Type IIP supernova SN 2004et: a multiwavelength study in X-ray, optical and radio |
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| Authors: | Kuntal Misra Dave Pooley † Poonam Chandra D Bhattacharya Alak K Ray Ram Sagar Walter H G Lewin |
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| Institution: | Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital 263129, India;Astronomy Department, University of California at Berkeley, Berkeley, CA 94720, USA;National Radio Astronomy Observatory, Charlottesville, VA 22903, USA;University of Virginia, Charlottesville, VA 22904, USA;Raman Research Institute, Bangalore 560080, India;Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India;Center for Space Research and Department of Physics, Massachusetts Institute of Technology, 70 Vassar Street, Building 37, Cambridge, MA 02139-4307, USA |
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| Abstract: | We present X-ray, broad-band optical and low-frequency radio observations of the bright type IIP supernova SN 2004et. The Chandra X-ray Observatory observed the supernova at three epochs, and the optical coverage spans a period of ～470 d since explosion. The X-ray emission softens with time, and we characterize the X-ray luminosity evolution as L X∝ t ?0.4 . We use the observed X-ray luminosity to estimate a mass-loss rate for the progenitor star of ～2 × 10?6 M⊙ yr?1 . The optical light curve shows a pronounced plateau lasting for about 110 d. Temporal evolution of photospheric radius and colour temperature during the plateau phase is determined by making blackbody fits. We estimate the ejected mass of 56Ni to be 0.06 ± 0.03 M⊙ . Using the expressions of Litvinova & Nadëzhin we estimate an explosion energy of (0.98 ± 0.25) × 1051 erg . We also present a single epoch radio observation of SN 2004et. We compare this with the predictions of the model proposed by Chevalier, Fransson & Nymark. These multiwavelength studies suggest a main-sequence progenitor mass of ～20 M⊙ for SN 2004et. |
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| Keywords: | techniques: photometric supernovae: general supernovae: individual: SN 2004et |
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