Soria 2004 XMM-Newton 对SN2002ap的观测

主要内容:


精彩摘抄:


文章信息:

· Electronic Refereed Journal Article (HTML)

· Full Refereed Journal Article (PDF/Postscript)

· arXiv e-print (arXiv:astro-ph/0304526)

· On-line Data

· References in the article

· Citations to the Article (9) (Citation History)

· Refereed Citations to the Article

· SIMBAD Objects (17)

· NED Objects (82)

· Also-Read Articles (Reads History)

·

· Translate This Page

Title:		A second glance at SN 2002ap and the M 74 field with XMM-Newton
Authors:		Soria, R.; Pian, E.; Mazzali, P. A.
Affiliation:		AA(Mullard Space Science Laboratory, University College London, Holmbury St Mary, Surrey RH5 6NT, UK Roberto.Soria@mssl.ucl.ac.uk), AB(INAF, Osservatorio Astronomico di Trieste, via Tiepolo 11, I-34131 Trieste, Italy pian@ts.astro.it), AC(INAF, Osservatorio Astronomico di Trieste, via Tiepolo 11, I-34131 Trieste, Italy mazzali@ts.astro.it)
Publication:		Astronomy and Astrophysics, v.413, p.107-119 (2004) (A&A Homepage)
Publication Date:		01/2004
Origin:		A&A
A&A Keywords:		galaxies: individual: M 74, galaxies: spiral, supernovae: individual: SN 2002ap, X-rays: binaries, \ X-rays: galaxies
DOI:		10.1051/0004-6361:20031506
Bibliographic Code:		2004A&A...413..107S

Abstract

We have re-observed the field of M 74 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 X-ray 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 ≈ 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 ˜ 10²⁰ 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 M 74 that had reached peak luminosities > 10³⁹ 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 M 74, typical of moderately-active late-type spirals.

---

Bibtex entry for this abstract Preferred format for this abstract (see Preferences)