Discovery of the short γ-ray burst GRB 050709

Villaseñor, J.; Lamb, D. Q.; Ricker, G.; Atteia, J. L.; Kawai, N.; Butler, Nathaniel R.; Nakagawa, Y. E.; Jernigan, J. G.; Boër, M.; Crew, G. B.; Donaghy, T.; Doty, J.; Fenimore, E. E.; Galassi, M.; Graziani, C.; Hurley, K.; Levine, A. M.; Martel, F.; Matsuoka, M.; Olive, J. F.; Prigozhin, G.; Sakamoto, T.; Shirasaki, Y.; Suzuki, M.; Tamagawa, T.; Vanderspek, R.; Woosley, S. E.; Yoshida, A.; Braga, J.; Manchanda, R. K.; Pizzichini, G.; Takagishi, K.; Yamauchi, M.

doi:10.1038/nature04213

Cited by 238 publications

(247 citation statements)

References 29 publications

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“…Although the two burst populations have different progenitors, the outflow that produces them must have a very high compactness in both cases, and may be driven by essentially the same mechanism (e.g., a MHD jet). The short GRBs have systematically higher peak energies than is implied by the Amati et al (2002) relation (Donaghy et al 2007), but so far only GRB 050709 has both a well-defined redshift and measured spectral peak energy (Fox et al 2005;Villasenor et al 2005).…”

Section: Implications For the E Pk -E Iso Relation Of Short Grbsmentioning

confidence: 76%

Thermalization in Relativistic Outflows and the Correlation between Spectral Hardness and Apparent Luminosity in Gamma‐Ray Bursts

Thompson¹,

Mészáros²,

Rees³

2007

ApJ

161

182

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We present an interpretation of the phenomenological relations between the spectral peak, isotropic luminosity, and duration of long gamma-ray bursts that have been discovered by Amati and coworkers, Ghirlanda and coworkers, Firmani and coworkers, and Liang & Zhang. In our proposed model, a jet undergoes internal dissipation which prevents its bulk Lorentz factor from exceeding 1/ ( being the jet opening angle) until it escapes from the core of its progenitor star, at a radius of order 10 10 cm; dissipation may continue at larger radii. The dissipated radiation will be partially thermalized, and we identify its thermal peak ( Doppler boosted by the outflow) with E pk . The radiation comes, in effect, from within the jet photosphere. The nonthermal, high-energy part of the GRB emission arises from Comptonization of this radiation by relativistic electrons and positrons outside the effective photosphere. This model can account naturally not only for the surprisingly small scatter in the various claimed correlations, but also for the normalization, as well as the slopes. It then has further implications for the jet energy, the limiting jet Lorentz factor, and the relation of the energy, opening angle and burst duration to the mass and radius of the stellar stellar progenitor. The observed relation between pulse width and photon frequency can be reproduced by inverse Compton emission at $10 14 cm from the engine, but there are significant constraints on the energy distribution and isotropy of the radiating particles.

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Section: Implications For the E Pk -E Iso Relation Of Short Grbsmentioning

confidence: 76%

Thermalization in Relativistic Outflows and the Correlation between Spectral Hardness and Apparent Luminosity in Gamma‐Ray Bursts

Thompson¹,

Mészáros²,

Rees³

2007

ApJ

161

182

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“…This situation has changed with the detection of X-ray afterglow from several short bursts by Swift (Gehrels et al 2005;Romano et al 2005) and by HETE II (Villasenor et al 2005). In some cases, optical (Covino et al 2005;Fox et al 2005;Bloom et al 2006;Price et al 2005;Jensen et al 2005;Hjorth et al 2005;Castro-Tiraldo et al 2005;Gal-Yam et al 2005b;Cobb et al 2005;Wiersema et al 2005) and radio (Cameron & Frail 2005;Berger 2005) afterglow was detected as well.…”

