On the environment of short gamma-ray bursts

Kopač, D.; D’Avanzo, P.; Melandri, A.; Campana, S.; Gomboc, A.; Japelj, J.; Bernardini, M. G.; Covino, S.; Vergani, S. D.; Salvaterra, R.; Tagliaferri, G.

doi:10.1111/j.1365-2966.2012.21418.x

Cited by 32 publications

(31 citation statements)

References 66 publications

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“…The best-fit spectral parameters are a photon index of −2.19 (z = 0) assuming the galactic N H at the burst direction of 3.7 × 10 20 cm −2 (Kalberla et al 2005). Both the measured photon index and N H for GRB 111117A are consistent with those of other Swift short GRBs (Kopač et al 2012;Fong et al 2012).…”

Section: X-rayssupporting

confidence: 69%

IDENTIFYING THE LOCATION IN THE HOST GALAXY OF THE SHORT GRB 111117A WITH THECHANDRASUBARCSECOND POSITION

Sakamoto

Troja

Aoki

et al. 2013

ApJ

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We present our successful Chandra program designed to identify, with subarcsecond accuracy, the X-ray afterglow of the short GRB 111117A, which was discovered by Swift and Fermi. Thanks to our rapid target of opportunity request, Chandra clearly detected the X-ray afterglow, though no optical afterglow was found in deep optical observations. The host galaxy was clearly detected in the optical and near-infrared band, with the best photometric redshift of z = 1.31 +0.46 −0.23 (90% confidence), making it one of the highest known short gamma-ray burst (GRB) redshifts. Furthermore, we see an offset of 1.0 ± 0.2 arcsec, which corresponds to 8.4 ± 1.7 kpc, between the host and the afterglow position. We discuss the importance of using Chandra for obtaining subarcsecond X-ray localizations of short GRB afterglows to study GRB environments.

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Section: X-rayssupporting

confidence: 69%

IDENTIFYING THE LOCATION IN THE HOST GALAXY OF THE SHORT GRB 111117A WITH THECHANDRASUBARCSECOND POSITION

Sakamoto

Troja

Aoki

et al. 2013

ApJ

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“…This interpretation has been supported by direct optical observations of GRBs located in the outskirt of the host galaxies (Sahu et al 1997;van Paradijs et al 1997;Bloom et al 2006;Troja et al 2008;Fong et al 2010;Berger 2011;Kopač et al 2012).…”

Section: The Disguised Short Grbssupporting

confidence: 53%

GRB 090227b: The Missing Link Between the Genuine Short and Long Gamma-Ray Bursts

Muccino¹,

Ruffini²,

Bianco³

et al. 2013

ApJ

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The time-resolved spectral analysis of GRB 090227B, made possible by the Fermi-GBM data, allows us to identify in this source the missing link between the genuine short and long gamma-ray bursts (GRBs). Within the Fireshell model of the GRBs we predict genuine short GRBs: bursts with the same inner engine of the long bursts but endowed with a severely low value of the baryon load, B 5 × 10 −5 . A first energetically predominant emission occurs at the transparency of the e + e − plasma, the Proper-GRB (P-GRB), followed by a softer emission, the extended afterglow. The typical separation between the two emissions is expected to be of the order of 10 −3 -10 −2 s. We identify the P-GRB of GRB 090227B in the first 96 ms of emission, where a thermal component with the temperature kT = (517 ± 28) keV and a flux comparable with the non-thermal part of the spectrum is observed. This non-thermal component as well as the subsequent emission, where there is no evidence for a thermal spectrum, is identified with the extended afterglow. We deduce a theoretical cosmological redshift z = 1.61 ± 0.14. We then derive the total energy E tot e + e − = (2.83 ± 0.15) × 10 53 erg, the baryon load B = (4.13 ± 0.05) × 10 −5 , the Lorentz Γ factor at transparency Γ tr = (1.44 ± 0.01) × 10 4 , and the intrinsic duration Δt ∼ 0.35 s. We also determine the average density of the circumburst medium (CBM), n CBM = (1.90 ± 0.20) × 10 −5 particles cm −3 . There is no evidence of beaming in the system. In view of the energetics and of the baryon load of the source, as well as of the low interstellar medium and of the intrinsic timescale of the signal, we identify the GRB progenitor as a binary neutron star. From the recent progress in the theory of neutron stars, we obtain masses of the stars m 1 = m 2 = 1.34 M and their corresponding radii R 1 = R 2 = 12.24 km and thickness of their crusts ∼0.47 km, consistent with the above values of the baryon load, of the energetics and of the time duration of the event.

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Section: The Disguised Short Grbssupporting

confidence: 56%

GRB 090227b: The Missing Link Between the Genuine Short and Long GRBS

Muccino¹,

Ruffini²,

Bianco³

et al. 2015

The Thirteenth Marcel Grossmann Meeting

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The time-resolved spectral analysis of GRB 090227B, made possible by the Fermi-GBM data, allows to identify in this source the missing link between the genuine short and long GRBs. Within the Fireshell model of the Gamma-Ray Bursts (GRBs) we predict genuine short GRBs: bursts with the same inner engine of the long bursts but endowed with a severely low value of the Baryon load, B 5 × 10 −5 . A first energetically predominant emission occurs at the transparency of the e + e − plasma, the Proper-GRB (P-GRB), followed by a softer emission, the extended afterglow. The typical separation between the two emissions is expected to be of the order of 10 −3 -10 −2 s. We identify the P-GRB of GRB 090227B in the first 96 ms of emission, where a thermal component with the temperature kT = (517 ± 28) keV and a flux comparable with the non thermal part of the spectrum is observed. This non thermal component as well as the subsequent emission, where there is no evidence for a thermal spectrum, is identified with the extended afterglow. We deduce a theoretical cosmological redshift z = 1.61 ± 0.14. We then derive the total energy E tot e + e − = (2.83 ± 0.15) × 10 53 ergs, the Baryon load B = (4.13 ± 0.05) × 10 −5, the Lorentz Γ factor at transparency Γ tr = (1.44 ± 0.01) × 10 4 , and the intrinsic duration ∆t ′ ∼ 0.35 s. We also determine the average density of the CircumBurst Medium (CBM), n CBM = (1.90 ± 0.20) × 10 −5 particles/cm 3 . There is no evidence of beaming in the system. In view of the energetics and of the Baryon load of the source, as well as of the low interstellar medium and of the intrinsic time scale of the signal, we identify the GRB progenitor as a binary neutron star. From the recent progress in the theory of neutron stars, we obtain masses of the stars m 1 = m 2 = 1.34M ⊙ and their corresponding radii R 1 = R 2 = 12.24 km and thickness of their crusts ∼ 0.47 km, consistent with the above values of the Baryon load, of the energetics and of the time duration of the event.

show abstract

On the environment of short gamma-ray bursts

Cited by 32 publications

References 66 publications

IDENTIFYING THE LOCATION IN THE HOST GALAXY OF THE SHORT GRB 111117A WITH THECHANDRASUBARCSECOND POSITION

IDENTIFYING THE LOCATION IN THE HOST GALAXY OF THE SHORT GRB 111117A WITH THECHANDRASUBARCSECOND POSITION

GRB 090227b: The Missing Link Between the Genuine Short and Long Gamma-Ray Bursts

GRB 090227b: The Missing Link Between the Genuine Short and Long GRBS

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