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 et al, 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

Preview

Text Modjaz_2009_ApJ_702_226.pdf - Published Version Download (1MB) | Preview

Abstract

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:	20 Apr 2022 09:24
DOI or ID number:	10.1088/0004-637X/702/1/226
URI:	https://researchonline.ljmu.ac.uk/id/eprint/6488

View Item