Jet Breaks in Short Gamma‐Ray Bursts. II. The Collimated Afterglow of GRB 051221A

Burrows, D. N.; Grupe, D.; Capalbi, M.; Panaitescu, A.; Patel, S.; Kouveliotou, C.; Zhang, Bing; Mészáros, P.; Chincarini, G.; Gehrels, N.; Wijers, R. A. M. J.

doi:10.1086/508740

Cited by 168 publications

(185 citation statements)

References 34 publications

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“…One immediate advantage offered by GRBs is that their bright electromagnetic emission allows a precise localization of the source on the sky, pinpointing the source directionn and lifting some of the degeneracies which limit distance determination. The extent of collimation in short GRBs is not well known, although recent analyses suggest that there may be a rather wide range in jet collimation from burst to burst [24,25]. For bursts that arise from binary NS mergers, our theoretical expectation is that emission should be beamed preferentially along the orbital angular momentum axis, where baryon loading is minimized.…”

Section: Grbs Observed By Gw Networkmentioning

confidence: 94%

Short GRB and binary black hole standard sirens as a probe of dark energy

Dalal

Holz

Hughes³

et al. 2006

Phys. Rev. D

311

340

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Observations of the gravitational radiation from well-localized, inspiraling compact-object binaries can measure absolute source distances with high accuracy. When coupled with an independent determination of redshift through an electromagnetic counterpart, these standard sirens can provide an excellent probe of the expansion history of the Universe and the dark energy. Short γ-ray bursts, if produced by merging neutron star binaries, would be standard sirens with known redshifts detectable by ground-based gravitational wave (GW) networks such as Advanced Laser Interferometer Gravitational-wave Observatory (LIGO), Virgo, and Australian International Gravitational Observatory (AIGO). Depending upon the collimation of these GRBs, the measurement of about 10 GW-GRB events (corresponding to about 1 yr of observation with an advanced GW detector network and an all-sky GRB monitor) can measure the Hubble constant h to ~ 2-3%. When combined with measurement of the absolute distance to the last scattering surface of the cosmic microwave background, this determines the dark energy equation of state parameter w to ~9%. Similarly, supermassive binary black hole inspirals will be standard sirens detectable by Laser Interferometer Space Antenna (LISA).Depending upon the precise redshift distribution, ~100 sources could measure w at the ~4% level. Disciplines Physical Sciences and Mathematics | PhysicsComments

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Section: Grbs Observed By Gw Networkmentioning

confidence: 94%

Short GRB and binary black hole standard sirens as a probe of dark energy

Dalal

Holz

Hughes³

et al. 2006

Phys. Rev. D

311

340

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“…The best case might again be GRB 090510 (de Pasquale et al 2010d), followed by GRBs 050724, 051221A, 061201, and 111020A. Unfortunately, the first burst (GRB 050724) allows only for an estimate of a lower limit on Θ jet ( 25 deg; Grupe et al 2006;Malesani et al 2007), while GRB 051221A relies on a well-sampled light curve (leading to Θ jet ∼ 4-8 deg; Burrows et al 2006;Soderberg et al 2006). The X-ray light curve of GRB 061201 is well-sampled, too ); again the observed break time is quite early (∼40 min; Θ jet = 1-2 deg).…”

Section: Jet Half-opening Anglesmentioning

confidence: 99%

Multi-color observations of short GRB afterglows: 20 events observed between 2007 and 2010

Guelbenzu

Klose

Greiner

et al. 2012

A&A

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We report on follow-up observations of 20 short-duration gamma-ray bursts (GRBs; T 90 < 2 s) performed in g r i z JHK s with the Gamma-Ray Burst Optical Near-Infrared Detector (GROND) between mid-2007 and the end of 2010. This is one of the most comprehensive data sets on GRB afterglow observations of short bursts published so far. In three cases, GROND was on target within less than 10 min after the trigger, leading to the discovery of the afterglow of GRB 081226A and its faint underlying host galaxy. In addition, GROND was able to image the optical afterglow and follow the light curve evolution in five further cases: GRBs 090305, 090426, 090510, 090927, and 100117A. In all other cases, optical/near-infrared upper limits can be provided on the afterglow magnitudes. After shifting all light curves to a common redshift, we find that the optical luminosities of the six events with light curves group into two subsamples. GRBs 090426 and 090927 are situated in the regime occupied by long-duration events (collapsars), while the other four bursts occupy the parameter space typical for merger events, confirming that the short-burst population is contaminated by collapsar events. Three of the aforementioned six bursts with optical light curves show a break: GRBs 090426 and 090510 (Papers I and II) as well as GRB 090305. For GRB 090927, no break is seen in the optical/X-ray light curve until about 150 ks/600 ks after the burst. The GROND multi-color data support the view that this burst is related to a collapsar event. A decay slope of the optical afterglow of GRB 100117A could be measured. For all six GRBs a lower limit on the corresponding jet opening angle can be set. Using these data supplemented by about ten events taken from the literature, we compare the jet half-opening angles of long and short bursts. We find tentative evidence that short bursts have wider opening angles than long bursts. However, the statistics are still very poor.

