Bibcode
Modjaz, M.; Li, W.; Butler, N.; Chornock, R.; Perley, D.; Blondin, S.; Bloom, J. S.; Filippenko, A. V.; Kirshner, R. P.; Kocevski, D.; Poznanski, D.; Hicken, M.; Foley, R. J.; Stringfellow, G. S.; Berlind, P.; Barrado y Navascues, D.; Blake, C. H.; Bouy, H.; Brown, W. R.; Challis, P.; Chen, H.; de Vries, W. H.; Dufour, P.; Falco, E.; Friedman, A.; Ganeshalingam, M.; Garnavich, P.; Holden, B.; Illingworth, G.; Lee, N.; Liebert, J.; Marion, G. H.; Olivier, S. S.; Prochaska, J. X.; Silverman, J. M.; Smith, N.; Starr, D.; Steele, T. N.; Stockton, A.; Williams, G. G.; Wood-Vasey, W. M.
Bibliographical reference
The Astrophysical Journal, Volume 702, Issue 1, pp. 226-248 (2009).
Advertised on:
9
2009
Journal
Citations
255
Refereed citations
230
Description
We present extensive early photometric (ultraviolet through
near-infrared) and spectroscopic (optical and near-infrared) data on
supernova (SN) 2008D as well as X-ray data analysis on the associated
Swift X-ray transient (XRT) 080109. Our data span a time range of 5 hr
before the detection of the X-ray transient to 150 days after its
detection, and a detailed analysis allowed us to derive constraints on
the nature of the SN and its progenitor; throughout we draw comparisons
with results presented in the literature and find several key aspects
that differ. We show that the X-ray spectrum of XRT 080109 can be fit
equally well by an absorbed power law or a superposition of about equal
parts of both power law and blackbody. Our data first established that
SN 2008D is a spectroscopically normal SN Ib (i.e., showing conspicuous
He lines) and showed that SN 2008D had a relatively long rise time of 18
days and a modest optical peak luminosity. The early-time light curves
of the SN are dominated by a cooling stellar envelope (for
Δt≈0.1-4 days, most pronounced in the blue bands) followed by
56Ni decay. We construct a reliable measurement of the
bolometric output for this stripped-envelope SN, and, combined with
estimates of E K and M ej from the literature,
estimate the stellar radius R sstarf of its probable
Wolf-Rayet progenitor. According to the model of Waxman et al. and
Chevalier & Fransson, we derive R W07 sstarf =
1.2 ± 0.7R sun and R CF08 sstarf
= 12 ± 7 R sun, respectively; the latter being more in
line with typical WN stars. Spectra obtained at three and four months
after maximum light show double-peaked oxygen lines that we associate
with departures from spherical symmetry, as has been suggested for the
inner ejecta of a number of SN Ib cores.