FROM SHOCK BREAKOUT TO PEAK AND BEYOND: EXTENSIVE PANCHROMATIC OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH SWIFT X-RAY TRANSIENT 080109

By Maryam Modjaz, W. Li, N. Butler, Ryan Chornock, D. Perley, S. Blondin, Joshua S. Bloom, A. Filippenko, R. Kirshner, D. Kocevski and 31 more. 2008

203 citations recorded by the source corpus.

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 EK and Mej from the literature, estimate the stellar radius R⋆ of its probable Wolf–Rayet progenitor. According to the model of Waxman et al. and Chevalier & Fransson, we derive RW07⋆ = 1.2 ± 0.7R☉ and RCF08⋆ = 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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0758cb16dc877c046c6bc17c9439c29c2f737138

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The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. E. Berger
2. B. Metzger
3. S. Smartt
4. Stan Woosley
5. N. Smith
6. A. Filippenko
7. Bing Zhang
8. Ryan Chornock

In Nuclear and High Energy Physics

1. E. Berger
2. B. Metzger
3. S. Smartt
4. Ryan Chornock
5. Stan Woosley
6. A. Filippenko
7. Weidong Li
8. E. Nakar

Citations in the corpus

• THE EARLY UV/OPTICAL EMISSION FROM CORE-COLLAPSE SUPERNOVAE (2010, methodology): “The photospheric velocity predicted by our model is consistent with the velocities inferred from spec- 17 tral analyses (Mazzali et al. 2008; Modjaz et al. 2009; Tanaka et al. 2009), see fig.”
• TYPE Ib/c SUPERNOVAE IN BINARY SYSTEMS. I. EVOLUTION AND PROPERTIES OF THE PROGENITOR STARS (2010, background): “…of the X-ray outburst with SN 2008D by Soderberg et al. (2008) indeed suggests the usefulness of such a study for the probe of supernova progenitors (e.g. Soderberg et al. 2008; Chevalier & Fransson 2008; Xu, Zou & Fan 2008; Modjaz et al. 2009), for which our new models would provide ideal input.”
• THE ULTRAVIOLET-BRIGHT, SLOWLY DECLINING TRANSIENT PS1-11af AS A PARTIAL TIDAL DISRUPTION EVENT (2013, background): “This is true for objects ranging from normal SNe II (e.g., Leonard et al. 2002) and Ib/c (Soderberg et al. 2008; Modjaz et al. 2009) to the SN IIn 2007pk (Pritchard et al. 2012) and even SLSNe (Miller et al. 2009; Gezari et al. 2009a; Quimby et al. 2011; Chomiuk et al. 2011; Lunnan et al. 2013;…”
• Core-collapse explosions of Wolf–Rayet stars and the connection to Type IIb/Ib/Ic supernovae (2011, background): “SN 2008D was caught as the shock broke out of the progenitor star (Soderberg et al. 2008; Chevalier & Fransso2008; Modjaz et al. 2009).”
• Nearby Supernova Rates from the Lick Observatory Supernova Search. II. The Observed Luminosity Functions and Fractions of Supernovae in a Complete Sample (2010, background): “This doublepeak light curve behaviour has most recently also been seen in the Type Ib SN 2008D (Soderberg et al. 2008; Modjaz et al. 2009).”
• THE SPECTROSCOPIC DIVERSITY OF TYPE Ia SUPERNOVAE (2000, background): “…to follow up peculiar objects) (2) bright Type Ib/c supernovae, to study both individual objects (e.g., SN 2006aj, Modjaz et al. 2006; SN 2008D, Modjaz et al. 2009) and the connection of broad-line SN Ic with gamma-ray bursts (e.g., Modjaz et al. 2008), and (3) bright Type IIP supernovae…”
• ULTRA-BRIGHT OPTICAL TRANSIENTS ARE LINKED WITH TYPE Ic SUPERNOVAE (2010, background): “Interestingly, Modjaz et al. (2009) noted a shortlife “W” feature in a very early spectrum of the type Ib SN 2008D.”
• OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, methodology): “…of the following SNe were published as single objects: SN 1994I (Millard et al. 1999), 1997ef (Iwamoto et al. 2000), 2000H (Branch et al. 2002), 2003jd (Valenti et al. 2008a), 2005bf (Tominaga et al. 2005; Modjaz et al. 2008b), 2006aj (Modjaz et al. 2006, 2008b), and 2008D (Modjaz et al. 2009).”
• On the nature of supernovae Ib and Ic (2012, background): “…(left-hand panel), we show a comparison of the heavily mixed model Bmf5p1x4 at 10.3 d after explosion with the observations of the Type Ib SN2008D (Modjaz et al. 2009) on 2008 February 2, which corresponds to 23.88 d after the X-ray detection (we choose a time when the model matches both the…”
• SEEING THE COLLISION OF A SUPERNOVA WITH ITS COMPANION STAR (2009, background): “The early shock luminosity phase, however, has been observed in several events, e.g., SN 1987A (Arnett et al. 1989) and SN 1993J (Wheeler et al. 1993) while the shock breakout itself was caught for SN 2008D (Soderberg et al. 2008; Modjaz et al. 2009).”
• The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, background): “Further discussion on the effects of including additional filters when constructing a bolometric LC of a given SN can be found in [30, 41, 49, 120, 123], who show that including NIR flux leads to brighter bolometric LCs that decay slower at later times and including UV flux leads to an increase in l”
• On the diversity of superluminous supernovae: ejected mass as the dominant factor (2015, unknown): “…Valenti et al. (2008a) SN2004aw Ic −17.24 Taubenberger et al. (2006) SN2007gr Ic −16.36 Valenti et al. (2008b) SN2008D Ib −16.24 Soderberg et al. (2008), Modjaz et al. (2009) SN2009jf Ic −17.34 Valenti et al. (2011) SN2010bh IcBLa −16.97 Cano et al. (2011) SN2011bm Ic −17.63 Valenti et al.…”
• Rates of superluminous supernovae at z ∼ 0.2 (2013, background): “Other supernovae with more normal peak luminosities may also display such features at very early times, but these quickly disappear as the ejecta cool and oxygen recombines (cf. c© — RAS, MNRAS 000, 1 - ?? the spectral series of SN2008D presented by Modjaz et al. 2009).”
• AN r-PROCESS KILONOVA ASSOCIATED WITH THE SHORT-HARD GRB 130603B (2013, background): “Indeed, only SN 2008D had comparable observed absolute magnitudes,MB ≈−13.4 mag andMJ ≈ −15.6 mag (Soderberg et al. 2008; Modjaz et al. 2009), but this supernova was heavily reddened, withE(B − V ) ≈ 0.6 mag (Soderberg et al. 2008).”