Maguire, K. and Di Carlo, E. and Smartt, S. J. and Pastorello, A. and Tsvetkov, D. Yu. and Benetti, S. and Spiro, S. and Arkharov, A. A. and Beccari, G. and Botticella, M. T. and Cappellaro, E. and Cristallo, S. and Dolci, M. and Elias-Rosa, N. and Fiaschi, M. and Gorshanov, D. and Harutyunyan, A. and Larionov, V. M. and Navasardyan, H. and Pietrinferni, A. and Raimondo, G. and Di Rico, G. and Valenti, S. and Valentini, G. and Zampieri, L. (2010) Optical and near-infrared coverage of SN 2004et: physical parameters and comparison with other Type IIP supernovae. Monthly Notices of the Royal Astronomical Society, 404 (2). pp. 981-1004. ISSN 0035-8711 http://resolver.caltech.edu/CaltechAUTHORS:20100611-073852990
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We present new optical and near-infrared (NIR) photometry and spectroscopy of the Type IIP supernova (SN), SN 2004et. In combination with already published data, this provides one of the most complete studies of optical and NIR data for any Type IIP SN from just after explosion to +500 d. The contribution of the NIR flux to the bolometric light curve is estimated to increase from 15 per cent at explosion to around 50 per cent at the end of the plateau and then declines to 40 per cent at 300 d. SN 2004et is one of the most luminous IIP SNe which has been well studied and characterized, and with a luminosity of log L= 42.3 erg s^(−1) and a ^(56)Ni mass of 0.06 ± 0.04 M_⊙, it is two times brighter than SN 1999em. We provide parametrized bolometric corrections as a function of time since explosion for SN 2004et and three other IIP SNe that have extensive optical and NIR data. These can be used as templates for future events in optical and NIR surveys without full wavelength coverage. We compare the physical parameters of SN 2004et with those of other well-studied IIP SNe and find that the kinetic energies span a range of 10^(50)–10^(51) erg. We compare the ejected masses calculated from hydrodynamic models with the progenitor masses and limits derived from pre-discovery images. Some of the ejected mass estimates are significantly higher than the progenitor mass estimates, with SN 2004et showing perhaps the most serious mass discrepancy. With the current models, it appears difficult to reconcile 100 d plateau lengths and high expansion velocities with the low ejected masses of 5–6 M_⊙ implied from 7–8 M_⊙ progenitors. The nebular phase is studied using very late-time Hubble Space Telescope photometry, along with optical and NIR spectroscopy. The light curve shows a clear flattening at 600 d in the optical and the NIR, which is likely due to the ejecta impacting on circumstellar material. We further show that the [O i] 6300, 6364 Å line strengths in the nebular spectra of four Type IIP SNe imply ejected oxygen masses of 0.5–1.5 M_⊙.
|Additional Information:||© 2010 The Authors. Journal compilation © 2010 RAS. Accepted 2010 January 11. Received 2010 January 8; in original form 2009 December 10. Published Online: 2 Mar 2010. This work, conducted as part of the award ‘Understanding the lives of massive stars from birth to supernovae’ (S. J. Smartt) made under the European Heads of Research Councils and European Science Foundation EURYI (European Young Investigator) Awards scheme, was supported by funds from the Participating Organizations of EURYI and the EC Sixth Framework Programme. SB and EC acknowledge some support from contract ASI/COFIS. We thank Nikolai Chugai andMelina Bersten for helpful discussions on progenitor models and Vallery Stanishev for the earliest spectrum of SN 2006my. We thank the referee, David Branch, for comments that improved the manuscript. This paper is based on observations made with the following facilities: the 1.82-m Copernico Telescope of the Asiago Observatory (Asiago), the 3.58-m Italian National Telescope Galileo operated by the Fundacin Galileo Galilei of the INAF (La Palma), the 0.72-m TNT telescope of the Teramo Astronomical Observatory (Teramo), the 2.6-m NOT (La Palma), 0.7-m AZT2 telescope of the Sternberg Astronomical Institute (Moscow), 0.6-m Z600 telescope of the Crimean Observatory of SAI (Crimea), the 0.38-m KGB telescope at the Crimean Astrophysical Observatory (Crimea) and the 1-m SAO Z1000 telescope of the Russian Academy of Sciences (Zelenchuk). NIR data were collected with the AZT-24 telescope (Campo Imperatore, Italy), operated jointly by Pulkovo Observatory (St. Petersburg, Russia) and INAF Observatorio Astronomico di Roma/Collurania. Observations were also used from NASA/ESA HST, obtained from the data archive at the Space Telescope Institute. STScI is operated by the association of Universities for Research in Astronomy, Inc., under the NASA contract NAS 5-26555.|
|Subject Keywords:||supernovae: general; supernovae: individual: 2004et; supernovae: individual: 2004A; supernovae: individual: 2006my.|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||11 Jun 2010 21:43|
|Last Modified:||26 Dec 2012 12:08|
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