Volume 488, Number 1, September II 2008
|Page(s)||151 - 159|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||01 July 2008|
The young Galactic star cluster [DBS2003] 179 *
Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Ave. Gran Bretaña 1111, Playa Ancha, Casilla 5030, Valparaíso, Chile e-mail: email@example.com
2 European Southern Observatory, Av. Alonso de Córdoba 3107, Casilla 19, Santiago 19001, Chile e-mail: firstname.lastname@example.org
3 University of Cincinnati, Cincinnati, Ohio 45221-0011, USA e-mail: email@example.com
4 Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-254, CD Universitaria, CP 04510 Mexico DF, Mexico e-mail: firstname.lastname@example.org
5 Departmento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile and Vatican Observatory, Specola Vaticana, V00120 Vatican City State, Italy e-mail: email@example.com
6 Departmento de Astronomía, Universidad de Concepcion, Casilla 160-C, Concepcion, Chile e-mail: firstname.lastname@example.org
Accepted: 16 April 2008
Context. Recent near- and mid-infrared surveys have brought evidence that the Milky Way continues to form massive clusters.
Aims. We carry out a program to determine the basic physical properties of the new massive cluster candidate [DBS2003] 179.
Methods. Medium-resolution K-band spectra and deep near-infrared images of [DBS2003] 179 were used to derive the spectral types of eight member stars, and to estimate the distance and reddening to the cluster.
Results. Seven of ten stars with spectra show emission lines. Comparison with template spectra indicated that they are early O-type stars. The mean radial velocity of the cluster is km s-1. Knowing the spectral types of the members and the color excesses, we determined extinction and distance modulus ( mag ( Kpc). The presence of early O-stars and a lack of red supergiants suggests a cluster age of 2–5 Myr. The total cluster mass is approximated to and it is not yet dynamically relaxed.
Conclusions. The candidate [DBS2003] 179 further increases the family of the massive young clusters in the Galaxy, although it appears less massive than the prototypical starburst clusters.
Key words: Galaxy: open clusters and associations: general / Galaxy: open clusters and associations: individual [DBS2003] 179 / stars: early-type / stars: emission-line, Be
© ESO, 2008
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