Optical and near-infrared coverage of SN 2004et: physical parameters and comparison with other Type IIP supernovae

Kathrina Maguire, E. Di Carlo, Stephen Smartt, Andrea Pastorello, D.Y. Tsvetkov, S. Benetti, S. Spiro, A.A. Arkharov, G. Beccari, Maria Botticella, E. Cappellaro, S. Cristallo, M. Dolci, N. Elias-Rosa, M. Fiaschi, D. Gorshanov, A. Harutyunyan, V.M. Larionov, H. Navasardyan, A. PietrinferniG. Raimondo, G. Di Rico, Stefano Valenti, G. Valentini, L. Zampieri

Research output: Contribution to journalArticlepeer-review

107 Citations (Scopus)


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 56Ni mass of 0.06 +/- 0.04 M-circle dot, 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 1050-1051 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-circle dot implied from 7-8 M-circle dot 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 A line strengths in the nebular spectra of four Type IIP SNe imply ejected oxygen masses of 0.5-1.5 M-circle dot.
Original languageEnglish
Pages (from-to)981-1004
Number of pages24
JournalMonthly Notices of the Royal Astronomical Society
Issue number2
Publication statusPublished - Jan 2010

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics


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