PIECKA, Martin and Ernst PAUNZEN. Structure of Open Clusters - Gaia DR2 and its limitations. Bulgarian Astronomical Journal. Institute of Astronomy and NAO, 2022, vol. 36, July, p. 1-27. ISSN 1313-2709.
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Basic information
Original name Structure of Open Clusters - Gaia DR2 and its limitations
Authors PIECKA, Martin (703 Slovakia, guarantor, belonging to the institution) and Ernst PAUNZEN (40 Austria, belonging to the institution).
Edition Bulgarian Astronomical Journal, Institute of Astronomy and NAO, 2022, 1313-2709.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher Bulgaria
Confidentiality degree is not subject to a state or trade secret
WWW URL URL
Impact factor Impact factor: 0.400
RIV identification code RIV/00216224:14310/22:00125034
Organization unit Faculty of Science
UT WoS 000709909100001
Keywords in English open clusters; astrometry; galactic structure; gaia; satellite mission
Tags rivok
Tags International impact, Reviewed
Changed by Changed by: Mgr. Marie Šípková, DiS., učo 437722. Changed: 9/1/2023 10:44.
Abstract
Very precise observational data are needed for studying the stellar cluster parameters (distance, reddening, age, metallicity) and cluster internal kinematics. In turn, these give us an insight into the properties of our Galaxy, for example, by giving us the ability to trace Galactic spiral structure, star formation rates and metallicity gradients. We investigated the available Gaia DR2 catalogue of 1229 open clusters and studied cluster distances, sizes and membership distributions in the 3D space. An appropriate analysis of the parallax to-distance transformation problem is presented in the context of getting distances toward open clusters and estimating their sizes. Based on our investigation of the Gaia DR2 data we argue that, within 2 kpc, the inverse-parallax method gives comparable results (distances and sizes) as the Bayesian approach based on the exponentially decreasing volume density prior. Both of these methods show very similar dependence of the line-of-sight elongation of clusters (needle-like shapes resulting from the parallax uncertainties) on the distance. We also looked at a measure of elongations of the studied clusters and find the maximum distance of 665 pc at which a spherical fit still contains about half of the stellar population of a cluster. It follows from these results that the 3D structure of an open cluster cannot be properly studied beyond similar to 500 pc when using any of the mentioned standard transformations of parallaxes to distances.
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