NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-08-18 T14:01:04 PDT
Help | Comment | NED Home

For refcode 2005ApJ...632..283I:
Retrieve 2 NED objects in this reference.
Please click here for ADS abstract

NED Abstract

Copyright by American Astronomical Society. Reproduced by permission
2005ApJ...632..283I 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, and Gwen C. Rudie Abstract. We present results from observations of supernova (SN) 1979C with the Newton X-Ray Multi-Mirror (XMM-Newton) mission in X-rays and in UV, archival X-ray, and Hubble Space Telescope (HST) data, and follow-up ground-based optical imaging. The XMM-Newton MOS spectrum shows the best-fit two-temperature thermal plasma emission characteristics of both the forward (kT_high_=4.1^+76^_-2.4_ keV) and reverse shock (kT_low_=0.79^+0.24^_-0.17_ keV) with no intrinsic absorption. The long-term X-ray light curve, constructed from all X-ray data available, reveals that SN 1979C is still radiating at a flux level similar to that detected by ROSAT in 1995, showing no sign of a decline over the last 6 years, some 16 -- 23 yr after its outburst. The high inferred X-ray luminosity (L_0.3 -- 2_=8x10^38^ergs s^-1^) is caused by the interaction of the SN shock with dense circumstellar matter, likely deposited by a strong stellar wind from the progenitor with a high mass-loss rate of M^dot^~1.5x10^-4^M_sun_yr^-1^(v_w_/10kms^-1^). The X-ray data support a strongly decelerated shock and show a mass-loss rate history that is consistent with a constant progenitor mass-loss rate and wind velocity over the past >~16,000 yr in the stellar evolution of the progenitor. We find a best-fit circumstellar medium (CSM) density profile of {rho}_CSM_ is proportional to 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 (r>~4x10^17^cm). Using XMM-Newton Optical Monitor data, we further detect a pointlike optical/UV source consistent with the position of SN 1979C, with B-, U-, and UVW1-band luminosities of 5, 7, and 9x10^36^ergss^-1^, respectively. 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. Key words: Stars: Circumstellar Matter, Galaxies: Individual: M100, Galaxies: Individual: NGC 4321, Stars: Supernovae: Individual: SN 1979C, Ultraviolet: ISM, X-Rays: General, X-rays: individual (M100), X-rays: individual (NGC 4321), X-rays: individual (SN 1979C), X-Rays: ISM
Retrieve 2 NED objects in this reference.
Please click here for ADS abstract

Back to NED Home