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20 April 2024 |
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Chandra Observation of the Trifid Nebula: X-ray emission from the O star complex and actively forming pre-main sequence stars | | J. Rho
; S. Ramirez
; M.F. Corcoran
; K. Hamaguchi
; B. Lefloch
; | | Date: |
20 Dec 2003 | | Journal: | Astrophys.J. 607 (2004) 904-912 | | Subject: | astro-ph | | Affiliation: | SSC/Caltech), M.F. Corcoran, K. Hamaguchi (NASA/GSFC) and B. Lefloch (LAGO, France | | Abstract: | The Trifid Nebula, a young star-forming HII region, was observed for 16 hours by the Chandra X-ray Observatory. We detected 304 X-ray sources, thirty percent of which are hard sources and seventy percent of of which have near-infrared counterparts. Chandra resolved the HD164492 multiple system into a number of discrete X-ray sources. X-ray emission is detected from components HD164492A (an O7.5III star which ionizes the nebula), B and C (a B6V star), and possibly D (a Be star). HD164492A has a soft spectrum (kT ~ 0.5 keV) while the component C blend shows much harder emission (kT ~ 6 keV). The soft spectrum of the O star is similar to emission seen from other single O stars and is probably produced by shocks within its massive stellar wind. Lack of hard emission suggests that neither a magnetically confined wind shock nor colliding wind emission is important in HD164492A. A dozen stars are found to have flares in the field and most of them are pre-main sequence stars (PMS). Six sources with flares have both optical and 2MASS counterparts. These counterparts are not embedded and thus it is likely that these sources are in a later stage of PMS evolution, possibly Class II or III. Two flare sources did not have any near-IR, optical, or radio counterparts. We suggest these X-ray flare stars are in an early pre-main sequence stage (Class I or earlier). We also detected X-ray sources apparently associated with two massive star forming cores, TC1 and TC4. The spectra of these sources show high extinction and X-ray luminosities of 2 - 5 x 10^{31} erg/s. If these sources are Class 0 objects, it is unclear if their X-ray emission is due to solar-type magnetic activities as in Class I objects, or some other mechanism. | | Source: | arXiv, astro-ph/0401377 | | Services: | Forum | Review | PDF | Favorites | |
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