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From shock breakout to peak and beyond: Extensive panchromatic observations of the type Ib supernova 2008D associated with swift x-ray transient 080109

Modjaz, M and Li, W and Butler, N and Chornock, R and Perley, DA and Blondin, S and Bloom, JS and Filippenko, AV and Kirshner, RP and Kocevski, D and Poznanski, D and Hicken, M and Foley, RJ and Stringfellow, GS and Berlind, P and Barrado Y Navascues, D and Blake, CH and Bouy, H and Brown, WR and Challis, P and Chen, H and De Vries, WH and Dufour, P and Falco, E and Friedman, A and Ganeshalingam, M and Garnavich, P and Holden, B and Illingworth, G and Lee, N and Liebert, J and Marion, GH and Olivier, SS and Prochaska, JX and Silverman, JM and Smith, N and Starr, D and Steele, TN and Stockton, A and Williams, GG and Wood-Vasey, WM (2009) From shock breakout to peak and beyond: Extensive panchromatic observations of the type Ib supernova 2008D associated with swift x-ray transient 080109. The Astrophysical Journal, 702 (1). pp. 226-248. ISSN 1538-4357

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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 150days 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 18days and a modest optical peak luminosity. The early-time light curves of the SN are dominated by a cooling stellar envelope (for Δt0.1-4days, 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 ⊙ of its probable Wolf-Rayet progenitor. According to the model of Waxman etal. and Chevalier & Fransson, we derive R W07⊙ = 1.2 0.7R ⊙ and R CF08⊙ = 12 7 R ⊙, 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. © 2009. The American Astronomical Society. All rights reserved.

Item Type: Article
Uncontrolled Keywords: 0201 Astronomical And Space Sciences, 0305 Organic Chemistry, 0306 Physical Chemistry (Incl. Structural)
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: American Astronomical Society
Date Deposited: 18 May 2017 11:10
Last Modified: 09 Sep 2017 19:20
DOI or Identification number: 10.1088/0004-637X/702/1/226
URI: http://researchonline.ljmu.ac.uk/id/eprint/6488

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