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dc.contributor.author
Carraro, G.
dc.contributor.author
Turner, D.
dc.contributor.author
Majaess, D.
dc.contributor.author
Baume, Gustavo Luis
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dc.date.available
2015-10-08T19:16:04Z
dc.date.issued
2013-07
dc.identifier.citation
Carraro, G.; Turner, D.; Majaess, D.; Baume, Gustavo Luis; The distance to the young open cluster Westerlund 2; EDP Sciences; Astronomy & Astrophysics; 555; A50; 7-2013; 1-9
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/2430
dc.description.abstract
A new X-ray, UBVRIc, and JHKs study of the young cluster Westerlund 2 was undertaken to resolve discrepancies tied to the cluster’s distance. Existing spectroscopic observations for bright cluster members and new multi-band photometry imply a reddening relation toward Westerlund 2 described by EU−B/EB−V = 0.63 + 0.02 EB−V . Variable-extinction analyses for Westerlund 2 and nearby IC 2581 based upon spectroscopic distance moduli and ZAMS fitting yield values of RV = AV/EB−V = 3.88±0.18 and 3.77±0.19, respectively, and confirm prior assertions that anomalous interstellar extinction is widespread throughout Carina. The results were confirmed by applying the color-difference method to UBVRIcJHKs data for 19 spectroscopically observed cluster members, yielding RV = 3.85 ± 0.07. The derived distance to Westerlund 2 of d = 2.85 ± 0.43 kpc places the cluster on the far side of the Carina spiral arm. The cluster’s age is no more than τ ∼ 2 × 106 yr as inferred from the cluster’s brightest stars and an X-ray (Chandra) cleaned analysis of its pre-main-sequence demographic. Four Wolf-Rayet stars in the cluster core and surrounding corona (WR20a, WR20b, WR20c, and WR20aa) are very likely cluster members, and their inferred luminosities are consistent with those of other late-WN stars in open clusters. The color–magnitude diagram for Westerlund 2 also displays a gap at spectral type B0.5 V with associated color spread at higher and lower absolute magnitudes that might be linked to close binary mergers. These features, in conjunction with the evidence for mass loss from the WR stars, may help to explain the high flux of γ-rays, cosmic rays, and X-rays from the direction toward Westerlund 2.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc/2.5/ar/
dc.subject
Open Clusters And Associations
dc.subject
Wolf-Rayet
dc.subject
H Ii Regions
dc.subject
Westerlund 2
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
The distance to the young open cluster Westerlund 2
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2016-03-30 10:35:44.97925-03
dc.journal.volume
555
dc.journal.number
A50
dc.journal.pagination
1-9
dc.journal.pais
Francia
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dc.journal.ciudad
Les Ulis
dc.conicet.avisoEditorial
© ESO 2013
dc.description.fil
Fil: Carraro, G.. Observatorio Europeo Austral; Chile;
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Fil: Turner, D.. Saint Mary’s University. Department of Astronomy and Physics; Canadá;
dc.description.fil
Fil: Majaess, D.. Saint Mary’s University. Department of Astronomy and Physics; Canadá;
dc.description.fil
Fil: Baume, Gustavo Luis. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica La Plata; Argentina;
dc.journal.title
Astronomy & Astrophysics
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2013/07/aa21421-13/aa21421-13.html
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/http://arxiv.org/abs/1305.4309
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/201321421
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