An Energetic Afterglow from a Distant Stellar Explosion

Frail, D. A.; Cameron, P. B.; Kasliwal, Mansi M.; Nakar, Ehud; Price, P. A.; Berger, E.; Gal‐Yam, A.; Kulkarni, S. R.; Fox, D. B.; Söderberg, A. M.; Schmidt, B.; Ofek, E. O.; Cenko, S. B.

doi:10.1086/506934

Cited by 69 publications

(118 citation statements)

References 38 publications

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“…A k-correction factor of (1 + z) α−β is also applied, where α and β are the temporal and spectral indices defined by F ∝ t α ν β , resulting in a k-corrected radio spectral luminosity of L = 4πF d 2 L /(1 + z) α−β−1 . Similar to Chandra & Frail (2012), we also assume α = 0 and β = 1/3, which is appropriate for an optically thin, flat, post-jet-break light curve (see their Section 3.2 and Frail et al 2006). Figure 9 shows the luminosity histogram of the radio detections and 4σs upper-limits.…”

Section: Radio Spectral Luminositymentioning

confidence: 99%

The Arcminute Microkelvin Imager catalogue of gamma-ray burst afterglows at 15.7 GHz

Anderson

Staley

Horst

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the Arcminute Microkelvin Imager (AMI) Large Array catalogue of 139 gamma-ray bursts (GRBs). AMI observes at a central frequency of 15.7 GHz and is equipped with a fully automated rapid-response mode, which enables the telescope to respond to highenergy transients detected by Swift. On receiving a transient alert, AMI can be on-target within two minutes, scheduling later start times if the source is below the horizon. Further AMI observations are manually scheduled for several days following the trigger. The AMI GRB programme probes the early-time (< 1 day) radio properties of GRBs, and has obtained some of the earliest radio detections (GRB 130427A at 0.36 and GRB 130907A at 0.51 days post-burst). As all Swift GRBs visible to AMI are observed, this catalogue provides the first representative sample of GRB radio properties, unbiased by multi-wavelength selection criteria. We report the detection of six GRB radio afterglows that were not previously detected by other radio telescopes, increasing the rate of radio detections by 50% over an 18-month period. The AMI catalogue implies a Swift GRB radio detection rate of 15%, down to ∼ 0.2 mJy/beam. However, scaling this by the fraction of GRBs AMI would have detected in the Chandra & Frail sample (all radio-observed GRBs between 1997 − 2011), it is possible ∼ 44 − 56% of Swift GRBs are radio bright, down to ∼ 0.1 − 0.15 mJy/beam. This increase from the Chandra & Frail rate (∼ 30%) is likely due to the AMI rapid-response mode, which allows observations to begin while the reverse-shock is contributing to the radio afterglow.

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Section: Radio Spectral Luminositymentioning

confidence: 99%

The Arcminute Microkelvin Imager catalogue of gamma-ray burst afterglows at 15.7 GHz

Anderson

Staley

Horst

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…In Fig. 13 we have drawn the SED of GRB 050904 at z = 6.3, including radio limits (Frail et al 2006), a detection in band 3 (and a limit in band 6) from Plateau de Bure Interferometer (CastroTirado et al, in prep. ), near-infrared and optical data (Tagliaferri et al 2005;Haislip et al 2006) and X-ray data from Swift.…”

Section: Grb Afterglowsmentioning

confidence: 99%

“…SED of GRB 050904 at redshift z = 6.29 (Kawai et al 2006) using the detection from PdBI 5.896 days after the burst (Castro-Tirado et al, in prep.). The X-ray flux is estimated from the XRT light curve, the radio data are from Frail et al (2006), while optical/NIR are extrapolations from Tagliaferri et al (2005); Haislip et al (2006). For the rough synchrotron spectrum drawn in blue, we have assumed an electron energy distribution index of p = 2.30, while an SMC extinction with A V = 0.12 (consistent with the value derived by Stratta et al 2011; but see also Zafar et al 2010) and Lyman blanketing (Madau 1995) have been considered in the red dotted line to match the optical/NIR observations.…”

