DIAS, W. S., H. MONTEIRO, A. MOITINHO, J. R. D. LEPINE, G. CARRARO, Ernst PAUNZEN, B. ALESSI and L. VILLELA. Updated parameters of 1743 open clusters based on Gaia DR2. Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021, vol. 504, No 1, p. 356-371. ISSN 0035-8711. Available from: https://dx.doi.org/10.1093/mnras/stab770.
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Basic information
Original name Updated parameters of 1743 open clusters based on Gaia DR2
Authors DIAS, W. S. (guarantor), H. MONTEIRO, A. MOITINHO, J. R. D. LEPINE, G. CARRARO, Ernst PAUNZEN (40 Austria, belonging to the institution), B. ALESSI and L. VILLELA.
Edition Monthly Notices of the Royal Astronomical Society, Oxford University Press, 2021, 0035-8711.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher United Kingdom of Great Britain and Northern Ireland
Confidentiality degree is not subject to a state or trade secret
WWW URL
Impact factor Impact factor: 5.235
RIV identification code RIV/00216224:14310/21:00121843
Organization unit Faculty of Science
Doi http://dx.doi.org/10.1093/mnras/stab770
UT WoS 000656137100024
Keywords in English Galaxy: open clusters and associations: general
Tags rivok
Tags International impact, Reviewed
Changed by Changed by: Mgr. Marie Šípková, DiS., učo 437722. Changed: 25/6/2021 11:56.
Abstract
In this study, we follow up our recent paper (Monteiro et al. 2020) and present a homogeneous sample of fundamental parameters of open clusters in our Galaxy, entirely based on Gaia DR2 data. We used published membership probability of the stars derived from Gaia DR2 data and applied our isochrone fitting code, updated as in Monteiro et al. (2020), to GBP and GRPGaia DR2 data for member stars. In doing this, we take into account the nominal errors in the data and derive distance, age, and extinction of each cluster. This work therefore provides parameters for 1743 open clusters and, as a by-product, a list of likely not physical or dubious open clusters is provided as well for future investigations. Furthermore, it was possible to estimate the mean radial velocity of 831 clusters (198 of which are new and unpublished so far), using stellar radial velocities from Gaia DR2 catalogue. By comparing the open cluster distances obtained from isochrone fitting with those obtained from a maximum likelihood estimate of individual member parallaxes, we found a systematic offset of (−0.05 ± 0.04) mas.
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