The afterglow and elliptical host galaxy of the short γ-ray burst GRB 050724

Berger, E.; Price, P. A.; Cenko, S. B.; Gal‐Yam, A.; Söderberg, A. M.; Kasliwal, M. M.; Leonard, D. C.; Cameron, P. B.; Frail, D. A.; Kulkarni, S. R.; Murphy, David; Krzemiński, W.; Piran, Tsvi; Lee, B L; Roth, Kathy; Moon, D. S.; Fox, D. B.; Harrison, Fiona A.; Persson, S. E.; Schmidt, B.; Penprase, B. E.; Rich, J.; Peterson, Bruce A.; Cowie, L. L.

doi:10.1038/nature04238

Cited by 343 publications

(390 citation statements)

References 24 publications

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“…However, past sGRBs that were detected in the radio despite being 30-60 times more distant than this event (Berger et al 2005;Soderberg et al 2006;Fong et al 2014;18 Andreoni et al Zhang et al 2017) imply that future neutron star mergers at these (40 Mpc) distances could reach flux densities of 0.1 to 1 Jy. The Parkes and ASKAP radio telescopes searched for FRBs in NGC 4993 after the BNS merger for a total of 5 and 18.7 h, respectively.…”

Section: Discussionmentioning

confidence: 99%

Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes

Andreoni

Ackley

Cooke

et al. 2017

Publ. Astron. Soc. Aust.

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179

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The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early-to late-time multi-wavelength observations, including optical imaging and spectroscopy, midinfrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source emission cooled from approximately 6 400 K to 2 100 K over a 7-d period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (∼2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor.

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Section: Discussionmentioning

confidence: 99%

Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes

Andreoni

Ackley

Cooke

et al. 2017

Publ. Astron. Soc. Aust.

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179

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“…This is significantly less than the typical SFR observed in long GRB host galaxies (Christensen et al 2004). Comparing with other short GRBs host galaxy SFRs, this is lower than that of the host of GRB 051221A by a factor of 3.3 (Soderberg et al 2006) but much larger than that of the hosts of the short GRBs GRB 050509B (Bloom et al 2005, Gehrels et al 2006 and GRB 050724 (Berger et al 2005), by factors of more than about 20 and 60 respectively. We also note that our SFR value is of the same order as that measured for GRB 050709, a short GRB for which the association to a star-forming galaxy is secure (Covino et al 2006).…”

Section: Optical Spectroscopy and Host Galaxy Candidates For Grb061201mentioning

confidence: 96%

“…Short burst jet opening angles estimated so far were obtained for GRB 051221A, angle of ∼4-8 degrees Soderberg et al 2006) based on multiwavelength observations (from radio to X-rays) and for GRB 050709, based however on few data points that provided a poorly constrained jet angle of about ∼15 degrees (Fox et al 2005; but see also Watson et al 2006). For GRB 050724, a jet angle of ∼8-12 degree was claimed from radio and NIR observations (Berger et al 2005). This measure is however still under debate since no break was observed in the X-ray light curve up to three weeks after the burst, implying a jet opening angle lower limit of 25 degrees ).…”

Section: Discussionmentioning

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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“…One possible exception is the case of GRB 090426 at z = 2.609 (Levesque et al 2010;Antonelli et al 2009;Zhang et al 2009) for which absorption line spectroscopy of the afterglow was successfully obtained, but may be considered on balance by the authors to be associated with the population of long gamma-ray bursts. The host galaxies of the short bursts were found initially to be mostly elliptical galaxies, e.g., GRB 050509B (Gehrels et al 2005;Bloom et al 2006) and GRB 050724 (Berger et al 2005;Gorosabel et al 2006) and that an old progenitor population was required. However, as the sample has since increased, all types of galaxies, from elliptical to star-forming, have been found to be associated with short bursts and the majority of short bursts are now found to reside in star forming galaxies (e.g., Berger et al 2007;Berger 2009;Prochaska et al 2006).…”

Section: Discussionmentioning

confidence: 99%

Optical and near-infrared follow-up observations of fourFermi/LAT GRBs: redshifts, afterglows, energetics, and host galaxies

McBreen

Krühler

Rau

et al. 2010

A&A

114

100

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Aims. Fermi can measure the spectral properties of gamma-ray bursts over a very large energy range and is opening a new window on the prompt emission of these energetic events. Localizations by the instruments on Fermi in combination with follow-up by Swift provide accurate positions for observations at longer wavelengths leading to the determination of redshifts, the true energy budget, host galaxy properties and facilitate comparison with pre-Fermi bursts. Methods. Multi-wavelength follow-up observations were performed on the afterglows of four bursts with high energy emission detected by Fermi/LAT: GRB 090323, GRB 090328, GRB 090510 and GRB 090902B. They were obtained in the optical/near-infrared bands with GROND mounted at the MPG/ESO 2.2 m telescope and additionally of GRB 090323 in the optical with the 2 m telescope in Tautenburg, Germany. Three of the events are classified as long bursts while GRB 090510 is a well localized short GRB with GeV emission. In addition, host galaxies were detected for three of the four bursts. Spectroscopic follow-up was initiated with the VLT for GRB 090328 and GRB 090510. Results. The afterglow observations in 7 bands are presented for all bursts and their host galaxies are investigated. Knowledge of the distance and the local dust extinction enables comparison of the afterglows of LAT-detected GRBs with the general sample. The spectroscopic redshifts of GRB 090328 and GRB 090510 were determined to be z = 0.7354 ± 0.0003 and z = 0.903 ± 0.001 and dust corrected star-formation rates of 4.8 M yr −1 and 0.60 M yr −1 were derived for their host galaxies, respectively. Conclusions. The afterglows of long bursts exhibit power-law decay indices (α) from less than 1 to ∼2.3 and spectral indices (β opt ) values from 0.65 to ∼1.2 which are fairly standard for GRB afterglows. Constraints are placed on the jet half opening angles of < ∼ 2.1 • to > ∼ 6.4 • , which allows limits to be placed on the beaming corrected energies. These range from < ∼ 5 × 10 50 erg to the one of the highest values ever recorded, > ∼ 2.2 × 10 52 erg for GRB 090902B, and are not consistent with a standard candle. The extremely energetic long Fermi bursts have optical afterglows which lie in the top half of the brightness distribution of all optical afterglows detected in the Swift era or even in the top 5% if incompleteness is considered. The properties of the host galaxies of these LAT detected bursts in terms of extinction, star formation rates and masses do not appear to differ from previous samples.

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The afterglow and elliptical host galaxy of the short γ-ray burst GRB 050724

Cited by 343 publications

References 24 publications

Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes

Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes

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

Optical and near-infrared follow-up observations of fourFermi/LAT GRBs: redshifts, afterglows, energetics, and host galaxies

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