Prompt and Afterglow Emission Properties of Gamma‐Ray Bursts with Spectroscopically Identified Supernovae

Kaneko, Yuki; Ramírez-Ruiz, E.; Granot, Jonathan; Kouveliotou, C.; Woosley, S. E.; Patel, S.; Rol, E.; Zand, J. J. M. in ’t; Horst, A. J. van der; Wijers, R. A. M. J.; Strom, R. G.

doi:10.1086/508324

Cited by 99 publications

(136 citation statements)

References 88 publications

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“…The Lorentz gamma factor, obtained solving the fireshell equations of motion (Bianco & Ruffini 2005a,b), is γ • = 99.2 at the beginning of the afterglow phase at a distance from the progenitor r • = 7.82 × 10 12 cm. It is much larger than γ ∼ 5 estimated by Kaneko et al (2006) and Toma et al (2006).…”

Section: The Fit Of the Observed Datacontrasting

confidence: 52%

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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: The Fit Of the Observed Datacontrasting

confidence: 52%

“…This same point recently received strong observational support in the case of GRB 060218 (Liang et al 2006a) and a consensus by other models in the literature (Kaneko et al 2006). …”

Section: Discussionmentioning

confidence: 52%

GRB 060218 and GRBs associated with supernovae Ib/c

Dainotti¹,

Bernardini²,

Bianco³

et al. 2007

A&A

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“…In this respect, its profile is similar to that of low luminosity GRBs 031203 and 980425 (Kaneko et al 2007), although the profile is not unusual amongst GRBs more generally (Fenimore, Madras, & Nayakshin 1996).…”

Section: Burst Propertiesmentioning

confidence: 54%

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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“…The large-angle SN outflow, responsible for exploding the star and producing the 56 Ni, would generally carry more energy and inertia than the relativistic jet itself (e.g., Soberberg et al 2004;Mazzali et al 2006;Kaneko et al 2007), so that the latter always overtakes it, and sweeps up the GRB ejecta. It is to this problem that we now turn our attention.…”

Section: Evolution In a Circumstellar Wind Mediummentioning

confidence: 99%

The Hydrodynamics of Gamma-Ray Burst Remnants

Ramírez-Ruiz

MacFadyen

2010

ApJ

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This paper reports on the results of a numerical investigation designed to address how the initially anisotropic appearance of a GRB remnant is modified by the character of the circumburst medium and by the possible presence of an accompanying supernova (SN). Axisymmetric hydrodynamical calculations of light, impulsive jets propagating in both uniform and inhomogeneous external media are presented, which show that the resulting dynamics of their remnants since the onset of the non-relativistic phase is different from the standard selfsimilar solutions. Because massive star progenitors are expected to have their close-in surroundings modified by the progenitor winds, we consider both free winds and shocked winds as possible external media for GRB remnant evolution. Abundant confirmation is provided here of the important notion that the morphology and visibility of GRB remnants are determined largely by their circumstellar environments. For this reason, their detectability is highly biased in favor of those with massive star progenitors; although, in this class of models, the beamed component may be difficult to identify because the GRB ejecta is eventually swept up by the accompanying SN. The number density of asymmetric GRB remnants in the local Universe could be, however, far larger if they expand in a tenuous interstellar medium, as expected for some short GRB progenitor models. In these sources, the late size of the observable, asymmetric remnant could extend over a wide, possibly resolvable angle and may be easier to constrain directly.

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Prompt and Afterglow Emission Properties of Gamma‐Ray Bursts with Spectroscopically Identified Supernovae

Cited by 99 publications

References 88 publications

GRB 060218 and GRBs associated with supernovae Ib/c

GRB 060218 and GRBs associated with supernovae Ib/c

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

The Hydrodynamics of Gamma-Ray Burst Remnants

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