XRF 100316D/SN 2010bh AND THE NATURE OF GAMMA-RAY BURST SUPERNOVAE

Cano, Z.; Bersier, D.; Guidorzi, C.; Kobayashi, Shinya; Levan, A. J.; Tanvir, N. R.; Wiersema, K.; D’Avanzo, P.; Fruchter, A. S.; Garnavich, P.; Gomboc, A.; Gorosabel, J.; Kasen, Daniel; Kopač, D.; Margutti, R.; Mazzali, P. A.; Melandri, A.; Mundell, C. G.; Nugent, P.; Pian, E.; Smith, R. J.; Steele, I. A.; Wijers, R. A. M. J.; Woosley, S. E.

doi:10.1088/0004-637x/740/1/41

Cited by 100 publications

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“…Only a handful of such low luminosity events have been identified in the past decade, all of which have been relatively local (given the difficulty in observing low luminosity bursts beyond z ∼ 0.1). These include the well studied GRBsupernova pairs GRB 980425/SN 1998bw (Galama et al 1998), GRB 031203/SN 2003lw (Malesani et al 2004;Soderberg et al 2004), GRB 060218/SN 2006aj (Pian et al 2006) and GRB 100316D/SN 2010bh (Starling et al 2011;Cano et al 2011), and the enigmatic GRBs 060505 and 060614, where associated SNe have been ruled out to deep limits, and whose origin remains mysterious (Fynbo et al 2006;Della Valle et al 2006). They may be low luminosity events akin to those above, but where the SNe is absent (e.g.…”

Section: Burst Propertiesmentioning

confidence: 99%

GRB 080517: a local, low-luminosity gamma-ray burst in a dusty galaxy at z = 0.09

Stanway¹,

Levan²,

Tanvir³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the photometry and spectroscopy of the host galaxy of Swift-detected GRB 080517. From our optical spectroscopy, we identify a redshift of z = 0.089 ± 0.003, based on strong emission lines, making this a rare example of a very local, low luminosity, long gamma ray burst. The galaxy is detected in the radio with a flux density of S 4.5 GHz =0.22±0.04 mJy -one of relatively few known GRB hosts with a securely measured radio flux. Both optical emission lines and a strong detection at 22µm suggest that the host galaxy is forming stars rapidly, with an inferred star formation rate ∼ 16 M ⊙ yr −1 and a high dust obscuration (E(B − V ) > 1, based on sight-lines to the nebular emission regions). The presence of a companion galaxy within a projected distance of 25 kpc, and almost identical in redshift, suggests that star formation may have been triggered by galaxy-galaxy interaction. However, fitting of the remarkably flat spectral energy distribution from the ultraviolet through to the infrared suggests that an older, 500 Myr post-starburst stellar population is present along with the ongoing star formation. We conclude that the host galaxy of GRB 080517 is a valuable addition to the still very small sample of well-studied local gamma-ray burst hosts.

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Section: Burst Propertiesmentioning

confidence: 99%

GRB 080517: a local, low-luminosity gamma-ray burst in a dusty galaxy at z = 0.09

Stanway¹,

Levan²,

Tanvir³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…The early maximum was interpreted as being due to the presence of an extended envelope formed by a dense wind (Campana et al 2006;Waxman et al 2007;Irwin & Chevalier 2016). Similar to SN 2006aj, the GRB-SN 2010bh also exhibited an early peak (Cano et al 2011). The shock break-out through an extended and low-mass envelope could power the early peak (Margutti et al 2015;Nakar 2015).…”

Section: Introductionmentioning

confidence: 98%

iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor

Taddia

Fremling

Sollerman

et al. 2016

A&A

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Context. Type Ic supernovae (SNe Ic) arise from the core-collapse of H-(and He-) poor stars, which could either be single Wolf-Rayet (WR) stars or lower-mass stars stripped of their envelope by a companion. Their light curves are radioactively powered and usually show a fast rise to peak (∼10−15 d), without any early (in the first few days) emission bumps (with the exception of broad-lined SNe Ic) as sometimes seen for other types of stripped-envelope SNe (e.g., Type IIb SN 1993J and Type Ib SN 2008D). Aims. We have studied iPTF15dtg, a spectroscopically normal SN Ic with an early excess in the optical light curves followed by a long (∼30 d) rise to the main peak. It is the first spectroscopically-normal double-peaked SN Ic to be observed. Our aim is to determine the properties of this explosion and of its progenitor star. Methods. Optical photometry and spectroscopy of iPTF15dtg was obtained with multiple telescopes. The resulting light curves and spectral sequence are analyzed and modeled with hydrodynamical and analytical models, with particular focus on the early emission. Results. iPTF15dtg is a slow rising SN Ic, similar to SN 2011bm. Hydrodynamical modeling of the bolometric properties reveals a large ejecta mass (∼10 M ) and strong 56 Ni mixing. The luminous early emission can be reproduced if we account for the presence of an extended ( 500 R ), low-mass ( 0.045 M ) envelope around the progenitor star. Alternative scenarios for the early peak, such as the interaction with a companion, a shock-breakout (SBO) cooling tail from the progenitor surface, or a magnetar-driven SBO are not favored. Conclusions. The large ejecta mass and the presence of H-and He-free extended material around the star suggest that the progenitor of iPTF15dtg was a massive ( 35 M ) WR star that experienced strong mass loss.

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“…For the case of the association SN 2010bh/XRF 100316D, GROND provided data from 0.5 to 80 days after the burst covering a wavelength range from 350 to 1800 nm, significantly expanding the pre-existing data set for this event (e.g., Cano et al 2011). …”

Section: Introductionmentioning

confidence: 99%