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“…This is the best example of a temporal break in the X-ray afterglow of a short burst to date. Only one other short burst so far showed convincing evidence of a temporal break in the X-ray light curve (GRB 051221A, Burrows et al 2006;Soderberg et al 2006).…”

Section: The Origin Of the Break In The X-ray Light Curvementioning

confidence: 99%

“…Fox et al 2005;Burrows et al 2006;Soderberg et al 2006). Intrinsic spectral parameters such as the peak energy E p of the EF(E) spectrum of the burst and the equivalent isotropic energy E iso , do not match the E p − E iso correlation for long GRBs (e.g.…”

Section: Introductionmentioning

confidence: 99%

A study of the prompt and afterglow emission of the short GRB 061201

Stratta¹,

D’Avanzo

Piranomonte

et al. 2007

A&A

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Context. Our knowledge of the intrinsic properties of short duration Gamma-Ray Bursts has relied, so far, only upon a few cases for which the estimate of the distance and an extended, multiwavelength monitoring of the afterglow have been obtained. Aims. We carried out multiwavelength observations of the short GRB 061201 aimed at estimating its distance and studying its properties. Methods. We performed a spectral and timing analysis of the prompt and afterglow emission and discuss the results in the context of the standard fireball model. Results. A clear temporal break was observed in the X-ray light curve about 40 min after the burst trigger. We find that the spectral and timing behaviour of the X-ray afterglow is consistent with a jet origin of the observed break, although the optical data can not definitively confirm this and other scenarios are possible. No underlying host galaxy down to R ∼ 26 mag was found after fading of the optical afterglow. Thus, no secure redshift could be measured for this burst. The nearest galaxy is at z = 0.111 and shows evidence of star formation activity. We discuss the association of GRB 061201 with this galaxy and with the ACO S 995 galaxy cluster, from which the source is at an angular distance of 17 and 8.5 , respectively. We also test the association with a possible undetected, positionally consistent galaxy at z ∼ 1. In all these cases, in the jet interpretation, we find a jet opening angle of 1-2 degrees.Key words. gamma rays: bursts IntroductionShort duration Gamma-ray Bursts (GRBs) are historically defined as those GRBs with burst duration less than two seconds and hard spectra (Kouveliotou et al. 1993). As the sample of short GRBs increases, in order to take into account all the spectral and temporal properties of the prompt emission, alternative empirical definitions of short GRBs have been introduced (e.g. Norris & Bonnell 2006;Zhang et al. 2007).The expected progenitor for short GRBs is a merging binary system of compact objects. However, our present knowledge of the intrinsic properties of short bursts mainly relies upon a few cases for which the distance could be derived and an extendedThe results reported in this paper are partially based on observations carried out at ESO telescopes under program 078.D-0809.INAF personnel resident at ASDC. multiwavelength monitoring of the afterglow was carried out.From these it appears that short bursts are less energetic and less collimated than long GRBs (e.g. Fox et al. 2005;Burrows et al. 2006;Soderberg et al. 2006). Intrinsic spectral parameters such as the peak energy E p of the EF(E) spectrum of the burst and the equivalent isotropic energy E iso , do not match the E p − E iso correlation for long GRBs (e.g. Amati 2007).The short bursts for which unambiguous hosts have been found are at redshifts between z = 0.10 and z = 0.55. The optical afterglows of seven short bursts and their likely host galaxies have been recently observed with telescopes such as ESO/VLT, Gemini, Magellan and HST, but no firm estimation of...

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Jet Breaks in Short Gamma‐Ray Bursts. II. The Collimated Afterglow of GRB 051221A

Cited by 168 publications

References 34 publications

Short GRB and binary black hole standard sirens as a probe of dark energy

Short GRB and binary black hole standard sirens as a probe of dark energy

Multi-color observations of short GRB afterglows: 20 events observed between 2007 and 2010

A study of the prompt and afterglow emission of the short GRB 061201

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