Gaia Data Release 2 Variable stars in the colour-absolute magnitude diagram

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Gaia Collaboration , Eyer , L , Muinonen , K , Fedorets , G , Granvik , M & Siltala , L 2019 , ' Gaia Data Release 2 Variable stars in the colour-absolute magnitude diagram ' , Astronomy & Astrophysics , vol. 623 , A110 . https://doi.org/10.1051/0004-6361/201833304

Title: Gaia Data Release 2 Variable stars in the colour-absolute magnitude diagram
Author: Gaia Collaboration; Eyer, L.; Muinonen, K.; Fedorets, G.; Granvik, M.; Siltala, L.
Contributor: University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
Date: 2019-03-13
Language: eng
Number of pages: 20
Belongs to series: Astronomy & Astrophysics
ISSN: 1432-0746
URI: http://hdl.handle.net/10138/308409
Abstract: Context. The ESA Gaia mission provides a unique time-domain survey for more than 1.6 billion sources with G less than or similar to 21 mag. Aims. We showcase stellar variability in the Galactic colour-absolute magnitude diagram (CaMD). We focus on pulsating, eruptive, and cataclysmic variables, as well as on stars that exhibit variability that is due to rotation and eclipses. Methods. We describe the locations of variable star classes, variable object fractions, and typical variability amplitudes throughout the CaMD and show how variability-related changes in colour and brightness induce "motions". To do this, we use 22 months of calibrated photometric, spectro-photometric, and astrometric Gaia data of stars with a significant parallax. To ensure that a large variety of variable star classes populate the CaMD, we crossmatched Gaia sources with known variable stars. We also used the statistics and variability detection modules of the Gaia variability pipeline. Corrections for interstellar extinction are not implemented in this article. Results. Gaia enables the first investigation of Galactic variable star populations in the CaMD on a similar, if not larger, scale as was previously done in the Magellanic Clouds. Although the observed colours are not corrected for reddening, distinct regions are visible in which variable stars occur. We determine variable star fractions to within the current detection thresholds of Gaia. Finally, we report the most complete description of variability-induced motion within the CaMD to date. Conclusions. Gaia enables novel insights into variability phenomena for an unprecedented number of stars, which will benefit the understanding of stellar astrophysics. The CaMD of Galactic variable stars provides crucial information on physical origins of variability in a way that has previously only been accessible for Galactic star clusters or external galaxies. Future Gaia data releases will enable significant improvements over this preview by providing longer time series, more accurate astrometry, and additional data types (time series BP and RP spectra, RVS spectra, and radial velocities), all for much larger samples of stars.
Subject: stars: general
stars: variables: general
stars: oscillations
binaries: eclipsing
surveys
methods: data analysis
CEPHEID PULSATION MODELS
RR LYRAE STARS
VARIABILITY
CATALOG
ASTEROSEISMOLOGY
SEARCH
115 Astronomy, Space science
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