Classification of the young population of Monoceros and Tosette molecular clouds

Details Classification of the young population of Monoceros and Tosette molecular clouds Classification of the young population of Monoceros and Tosette molecular clouds

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23...13g&link_type=abstract

Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p. 13-13

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Gregorio-Hetem et al. (1998, A&A 331, 193) published the ROSAT sources detected in Monoceros and Rosette clouds, located respectively at 0.8 and 1.5 Kpc. This work is dedicated to continue the study of young stars associated to giant molecular clouds, showing new results obtained for these star-forming regions. The characteristics of the X-ray sources were compared with those of optical and infrared counterparts showing the same correlations found in young stars. More than 70% of the sources could be compared to the LX x MR distribution presented by the population of Cha 1. It was verified that the Rosette sample could be divided into different categories: OB stars (14%), intermediate-mass Herbig Ae/Be (HAeBe) stars (38%); and T Tauri (TT) stars (17%). A more accurate distribution could be obtained for Monoceros, considering the analysis of the infrared counterparts found in the 2MASS catalog. In this case, the relation log(Cnt/ks) x J was used as an additional criterion to separate the sample in different categories. Most of the Monoceros X-rays sources have near-IR counterparts, which could be classified as OB stars (4%), HAeBes (31%), and TTs (33%). Comparing the population of both clouds, it is found that the presence of low-mass stars is more important in Monoceros, and an opposite result is found concerning the number of massive stars. The ages could be estimated by comparing the X-ray luminosity functions with those of the Cha1 and r Oph clouds. It is found that Monoceros population seems to be older than r Oph, but younger than Cha1. In the other hand, Rosette is younger than r Oph.

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