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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, Li, W, Butler, N, Chornock, R, Perley, DA, Blondin, S, Bloom, JS, Filippenko, AV, Kirshner, RP, Kocevski, D, Poznanski, D, Hicken, M, Foley, RJ, Stringfellow, GS, Berlind, P, Barrado Y Navascues, D, Blake, CH, Bouy, H, Brown, WR, Challis, P , Chen, H, De Vries, WH, Dufour, P, Falco, E, Friedman, A, Ganeshalingam, M, Garnavich, P, Holden, B, Illingworth, G, Lee, N, Liebert, J, Marion, GH, Olivier, SS, Prochaska, JX, Silverman, JM, Smith, N, Starr, D, Steele, TN, Stockton, A, 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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