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Embedded star clusters in the W51 giant molecular cloud

Nanda Kumar, M. S. ; Kamath, U. S. ; Davis, C. J.

Monthly notices of the Royal Astronomical Society, 2004-10, Vol.353 (4), p.1025-1034 [Periódico revisado por pares]

23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone 226 7232 Fax 226 3803: Blackwell Science Ltd

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  • Título:
    Embedded star clusters in the W51 giant molecular cloud
  • Autor: Nanda Kumar, M. S. ; Kamath, U. S. ; Davis, C. J.
  • Assuntos: H ii regions ; infrared: stars ; ISM: clouds ; ISM: individual: W51 GMC ; stars: formation ; turbulence
  • É parte de: Monthly notices of the Royal Astronomical Society, 2004-10, Vol.353 (4), p.1025-1034
  • Notas: istex:9EFA8F9F6D91574789B8132EB408A8EEB05FE783
    ArticleID:MNR8143
    ark:/67375/WNG-FTT9R7ZG-Q
    ObjectType-Article-2
    SourceType-Scholarly Journals-1
    ObjectType-Feature-1
    content type line 23
  • Descrição: ABSTRACT We present sub‐arcsecond (0.35–0.9 arcsec), near‐infrared J‐, H‐ and K‐band photometric observations of six fields along the W51 giant molecular cloud (W51 GMC). Our observations reveal four new, embedded clusters and provide a new high‐resolution (0.35 arcsec) view of the W51 IRS2 (G49.5 − 0.4) region. The cluster associated with G48.9 − 0.3 is found to be a double cluster enclosed in a nest of near‐infrared nebulosity. We construct stellar surface density maps for four major clusters in the W51 GMC. These unveil the underlying hierarchical structure. Colour–colour and colour–magnitude diagrams for each of these clusters show clear differences in the embedded stellar populations and indicate the relative ages of these clusters. In particular, the clusters associated with the H ii regions G48.9 − 0.3 and G49.0 − 0.3 are found to have a high fraction of young stellar objects and are therefore considered the youngest of all the near‐infrared clusters in the W51 GMC. The estimated masses of the individual clusters, when summed, yield a total stellar mass of ∼104 M⊙ in the W51 GMC, implying a star formation efficiency of 5–10 per cent. These results, in comparison with the CO observations of the W51 GMC, suggest for the first time that star formation in the W51 GMC is probably triggered by a galactic spiral density wave.
  • Editor: 23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone 226 7232 Fax 226 3803: Blackwell Science Ltd
  • Idioma: Inglês
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