P= a... =... a=... a=... system P =... P=... P= a... =... P= a= a=... a= components table component A component A M =... M=... R =... component B component B M =... M=... R =... Fig. 1. BDB scheme eccentricity. If the is an unresolved binary, the record can also contain information on coordinates, parallax, proper motion, radial velocity, minimum and maximum magnitude. Also, each record in this table can refer up to two records in the Components table. If a contains a smaller-order ing (in hierarchical systems), then the record will refer to the primary component in the smaller-order ing. Some of the fields in this table duplicate fields from the Components table because, in some cases, we have no information about components of, for example, a spectroscopic binary. The Systems table does not contain specific information; it is only used to connect s of each system. Each record in this table can refer to one or more records in the Pairs table. All of the records in the tables have one or more references in the ID s table. The ID s table contains identifiers (ID s) of systems, s and components. Each ID can be referenced by one or more entities because different catalogues can provide information about same s or components. Also, some additional references between ID s can be produced by cross-identification process. Cross-identification in the BDB takes place in three stages. At the first stage, the cross-identification data, provided by the catalogue, are analyzed and references in the ID s table are created. At the second stage, all the components from the Components table that are close in their parameters are detected and cross-identification data are produced for them in a semi-manual manner. At the last stage, the cross-identification data for s are produced, based on crossidentification of the components.

4 312 P. Kaygorodov, B. Debray, N. Kolesnikov, D. Kovaleva, O. Malkov 3. BDB DATA SOURCES The efficiency of a database strongly depends on the catalogues that are included into it. The list of catalogues to be integrated in the BDB was published by Malkov et al. (2011). The catalogues are included as is. We do not modify catalogued data without permission of the authors. The origin of information, presented as a result of a BDB query, is clearly indicated. Some sources listed in Malkov et al. (2011) were recently substituted by modern versions, namely: DM3 ( replaced DM2; Multiple star catalogue ( version of 1997 is replaced by up-to-date version of 2010; regularly updated on-line version is available at ATNF Pulsars database ( replaces Catalog of pulsars of A number of important binary star catalogues were recently published and uploaded in VizieR. Below we list catalogues of binaries of different types, published in , which are uploaded in the BDB: 1. Astrometrically detected Double stars with PISCO at Pic du Midi (Scardia et al. 2000); Pulkovo Visual Double Star Catalogue (Kiselev et al. 2003); Binary stars in the Orion Nebula Cluster (Koehler et al. 2006); Double-star speckle measurements (Horch et al. 2006); PISCO speckle observations in 2004 (Scardia et al. 2006); Faint companions of Hipparcos stars (Lepine and Bongiorno 2007); Wide companions of low-mass stars and brown dwarfs (Allen et al. 2007); Speckle interferometry at the USNO station (Hartkopf et al. 2008); Dynamical study of wide s of stars from WDS (Kiyaeva et al. 2008); WIYN binary stars speckle observations (Horch et al. 2008); Observations of contact binaries (Rucinski et al. 2007); MK classifications of visual multiples (Abt, 2008); PISCO speckle observations in 2006 (Scardia et al. 2009); CCD observations of visual double stars (Izmailov et al. 2010); CPMDS (Common Proper Motion Double Stars) catalogue (Gavras et al. 2010); HIP binaries with radial velocities (Frankowski et al. 2007). 2. Spectroscopically detected Companions to close spectroscopic binaries (Tokovinin et al. 2006); Close binary systems from SDSS DR4 (Silvestri et al. 2006);

5 The new version of the Binary star database (BDB) 313 Orbital elements of 156 spectroscopic binaries (Mermilliod et al. 2007); New close binary systems from the SDSS DR5 (Silvestri et al. 2007); SDSS WD main-sequence binaries (Rebassa-Mansergas et al. 2007); White dwarf red dwarf binaries in the SDSS (Augusteijn et al. 2008); Spectral analysis of 636 SDSS WD-M binaries (Heller et al. 2009); Radial velocities of SBs with an M giant (Famaey et al. 2009); Rotational velocities of early-type binaries (Howe and Clarke al. 2009); ASAS chromospherically active eclipsing binaries (Parihar et al. 2009); MK classifications of spectroscopic binaries (Abt 2009); Post-common-envelope binaries from SDSS. VIII (Schreiber et al. 2010); SDSS WD main-sequence binaries (Rebassa-Mansergas et al. 2010); Binaries with a white dwarf in 2MASS (Hoard et al. 2007). 3. Photometrically detected ASAS Variable Stars in the Southern hemisphere (Pojmanski et al ) BV photometry of M31 eclipsing binaries (Vilardell et al. 2006); LMC eclipsing binaries in the MACHO database (Derekas et al. 2007); BI light curves of NGC 2506 variables (Arentoft et al. 2007); MACHO r, b light curves of MC eclipsing binaries (Faccioli et al. 2007); Properties of eclipsing binaries found in TrES (Devor et al. 2008); ASAS eclipsing binaries with RASS counterparts (Szczygiel et al. 2008); Eclipsing binary candidates in the Corot-IRa01 field (Carpano et al. 2009); 1318 new variable stars in the Galactic plane (Miller et al. 2010); Period changes of EA-, EB- and EW-types binaries (Liao and Qian 2010). 4. Detected in other wavelengths XMM-Newton LMXBs in NGC4649 (Randall et al. 2006); A ROSAT survey of contact binary stars (Geske et al. 2006); LMXBs in globular clusters of 5 galaxies (Kundu et al. 2007). 5. Astrophysical parameters Catalogue of close binaries (Soydugan et al. 2006); Eclipsing Binary with Eccentric Orbits Catalog (Bulut and Demircan 2007); Early-type binaries on main sequence (Khaliullin and Khaliullina 2010); A survey of stellar families (Raghavan et al. 2010).

