THE CHANDRA CARINA COMPLEX PROJECT VIEW OF TRUMPLER 16
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
- Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 (United States)
- Universitaets-Sternwarte, Ludwig-Maximilians-Universitaet, Scheinerstr. 1, 81679 Muenchen (Germany)
- Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235 (United States)
- Astrophysics Group, College of Engineering, Mathematics, and Physical Sciences, University of Exeter, Exeter EX4 4QL (United Kingdom)
- Departement de Physique, Universite de Montreal, Succursale Centre-Ville, Montreal, QC, H3C 3J7 (Canada)
- Deutsches SOFIA Insitute, University of Stuttgart, Germany and NASA-Ames Research Center (United States)
Trumpler 16 is a well-known rich star cluster containing the eruptive supergiant {eta} Carinae and located in the Carina star-forming complex. In the context of the Chandra Carina Complex Project, we study Trumpler 16 using new and archival X-ray data. A revised X-ray source list of the Trumpler 16 region contains 1232 X-ray sources including 1187 likely Carina members. These are matched to 1047 near-infrared counterparts detected by the HAWK-I instrument at the Very Large Telescope allowing for better selection of cluster members. The cluster is irregular in shape. Although it is roughly circular, there is a high degree of sub-clustering, with no noticeable central concentration and an extension to the southeast. The high-mass stars show neither evidence of mass segregation nor evidence of strong differential extinction. The derived power-law slope of the X-ray luminosity function for Trumpler 16 reveals a much steeper function than the Orion Nebula Cluster, implying a different ratio of solar- to higher-mass stars. We estimate the total Trumpler 16 pre-main-sequence population to be >6500 Class II and Class III X-ray sources. An overall K-excess disk frequency of {approx}8.9% is derived using the X-ray-selected sample, although there is some variation among the sub-clusters, especially in the southeastern extension. X-ray emission is detected from 29 high-mass stars with spectral types between B2 and O3.
- OSTI ID:
- 21560389
- Journal Information:
- Astrophysical Journal, Supplement Series, Vol. 194, Issue 1; Other Information: DOI: 10.1088/0067-0049/194/1/12; ISSN 0067-0049
- Country of Publication:
- United States
- Language:
- English
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