期刊
ASTRONOMY & ASTROPHYSICS
卷 413, 期 1, 页码 107-119出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361:20031506
关键词
galaxies : individual : M 74; galaxies : spiral; supernovae : individual : SN 2002ap; X-rays : binaries; X-rays : galaxies
We have re-observed the field of M74 in January 2003 with XMM-Newton, 11 months after the X-ray detection of SN 2002ap. From a comparison of the two XMM-Newton observations we obtain more accurate values for the X-ray luminosity and colours of the source five days after the event, and a limit on its decline rate. We compare its X-ray behaviour (prompt soft Xray emission, relatively low luminosity) with that of other type Ic SNe, and speculate that SN 2002ap may share some physical properties (low mass-loss rate and high-velocity stellar wind from the progenitor star) with the candidate hypernova/gamma-ray-burst progenitor SN 1998bw, but with a lower (non-relativistic) speed of the ejecta. We suggest that the X-ray emission observed in 2002 is likely to come from the radiatively-cooling reverse shock, at a temperature kT approximate to 0.8 keV, and that this soft component was already detected 5 d after the event because the absorbing column density of the cool shell between the forward and reverse shocks was only similar to10(20) cm(-2), i.e., the shell was optically thin in the soft X-ray band. The new XMM-Newton data also allowed us to continue monitoring two bright variable sources in M74 that had reached peak luminosities > 10(39) erg s(-1) in previous XMM-Newton and Chandra observations. Finally, we used two Chandra observations from 2001 to investigate the luminosity and colour distribution of the X-ray source population of M74, typical of moderately-active late-type spirals.
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