Section: Grb Host Galaxies With Almamentioning

confidence: 99%

Pre-ALMA observations of GRBs in the mm/submm range

Postigo

Lundgren

Martín

et al. 2012

A&A

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Context. Gamma-ray bursts (GRBs) generate an afterglow emission that can be detected from radio to X-rays during days, or even weeks after the initial explosion. The peak of this emission crosses the millimeter and submillimeter range during the first hours to days, making their study in this range crucial for constraining the models. Observations have been limited until now due to the low sensitivity of the observatories in this range. This situation will be greatly improved with the start of scientific operations of the Atacama Large Millimeter/submillimeter Array (ALMA). Aims. In this work we do a statistical analysis of the complete sample of mm/submm observations of GRB afterglows obtained before the beginning of scientific operations at ALMA. Methods. We present observations of 11 GRB afterglows obtained from the Atacama Pathfinder Experiment (APEX) and the SubMillimeter Array (SMA), as well as the first detection of a GRB with ALMA, still in the commissioning phase, and put them into context with a catalogue of all the observations that have been published until now in the spectral range that is covered by ALMA.Results. The catalogue of mm/submm observations collected here is the largest to date and is composed of 102 GRBs, of which 88 have afterglow observations, whereas the rest are host galaxy searches. With our programmes, we contributed with data of 11 GRBs and the discovery of 2 submm counterparts. In total, the full sample, including data from the literature, has 22 afterglow detections with redshifts ranging from 0.168 to 8.2. GRBs have been detected in mm/submm wavelengths with peak luminosities spanning 2.5 orders of magnitude, the most luminous reaching 10 33 erg s −1 Hz −1 . We observe a correlation between the X-ray brightness at 0.5 days and the mm/submm peak brightness. Finally we give a rough estimate of the distribution of peak flux densities of GRB afterglows, based on the current mm/submm sample. Conclusions. Observations in the mm/submm bands have been shown to be crucial for our understanding of the physics of GRBs, but have until now been limited by the sensitivity of the observatories. With the start of the operations at ALMA, the sensitivity has improved by more than an order of magnitude, opening a new era in the study of GRB afterglows and their host galaxies. Our estimates predict that, once completed, ALMA will detect up to ∼98% of the afterglows if observed during the passage of the peak synchrotron emission.

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“…Further results of the modelling are a high density of the circumburst medium of n 0 = 600 +3000 −500 cm −3 (a high value, comparable to the high-z GRB 050904, Frail et al 2006), a rather low opening angle of θ 0 = 2.…”

Section: Modelling the Light Curve With Energy Injectionsmentioning

confidence: 76%

Photometry and spectroscopy of GRB 060526: a detailed study of the afterglow and host galaxy of az = 3.2 gamma-ray burst

Thöne

Канн²,

Jóhannesson

et al. 2010

A&A

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Aims. With this paper we want to investigate the highly variable afterglow light curve and environment of gamma-ray burst (GRB) 060526 at z = 3.221. Methods. We present one of the largest photometric datasets ever obtained for a GRB afterglow, consisting of multi-color photometric data from the ultraviolet to the near infrared. The data set contains 412 data points in total to which we add additional data from the literature. Furthermore, we present low-resolution high signal-to-noise spectra of the afterglow. The afterglow light curve is modeled with both an analytical model using broken power law fits and with a broad-band numerical model which includes energy injections. The absorption lines detected in the spectra are used to derive column densities using a multi-ion single-component curve-of-growth analysis from which we derive the metallicity of the host of GRB 060526. Results. The temporal behaviour of the afterglow follows a double broken power law with breaks at t = 0.090 ± 0.005 and t = 2.401 ± 0.061 days. It shows deviations from the smooth set of power laws that can be modeled by additional energy injections from the central engine, although some significant microvariability remains. The broadband spectral-energy distribution of the afterglow shows no significant extinction along the line of sight. The metallicity derived from S ii and Fe ii of [S/H] = -0.57 ± 0.25 and [Fe/H] = -1.09 ± 0.24 is relatively high for a galaxy at that redshift but comparable to the metallicity of other GRB hosts at similar redshifts. At the position of the afterglow, no host is detected to F775W(AB) = 28.5 mag with the HST, implying an absolute magnitude of the host M(1500 Å) > -18.3 mag which is fainter than most long-duration hosts, although the GRB may be associated with a faint galaxy at a distance of 11 kpc.

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An Energetic Afterglow from a Distant Stellar Explosion

Cited by 69 publications

References 38 publications

The Arcminute Microkelvin Imager catalogue of gamma-ray burst afterglows at 15.7 GHz

The Arcminute Microkelvin Imager catalogue of gamma-ray burst afterglows at 15.7 GHz

Pre-ALMA observations of GRBs in the mm/submm range

Photometry and spectroscopy of GRB 060526: a detailed study of the afterglow and host galaxy of az = 3.2 gamma-ray burst

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