Thermal emission in the early afterglow of gamma-ray bursts from their interaction with supernova ejecta

Ruffini, Remo; Vereshchagin, Gregory; Wang, Y.

doi:10.1051/0004-6361/201527553

Cited by 7 publications

(12 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…from the cooling photosphere after SN shock breakout (Waxman et al 2007;Nakar & Sari 2010; but see also Irwin & Chevalier 2016;Ruffini et al 2017). Substantial observational efforts have been put forward to search for such a signal in the X-ray data of long-duration GRBs (e.g., Olivares E. et al 2012;Starling et al 2012;Sparre & Starling 2012) as well as in the optical data of SNe in general (e.g., Förster et al 2016), mostly with negative results.…”

Section: Excess Of Blue Light In the Optical Transient That Followed ...mentioning

confidence: 99%

Four GRB supernovae at redshifts between 0.4 and 0.8

Klose

Schmidl

Канн

et al. 2019

A&A

View full text Add to dashboard Cite

Twenty years ago, GRB 980425/SN 1998bw revealed that long Gamma-Ray Bursts (GRBs) are physically associated with broad-lined type Ic supernovae. Since then more than 1000 long GRBs have been localized to high angular precision, but only in ∼ 50 cases the underlying supernova (SN) component was identified. Using the multi-channel imager GROND (Gamma-Ray Burst Optical Near-Infrared Detector) at ESO/La Silla, during the last ten years we have devoted a substantial amount of observing time to reveal and to study SN components in long-GRB afterglows.Here we report on four more GRB-SNe (associated with GRBs 071112C, 111228A, 120714B, and 130831A) which were discovered and/or followed-up with GROND and whose redshifts lie between z = 0.4 and 0.8. We study their afterglow light curves, follow the associated SN bumps over several weeks, and characterize their host galaxies. Using SN 1998bw as a template, the derived SN explosion parameters are fully consistent with the corresponding properties of the so-far known GRB-SN ensemble, with no evidence for an evolution of their properties as a function of redshift. In two cases (GRB 120714B/SN 2012eb at z = 0.398 and GRB 130831A/SN 2013fu at z = 0.479) additional Very Large Telescope (VLT) spectroscopy of the associated SNe revealed a photospheric expansion velocity at maximum light of about 40 000 and 20 000 km s −1 , respectively. For GRB 120714B, which was an intermediate-luminosity burst, we find additional evidence for a blackbody component in the light of the optical transient at early times, similar to what has been detected in some GRB-SNe at lower redshifts.

show abstract

Section: Excess Of Blue Light In the Optical Transient That Followed ...mentioning

confidence: 99%

Four GRB supernovae at redshifts between 0.4 and 0.8

Klose

Schmidl

Канн

et al. 2019

A&A

View full text Add to dashboard Cite

show abstract

“…10 where we plotted the difference of the peak flux and fluence E peak as a function of the peak flux E peak . One can infer from the figure that the softening depends on E peak itself (Ruffini et al 2017). At higher energies it seems to disappear (Norris et al 2000;Norris 2002;Kazanas et al 2002).…”

Section: Physical Differences Between the Spectral Type Obtained From...mentioning

confidence: 83%

Statistical properties of Fermi GBM GRBs’ spectra

Rácz¹,

Balázs²,

Horváth³

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Statistical studies of gamma-ray burst (GRB) spectra may result in important information on the physics of GRBs. The Fermi GBM catalog contains GRB parameters (peak energy, spectral indices, intensity) estimated fitting the gamma-ray SED of the total emission (fluence, flnc), and during the time of the peak flux (pflx ). Using contingency tables we studied the relationship of the models best fitting pflx and flnc time intervals.Our analysis revealed an ordering of the spectra into a power law -Comptonized -smoothly broken power law -Band series. This result was further supported by a correspondence analysis (CA) of the pflx and flnc spectra categorical variables. We performed a linear discriminant analysis (LDA) to find a relationship between categorical (spectral) and model independent physical data. LDA resulted in highly significant physical differences among the spectral types, that is more pronounced in the case of the pflx spectra, than for the flnc spectra. We interpreted this difference as caused by the temporal variation of the spectrum during the outburst. This spectral variability is confirmed by the differences in the low energy spectral index and peak energy, between the pflx and flnc spectra. We found that the synchrotron radiation is significant in GBM spectra. The mean low energy spectral index is close to the canonical value of α = −2/3 during the peak flux. However, α is ∼ −0.9 for the spectra of the fluences. We interpret this difference as showing that the effect of cooling is important only for the fluence spectra.

show abstract

“…GRBs show typical power-law decays, in many cases they overlap a Supernova light curve [5]. The connections between GRB and Supernovae have been documented several times.…”

Section: Fitting the 1054 Event With A Grbmentioning

confidence: 99%

Fitting the Crab Supernova with a Gamma-Ray Burst

Ruffini,

Sigismondi

2024

Preprint

View full text Add to dashboard Cite

A panorama of the current historiography on the Supernova of 1054 is outlined. Shklovsky (1968) [1], and Murdin (1985) [2] show how the interpretation of this phenomenon converged on a Su-pernova event. Here we reconsider the historical data, assuming a Gamma-Ray Burst (GRB) as its source. A Supernova correlated with the GRB explains well the fading time observed by the an-cient Chinese astronomers, in daytime and in night time, while the GRB power-law explains the present X-rays and GeV emission of the Crab. On the ground of recent understanding of the first episode of binary driven Hypernova GRB (BDHN GRB) in terms of the collapse of a ten solar masses core, we propose the possible identification of the real Supernova event at earlier time than Chinese chronicles. This work allows a new understanding of the significance of historical astronomical observations, including a fireball, due to gamma-rays air shower observation, and a plague of acute radiation syndrome, documented with several thousands of victims in the Eura-sian area (Egypt, Iraq and Siria).

show abstract

Thermal emission in the early afterglow of gamma-ray bursts from their interaction with supernova ejecta

Cited by 7 publications

References 32 publications

Four GRB supernovae at redshifts between 0.4 and 0.8

Four GRB supernovae at redshifts between 0.4 and 0.8

Statistical properties of Fermi GBM GRBs’ spectra

Fitting the Crab Supernova with a Gamma-Ray Burst

Contact Info

Product

Resources

About