| Texto completo | |
| Autor(es): |
Dias, W. S.
[1]
;
Monteiro, H.
[1]
;
Moitinho, A.
[2]
;
Lepine, J. R. D.
[3]
;
Carraro, G.
[4]
;
Paunzen, E.
[5]
;
Alessi, B.
[6]
;
Villela, L.
[1, 7]
Número total de Autores: 8
|
| Afiliação do(s) autor(es): | [1] Univ Fed Itajuba, Inst Fis & Quim, Av BPS 1303 Pinheirinho, BR-37500903 Itajuba, MG - Brazil
[2] Univ Lisbon, Fac Ciencias, CENTRA, Ed C8, PL-1749016 Lisbon - Portugal
[3] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, SP - Brazil
[4] Univ Padua, Dept Phys & Astron, Vicolo Osservatorio 3, I-35122 Padua - Italy
[5] Marsaryk Univ, Dept Theoret Phys & Astrophys, Brno 61137 - Czech Republic
[6] Av Engn Antonio Heitor Eiras Garcia 1236, Apto 142, BR-05588001 Sao Paulo, SP - Brazil
[7] Univ Fed Espirito Santo, Dept Engn Elect, Av Fernando Ferrari 514, Campus Univ Goiabeiras, BR-29075710 Vitoria, ES - Brazil
Número total de Afiliações: 7
|
| Tipo de documento: | Artigo Científico |
| Fonte: | Monthly Notices of the Royal Astronomical Society; v. 504, n. 1, p. 356-371, JUN 2021. |
| Citações Web of Science: | 2 |
| Resumo | |
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 G(BP) and G(RP) Gaia 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 Furthermore, it was possible to estimate the mean radial velocity of 831 clusters (198 of which are new and unpublished so far), using stellar radial velocities from Gaia DR2 catalogue.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. (AU) | |
| Processo FAPESP: | 13/01115-6 - Estudo da estrutura da galáxia por meio dos aglomerados abertos de estrelas |
| Beneficiário: | Jacques Raymond Daniel Lépine |
| Modalidade de apoio: | Auxílio à Pesquisa - Pesquisador Visitante - Brasil |