Astrophys. J., 554, 734-741 (2001/June-3)
Discovery of X-rays from class 0 protostar candidates in OMC-3.
TSUBOI Y., KOYAMA K., HAMAGUCHI K., TATEMATSU K., SEKIMOTO Y., BALLY J. and REIPURTH B.
Abstract (from CDS):
We have observed the Orion Molecular Clouds 2 and 3 (OMC-2 and OMC-3) with the Chandra X-Ray Observatory (CXO). The northern part of OMC-3 is found to be particularly rich in new X-ray features; four hard X-ray sources are located in and along the filament of cloud cores. Two sources coincide positionally with the submillimeter-millimeter dust condensations of MMS 2 and 3 or an outflow radio source VLA 1, which are in a very early phase of star formation. The X-ray spectra of these sources show an absorption column of (1-3)x1023 H.cm–2. Assuming a moderate temperature plasma, the X-ray luminosity in the 0.5-10 keV band is estimated to be ∼1030 ergs.s–1 at a distance of 450 pc. From the large absorption, positional coincidence, and moderate luminosity, we infer that the hard X-rays are coming from very young stellar objects embedded in the molecular cloud cores.We found another hard X-ray source near the edge of the dust filament. The extremely high absorption of 3x1023 H.cm–2 indicates that the source must be surrounded by dense gas, suggesting that it is either a young stellar object in an early accretion phase or a Type II AGN (e.g., a Seyfert 2), although no counterpart is found at any other wavelength. In contrast to the hard X-ray sources, soft X-ray sources are found spread around the dust filaments, most of which are identified with IR sources in the T Tauri phase.
ISM: individual (OMC-2, OMC-3) - Stars: Coronae - Stars: Flare - Stars: Late-Type - Stars: Pre-Main-Sequence - X-Rays: Stars
Table 1, Fig.1: [TKH2001] NN (Nos 1-13), [TKH2001] a (Nos a-c).
p. 740: H2 flow B and D from 1997ApJ...485L..45Y not in SIMBAD.
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