Supernova 2006aj and the associated X-Ray Flash 060218

Sollerman, J.; Jaunsen, A. O.; Fynbo, J. P. U.; Hjorth, J.; Jakobsson, P.; Stritzinger, M. D.; Féron, Christophe; Laursen, Peter; Ovaldsen, J. E.; Selj, Josefine; Thöne, C. C.; Xu, D.; Davis, Tamara M.; Gorosabel, J.; Watson, Derrick G.; Duro, Refiz; Ilyin, I.; Jensen, B. L.; Lysfjord, N.; Marquart, Thomas; Nielsen, T. B.; Näränen, Jyri; Schwarz, H. E.; Walch, Stefanie; Wold, M.; Östlin, Göran

doi:10.1051/0004-6361:20065226

Cited by 159 publications

(172 citation statements)

References 45 publications

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“…It was observed by the Chandra satellite on February 26.78 and March 7.55 UT (t 8.8 and 17.4 days) for 20 and 30 ks respectively (Soderberg et al 2006b). The spectroscopic redshift was z = 0.033 (Sollerman et al 2006;Mirabal et al 2006). The corresponding isotropic equivalent energy is E iso = (1.9 ± 0.1) × 10 49 erg (Sakamoto et al 2006) which sets this GRB as having a low luminosity, consistent with most of the GRBs associated with SNe (Liang et al 2006b;Cobb et al 2006;Guetta & Della Valle 2007).…”

Section: Grb 060218 -Sn2006ajmentioning

confidence: 80%

“…The host galaxy of SN2006aj is a low luminosity, metal-poor star-forming dwarf galaxy (Ferrero et al 2006) with an irregular morphology (Wiersema et al 2007), similar to those of other GRBs associated with SNe (Modjaz et al 2006;Sollerman et al 2006).…”

Section: Grb 060218 -Sn2006ajmentioning

confidence: 96%

“…GRB 060218, discovered by the Swift satellite with cosmological redshift z = 0.033 (Mirabal et al 2006;Sollerman et al 2006), is the best example of a Gamma-Ray Burst (GRB) associated with a Supernova (SN) Ib/c (Campana et al 2006). Its extremely long duration is unusual, with the longest T 90 ever observed (T 90 ∼ 2100 s).…”

Section: Introductionmentioning

confidence: 99%

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GRB 060218 and GRBs associated with supernovae Ib/c

Dainotti¹,

Bernardini²,

Bianco³

et al. 2007

A&A

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Context. The Swift satellite has given continuous data in the range 0.3-150 keV from 0 s to 10 6 s for GRB 060218 associated with SN2006aj. This Gamma-Ray Burst (GRB) which has an unusually long duration (T 90 ∼ 2100 s) fulfills the Amati relation. These data offer the opportunity to probe theoretical models for GRBs connected with Supernovae (SNe). Aims. We plan to fit the complete γ-and X-ray light curves of this long duration GRB, including the prompt emission, in order to clarify the nature of the progenitors and the astrophysical scenario of the class of GRBs associated with SNe Ib/c. Methods. We apply our "fireshell" model based on the formation of a black hole, giving the relevant references. It is characterized by the precise equations of motion and equitemporal surfaces and by the role of thermal emission. Results. The initial total energy of the electron-positron plasma E tot e ± = 2.32 × 10 50 erg has a particularly low value, similar to the other GRBs associated with SNe. For the first time, we observe a baryon loading B = 10 −2 which coincides with the upper limit for the dynamical stability of the fireshell. The effective CircumBurst Medium (CBM) density shows a radial dependence n cbm ∝ r −α with 1.0 < ∼ α < ∼ 1.7 and monotonically decreases from 1 to 10 −6 particles/cm 3 . This behavior is interpreted as being due to a fragmentation in the fireshell. Analogies with the fragmented density and filling factor characterizing Novae are outlined. The fit presented is particularly significant in view of the complete data set available for GRB 060218 and of the fact that it fulfills the Amati relation. Conclusions. We fit GRB 060218, usually considered as an X-Ray Flash (XRF), as a "canonical GRB" within our theoretical model. The smallest possible black hole, formed by the gravitational collapse of a neutron star in a binary system, is consistent with the especially low energetics of the class of GRBs associated with SNe Ib/c. We provide the first evidence for a fragmentation in the fireshell. This fragmentation is crucial in explaining both the unusually large T 90 and the consequently inferred abnormally low value of the CBM effective density.

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Section: Grb 060218 -Sn2006ajmentioning

confidence: 80%

Section: Grb 060218 -Sn2006ajmentioning

confidence: 96%

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GRB 060218 and GRBs associated with supernovae Ib/c

Dainotti¹,

Bernardini²,

Bianco³

et al. 2007

A&A

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“…SN 2006aj, a SN Ic-BL associated with an X-ray flash (e.g., Sollerman et al 2006), also showed a double peak. 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).…”

Section: Introductionmentioning

confidence: 99%

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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“…The five most solid cases of the SN-GRB connection, with high signal-to-noise and multiple spectra, are usually at low z : SN1998bw/GRB980425 at z = 0.0085 (Galama et al 1998), SN2003dh/GRB030329 at z = 0.1685 (Stanek et al 2003;Hjorth et al 2003;Matheson et al 2003), SN2003lw/GRB031203 at z = 0.10058 (Malesani et al 2004), SN2006aj/GRB060218 at z = 0.0335 (Campana et al 2006;Modjaz et al 2006;Pian et al 2006;Sollerman et al 2006;Mirabal et al 2006;Cobb et al 2006;Kocevski et al 2007), and most recently, SN2010bh/GRB100316D at z = 0.0593 Starling et al 2011), where the SN spectra lines were visible as early as 2 days after the GRB . Two special SNe, SNe 2008D and2009bb, and the potential presence of a jet in them will be discussed below.…”

Section: Solid Cases Of Sn-grb: Sne Ic-bl With Grbsmentioning

confidence: 99%

Stellar Forensics with the Supernova‐GRB Connection

Modjaz¹

2011

Reviews in Modern Astronomy

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Long-duration gamma-ray bursts (GRBs) and Type Ib/c Supernovae (SNe Ib/c) are amongst nature's most magnificent explosions. While GRBs launch relativistic jets, SNe Ib/c are core-collapse explosions whose progenitors have been stripped of their hydrogen and helium envelopes. Yet for over a decade, one of the key outstanding questions is which conditions lead to each kind of explosion and death in massive stars. Determining the fates of massive stars is not only a vibrant topic in itself, but also impacts using GRBs as star formation indicators over distances of up to 13 billion light-years and for mapping the chemical enrichment history of the universe. This article reviews a number of comprehensive observational studies that probe the progenitor environments, their metallicities and the explosion geometries of SN with and without GRBs, as well as the emerging field of SN environmental studies. Furthermore, it discusses SN 2008D/XRT 080109 which was discovered serendipitously with the Swift satellite via its X-ray emission from shock breakout, and which has generated great interest amongst both observers and theorists while illustrating a novel technique for stellar forensics. The article concludes with an outlook on how the most promising venues of research -with the many existing and upcoming large-scale surveys such as the Palomar Transient Factory and LSST -will shed new light on the diverse deaths of massive stars.

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Supernova 2006aj and the associated X-Ray Flash 060218

Cited by 159 publications

References 45 publications

GRB 060218 and GRBs associated with supernovae Ib/c

GRB 060218 and GRBs associated with supernovae Ib/c

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

Stellar Forensics with the Supernova‐GRB Connection

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