Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21114702w&link_type=abstract
American Astronomical Society, AAS Meeting #211, #147.02; Bulletin of the American Astronomical Society, Vol. 39, p.999
Astronomy and Astrophysics
Astronomy
1
Scientific paper
Much of the stellar populations inside of the massive star forming regions (MSFRs) are poorly studied in the optical and infrared (IR) wavelengths because of observational challenges caused by large distance, high extinction, and heavy contamination from unrelated sources. To probe the rich intermediate-mass and low-mass young stellar populations accompanying the massive OB stars in each region, we analyzed high resolution Chandra/ACIS images of two massive star forming complexes, namely the NGC 6357 region and the Rosette Complex. A large fraction of the X-ray detections have optical or near-IR stellar counterparts, most of which are previously uncatalogued young cluster members. Normal initial mass functions (IMFs) for NGC 6357 and NGC 2244 were found using the X-ray-sampled young stars nearly complete to solar mass range, inconsistent with the top-heavy IMFs suspected in previous optical studies. The observed X-ray luminosity functions (XLFs) in NGC 6357 and NGC 2244 are compared to the Orion Nebula Cluster XLF to estimate their total cluster populations. The morphologies and structures of the clusters are investigated with absorption-stratified stellar surface density maps. Small-scale substructures superposed on the spherical clusters are found in both NGC 6357 and NGC 2244. The X-ray stars in the Rosette Molecular Cloud show three distinctive structures, which include previously known embedded IR clusters and a new unobscured cluster. The concentration of X-ray identified young stars implies that <35% of stars could be in a distributed population throughout the RMC region and clustered star formation is the dominant mode in this cloud. The observed inner disk fraction in the MSFRs as indicated by K-excess appears lower than the IR-excess disk fractions found in the nearby low-mass star formation regions of similar age, which may be attributed to faster disk dissipation due to photoevaporation in the MSFRs.
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