6 314 P. Kaygorodov, B. Debray, N. Kolesnikov, D. Kovaleva, O. Malkov 6. Other Multiplicity of contact binaries (Pribulla and Rucinski 2006); Multiplicity among bright stellar systems (Eggleton and Tokovinin 2008). Beside these catalogues, the BDB provides links to external on-line data resources on binary stars of different observational types, particularly, to databases on visual binaries SIDONIe (Site Informatique des etoiles Doubles de Nice, Pulkovo Database of Observations of Visual Double Stars ( to databases on eclipsing binaries Cracow Observatory Eclipsing Minima Database (CESMID, Database of times of minima (E) and maxima (RR) (var.astro.cz/ocgate/index.php?lang=en); Eclipsing Binaries Minima Database ( Mt.Suhora Astronomical Observatory (Cracow) Linear ephemerides ( and O-C diagrams: ( Kepler Eclipsing Binary Catalogue ( and to catalogues and databases on variable stars, including some types of binaries: GCVS General Catalogue of Variable Stars ( IBVS Information Bulletin on Variable Stars ( containing ADS-like bibliographic database on variable stars; AAVSO Star Finder list ( British Astronomical Association. Variable Star Section list ( AFOEV Association Francaise des Observateurs d Etoiles Variables ( BAV Bundesdeutsche Arbeitsgemeinschaft fur Veranderliche Sterne ( OGLE-III Catalogue of Variable Stars (

7 The new version of the Binary star database (BDB) 315 Binary stars are clearly indicated in the GCVS, while the other six catalogues listed above have no indication of objects binarity. To facilitate and fasten a query to the BDB, current versions of permanently updated databases / catalogues (e.g. WDS, GSVS) will be uploaded to the BDB from time to time. The BDB will also provides links to general-purpose astronomical databases SIMBAD astronomical database ( The SAO/NASA Astrophysics Data System ADS ( 4. USE OF BDB The BDB can be accessed interactively on the site via a web interface. The main page offers forms for two types of queries: by identifier and by parameters. Query by identifier allows a user to select identification system from the list (Name/Bayer/Flamsteed, HD, HIP, GCVS, DM, CCDM, WDS, ADS, IDS, SBC9, IGR) and enter the ID. While typing the ID, an interactive hint is displayed, allowing user to write only a part of the identifier for searching. The CDS service Sesame is used to resolve various stellar identifiers. After submitting the form, the main result page is displayed. This page contains fundamental parameters of the entities found by the query. For the components, s and system, all the parameters, held in the database are presented. Also, all of the components of the and all s of the system (if a or system was found by the query) are displayed. All displayed entities are grouped by systems and s. Also, an image containing graphical representation of the all objects found is displayed. On the image, components of visual binaries are represented by circles; spectroscopic binaries and hierarchical systems are shown as circles with two or more dots within. Clicking to the dots, circles or entity names, one can mark them for displaying. When one or more items are marked, the Show catalogue data button and data selection form, where catalogues for data extraction can be selected, will appear. Clicking the Show catalogue data button leads to displaying the page with raw data, extracted from selected catalogues. Query by parameters allows a user to compile a list of binaries satisfying one or more conditions. One can make a query by coordinates, system type, catalogue name or other parameters of s (e.g., angular separation) and components (e.g., mass). Result of the query is listed in generally used formats HTML, ASCII, XML (VOTable). 5. CONCLUSIONS The Binary star database (BDB) is an attempt to unite most of available catalogued data on all types of binary and multiple stars. The current BHB version ( contains astrometric, photometric, spectroscopic and other data (and links to external on-line services) on some 100 thousand systems, which can be queried by object name, coordinates and various criteria. The BDB can serve as a database for deriving and combining empirical data for all types of binary/multiple systems, for determination of stellar and orbital pa-

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