Volume 557, September 2013
|Number of page(s)||12|
|Section||Galactic structure, stellar clusters and populations|
|Published online||20 August 2013|
Young stellar clusters in the Rosette molecular cloud
Arguments against triggered star formation⋆,⋆⋆
1 Observatoire astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR 7550, 11 rue de l’Université, 67000 Strasbourg, France
2 Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Konkoly Thege 15-17, 1121 Budapest, Hungary
3 Eötvös Loránd University, Department of Astronomy, Pázmány Péter sétány 1/A, 1117 Budapest, Hungary
4 Laboratoire d’Astrophysique de Bordeaux, CNRS/INSU, Université de Bordeaux, BP 89, 33271 Floirac Cedex, France
Received: 5 February 2013
Accepted: 15 July 2013
Aims. We focus on characterizing the young stellar population in the Rosette complex to improve our understanding of the processes that regulate the star formation in this region.
Methods. We propose an original method that relies on the joint analysis of the star color and density in the near-infrared. It leads to mapping the molecular cloud spatial distribution and detecting the embedded clusters with their characterization in terms of member number and age estimation.
Results. We have identified 13 clusters, 2 of which are new discoveries, and we estimate that the total number of young stellar objects in the Rosette ranges between 4000 and 8000 members. We find that the age distribution of the young clusters is not consistent with a general triggered scenario for the star formation in this molecular cloud.
Conclusions. This study proves that the Rosette complex evolution is not governed by the influence of its OB star population. It suggests that the simple morphological appearance of an active region is not sufficient to conclude much about the triggering role in the star formation process. Our method of constraining the cluster properties using UKIDSS and WISE data has proven efficient, and studies of other regions of the Galactic plane would definitely benefit from this approach.
Key words: stars: pre-main sequence / dust, extinction / infrared: general / ISM: individual objects: Rosette molecular cloud
Appendix A is available in electronic form at http://www.aanda.org
Full Table 4 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/557/A29
© ESO, 2013
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