Massive open star clusters using the VVV survey V. Young clusters with an OB stellar population
| Autor: | M. Gromadzki, J. Borissova, Radostin Kurtev, Michael A. Kuhn, A.-N. Chené, P. Amigo, Julio A. Carballo-Bello, S. Ramírez Alegría, Charles Jose Bonatto |
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| Jazyk: | angličtina |
| Rok vydání: | 2016 |
| Předmět: |
Vista Variables in the Via Lactea
Stellar population FOS: Physical sciences Fotometria estelar Astrophysics 01 natural sciences spectroscopic [Techniques] Photometry (optics) Astronomia infravermelha Bulge early-type [Stars] 0103 physical sciences Aglomerados estelares Cluster (physics) massive [Stars] 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Physics general [Open clusters and associations] 010308 nuclear & particles physics photometric [Techniques] Astronomy and Astrophysics Public survey Astrophysics - Astrophysics of Galaxies Espectroscopia infravermelha Star cluster Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) disk [Galaxy] |
| Zdroj: | Repositório Institucional da UFRGS Universidade Federal do Rio Grande do Sul (UFRGS) instacron:UFRGS |
| Popis: | The ESO public survey VISTA Variables in the V\'ia L\'actea (VVV) has contributed with deep multi-epoch photometry of the Galactic bulge and the adjacent part of the disk over 526 square degrees. More than a hundred cluster candidates have been reported thanks to this survey. We present the fifth article in a series of papers focused on young and massive clusters discovered in the VVV survey. In this paper, we present the physical characterization of five clusters with a spectroscopically confirmed OB-type stellar population. To characterize the clusters, we used near-infrared photometry ($J$, $H,$ and $K_S$) from the VVV survey and near-infrared $K$-band spectroscopy from ISAAC at VLT, following the methodology presented in the previous articles of the series. All clusters in our sample are very young (ages between 1-20 Myr), and their total mass are between $(1.07^{+0.40}_{-0.30})\cdot10^2$ $M_{\odot}$ and $(4.17^{+4.15}_{-2.08})\cdot10^3$ $M_{\odot}$. We observed a relation between the clusters total mass $M_{ecl}$ and the mass of their most massive stellar member $m_{max}$, even for clusters with an age $ Comment: Accepted for publication, A&A |
| Databáze: | OpenAIRE |
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