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Late-time X-Ray, UV and Optical Monitoring of Supernova 1979C | | Stefan Immler
; Robert A. Fesen
; Schuyler D. Van Dyk
; Kurt W. Weiler
; Robert Petre
; Walter H. G. Lewin
; David Pooley
; Wolfgang Pietsch
; Bernd Aschenbach
; Molly C. Hammell
; Gwen C. Rudie
; | | Date: |
30 Mar 2005 | | Journal: | Astrophys.J. 632 (2005) 283-293 | | Subject: | astro-ph | | Abstract: | We present results from observations of SN 1979C with XMM-Newton in X-rays and in the UV, archival X-ray and HST data, and follow-up ground-based optical imaging. The XMM-Newton MOS spectrum shows two-temperature thermal plasma emission characteristics of both the forward (4.1 keV) and reverse shock (0.78 keV) with no intrinsic absorption. The long-term X-ray lightcurve of SN 1979C shows no sign of a decline over 16-23 yrs after its outburst. The high X-ray luminosity (8 x 10^38 ergs/s) is caused by the interaction of the shock with dense circumstellar matter, likely deposited by a strong stellar wind from the progenitor with a high mass-loss rate of 1.5 x 10^-4 M_sun/yr. The X-ray data support a strongly decelerated shock and show a mass-loss rate history which is consistent with a constant progenitor mass-loss rate and wind velocity over the past >16,000 yrs in the evolution of the progenitor. We find a CSM density profile of rho_CSM propto r^-s with index s<1.7 and high CSM densities (>10^4 cm^-3) out to large radii from the site of the explosion (> 4 x 10^17 cm). Using XMM-Newton Optical Monitor data we further detect optical/UV emission from SN 1979C, with B, U, and UVW1-band lum. of 5,7, and 9 x 10^36 ergs/s. The young stellar cluster in the vicinity of the SN, as imaged by the HST and follow-up ground-based optical imaging, can only provide a fraction of the total observed flux, so that a significant contribution to the output likely arises from the strong interaction of SN 1979C with dense CSM. | | Source: | arXiv, astro-ph/0503678 | | Services: | Forum | Review | PDF | Favorites | |
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