Section: Introductionmentioning

confidence: 99%

The BATSE-Swift luminosity and redshift distributions of short-duration GRBs

Guetta¹,

Piran

2006

A&A

151

178

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We compare the luminosity function and rate inferred from the BATSE peak flux distribution of short hard bursts (SHBs) with the redshift and luminosity distributions of SHBs observed by Swift/HETE II. While the Swift/HETE II SHB sample is incompatible with the SHB population that follows the star formation rate, it is compatible with an SHB rate that reflects a distribution of delay times after the SFR. This would be the case if SHBs were associated with binary neutron star mergers. The available data allows, however, different interpretations. For example, a population whose rate is independent of the redshift fits the data very well. The implied SHB rates that we find range from ∼8 to ∼30 h 3 70 Gpc −3 yr −1 . This rate, which is comparable to the rate of neutron star mergers estimated from statistics of binary pulsars, is a much higher rate than what was previously estimated. We stress that our analysis, which is based on observed SHBs, is limited to bursts with luminosities above 10 49 erg/s. Weaker bursts may exist, but if so they are hardly detected by BATSE of Swift, so their rate is very weakly constrained by current observations.

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“…They noticed the existence of hybrid sources with an occasional, softer, prolonged emission lasting tenths of seconds in the gamma-ray energy band, following an initial spike-like emission comprising an otherwise short burst. The observations by Swift further infringed the short/long dichotomy in many ways: some short duration GRBs were observed to be followed by an X-ray afterglow (first GRB 050509B observed by Swift, see Gehrels et al 2005; and, two months later, GRB 050709 observed by HETE-2, see Villasenor et al 2005); some nearby long-duration GRBs were also observed to be not associated with SN (GRB 060614, Della Valle et al 2006;Fynbo et al 2006;Gal-Yam et al 2006;and GRB 060505, Xu et al 2009). …”

Section: Introductionmentioning

confidence: 99%

GRB 071227: an additional case of adisguisedshort burst

Caito¹,

Amati

Bernardini

et al. 2010

A&A

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Context. Observations of gamma-ray bursts (GRBs) have shown an hybridization between the two classes of long and short bursts. In the context of the fireshell model, the GRB light curves are formed by two different components: the proper GRB (P-GRB) and the extended afterglow. Their relative intensity is linked to the fireshell baryon loading B. The GRBs with P-GRB predominance are the short ones, the remainders are long. A new family of disguised short bursts has been identified: long bursts with a protracted low instantaneous luminosity due to a low density CircumBurst Medium (CBM). In the 15-150 keV energy band GRB 071227 exhibits a short duration (about 1.8 s) spike-like emission followed by a very soft extended tail up to one hundred seconds after the trigger. It is a faint (E iso = 5.8 × 10 50 ) nearby GRB (z = 0.383) that does not have an associated type Ib/c bright supernova (SN). For these reasons, GRB 071227 has been classified as a short burst not fulfilling the Amati relation holding for long burst. Aims. We check the classification of GRB 071227 provided by the fireshell model. In particular, we test whether this burst is another example of a disguised short burst, after GRB 970228 and GRB 060614, and, for this reason, whether it fulfills the Amati relation. Methods. We simulate GRB 071227 light curves in the Swift BAT 15-50 keV bandpass and in the XRT (0.3-10 keV) energy band within the fireshell model. Results. We perform simulations of the tail in the 15-50 keV bandpass, as well as of the first part of the X-ray afterglow. This infers that: E e ± tot = 5.04 × 10 51 erg, B = 2.0 × 10 −4 , E P−GRB /E aft ∼ 0.25, and n cbm = 3.33 particles cm −3 . These values are consistent with those of "long duration" GRBs. We interpret the observed energy of the first hard emission by identifying it with the P-GRB emission. The remaining long soft tail indeed fulfills the Amati relation. Conclusions. Previously classified as a short burst, GRB 071227 on the basis of our analysis performed in the context of the fireshell scenario represents another example of a disguised short burst, after GRB 970228 and GRB 060614. Further confirmation of this result is that the soft tail of GRB 071227 fulfills the Amati relation.

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Discovery of the short γ-ray burst GRB 050709

Cited by 238 publications

References 29 publications

Thermalization in Relativistic Outflows and the Correlation between Spectral Hardness and Apparent Luminosity in Gamma‐Ray Bursts

Thermalization in Relativistic Outflows and the Correlation between Spectral Hardness and Apparent Luminosity in Gamma‐Ray Bursts

The BATSE-Swift luminosity and redshift distributions of short-duration GRBs

GRB 071227: an additional case of adisguisedshort burst

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