VdBH 222: a starburst cluster in the inner Milky Way
Por favor, use este identificador para citar o enlazar este ítem:
http://hdl.handle.net/10045/40564
Título: | VdBH 222: a starburst cluster in the inner Milky Way |
---|---|
Autor/es: | Marco, Amparo | Negueruela, Ignacio | González-Fernández, Carlos | Maíz Apellániz, Jesús | Dorda Laforet, Ricardo | Clark, J. Simon |
Grupo/s de investigación o GITE: | Astrofísica Estelar (AE) |
Centro, Departamento o Servicio: | Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal |
Palabras clave: | Hertzsprung-Russell and C-M diagrams | Stars: evolution | Stars: early-type | Supergiants | Techniques: photometric | Techniques: spectroscopic |
Área/s de conocimiento: | Astronomía y Astrofísica |
Fecha de publicación: | 16-jul-2014 |
Editor: | EDP Sciences |
Cita bibliográfica: | Astronomy & Astrophysics. 2014, 567: A73. doi:10.1051/0004-6361/201423897 |
Resumen: | Context. It has been suggested that the compact open cluster VdBH 222 is a young massive distant object. Aims. We set out to characterise VdBH 222 using a comprehensive set of multi-wavelength observations. Methods. We obtained multi-band optical (UBVR) and near-infrared (JHKS) photometry of the cluster field, as well as multi-object and long-slit optical spectroscopy for a large sample of stars in the field. We applied classical photometric analysis, as well as more sophisticated methods using the CHORIZOS code, to determine the reddening to the cluster. We then plotted dereddened HR diagrams and determined cluster parameters via isochrone fitting. Results. We have identified a large population of luminous supergiants confirmed as cluster members via radial velocity measurements. We find nine red supergiants (plus one other candidate) and two yellow supergiants. We also identify a large population of OB stars. Ten of them are bright enough to be blue supergiants. The cluster lies behind ≈7.5 mag of extinction for the preferred value of RV = 2.9. Isochrone fitting allows for a narrow range of ages between 12 and 16 Ma. The cluster radial velocity is compatible with distances of ~6 and ~10 kpc. The shorter distance is inconsistent with the age range and Galactic structure. The longer distance implies an age ≈ 12 Ma and a location not far from the position where some Galactic models place the far end of the Galactic bar. Conclusions. VdBH 222 is a young massive cluster with a likely mass >20 000 M⊙. Its population of massive evolved stars is comparable to that of large associations, such as Per OB1. Its location in the inner Galaxy, presumably close to the end of the Galactic bar, adds to the increasing evidence for vigorous star formation in the inner regions of the Milky Way. |
Patrocinador/es: | This research is partially supported by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant AYA2012-39364-C02-02. J.M.A. acknowledges support for this work by the Spanish Government Ministerio de Ciencia e Innovación through grants AYA 2010-17631 and AYA 2010-15081 and by the Junta de Andalucía grant P08-TIC-4075. |
URI: | http://hdl.handle.net/10045/40564 |
ISSN: | 0004-6361 (Print) | 1432-0746 (Online) |
DOI: | 10.1051/0004-6361/201423897 |
Idioma: | eng |
Tipo: | info:eu-repo/semantics/article |
Derechos: | © ESO, 2014 |
Revisión científica: | si |
Versión del editor: | http://dx.doi.org/10.1051/0004-6361/201423897 |
Aparece en las colecciones: | INV - Astrofísica Estelar - Artículos de Revistas |
Archivos en este ítem:
Archivo | Descripción | Tamaño | Formato | |
---|---|---|---|---|
2014_Marco_etal_A&A.pdf | 1,58 MB | Adobe PDF | Abrir Vista previa | |
Todos los documentos en RUA están protegidos por derechos de autor. Algunos derechos reservados.