Probing the bright radio flare and afterglow of GRB 130427A with the Arcminute Microkelvin Imager

Anderson, G.; Horst, A. J. van der; Staley, T. D.; Fender, R. P.; Wijers, R. A. M. J.; Scaife, Anna M. M.; Rumsey, C.; Titterington, D.; Rowlinson, A.; Saunders, Richard D. E.

doi:10.1093/mnras/stu478

Cited by 46 publications

(70 citation statements)

References 41 publications

(72 reference statements)

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“…Further AMI observations beginning at 0.62 and 1.49 days post-burst then revealed a peak and rapid decay, demonstrating the early-time radio emission was likely dominated by the reverse-shock component at 15.7 GHz (see the light curve in Figure 2). The AMI fluxes for GRB 130427A displayed in Table 1 are slightly different to those quoted in Anderson et al (2014e) as they were calculated using the pipelined automated technique with a 4σs detection significance described in this paper rather than through a manual analysis using MIRIAD. However, the flux values from both analyses agree within their 1σs flux errors.…”

Section: Grb 130427amentioning

confidence: 89%

“…days post burst, as soon as GRB 130427A had risen above the horizon, resulting in one of the earliest published radio detections of a long GRB (Anderson et al 2014e). Further AMI observations beginning at 0.62 and 1.49 days post-burst then revealed a peak and rapid decay, demonstrating the early-time radio emission was likely dominated by the reverse-shock component at 15.7 GHz (see the light curve in Figure 2).…”

Section: Grb 130427amentioning

confidence: 95%

“…By the end of one year of operation the only radio counterparts detected were from GRB 120326A and GRB 130427A, with only one spectacular early detection coming from the latter (Anderson et al 2014e). The average sensitivity of these observations were 0.1 mJy/beam, with progressively worse RMS noise levels for lower declinations.…”

Section: Ami Strategy and Observationsmentioning

confidence: 98%

“…In order to investigate whether this new radio source was real, CASA was used to subtract a model of the contribution of the NVSS source from the visibilities. The resulting image revealed an unresolved point source at the position of the GRB with a peak flux of 0.46 ± 0.05 mJy/beam (Anderson et al 2014d). This same technique was performed on all the AMI observations, showing the detection of a fading point source present in two subsequent observations (see Figure 1), fading below detectability by 2014 July 18.…”

Section: Grb 140709amentioning

confidence: 99%

“…Early AMI-ALARRM results include observations of GRB 130427A, obtaining one of the earliest published radio detections of a long GRB at 0.36 days post-burst, allowing us to follow the rise and decline of the reverse-shock flare in the radio band (Anderson et al 2014e). Since 2014 May, the ALARRM programme has been expanded to also trigger on non-GRB Swift transients.…”

Section: Introductionmentioning

confidence: 99%

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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: Grb 130427amentioning

confidence: 89%

Section: Grb 130427amentioning

confidence: 95%

Section: Ami Strategy and Observationsmentioning

confidence: 98%

Section: Grb 140709amentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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GRB Observational Properties

Zhang¹,

Lü²,

Liang³

2016

Gamma-Ray Bursts

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Possible gamma-ray burst radio detections by the Square Kilometre Array. New perspectives

Ruggeri¹,

Capozziello²

2016

Astrophys Space Sci

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The next generation interferometric radio telescope, the Square Kilometre Array (SKA), which will be the most sensitive and largest radio telescope ever constructed, could greatly contribute to the detection, survey and characterization of Gamma Ray Bursts (GRBs). By the SKA, it will be possible to perform the follow up of GRBs even for several months. This approach would be extremely useful to extend the Spectrum Energetic Distribution (SED) from the gamma to the to radio band and would increase the number of radio detectable GRBs. In principle, the SKA could help to understand the physics of GRBs by setting constraints on theoretical models. This goal could be achieved by taking into account multiple observations at different wavelengths in order to obtain a deeper insight of the sources. Here, we present an estimation of GRB radio detections, showing that the GRBs can really be observed by the SKA. The approach that we present consists in determining blind detection rates derived by a very large sample consisting of merging several GRB catalogues observed by current missions as Swift, Fermi, Agile and INTEGRAL and by previous missions as BeppoSAX, CGRO, GRANAT, HETE-2, Ulysses and Wind. The final catalogue counts 7516 distinct sources. We compute the fraction of GRBs that could be observed by the SKA at high and low frequencies, above its observable sky. Considering the planned SKA sensitivity and through an extrapolation Alan Cosimo Ruggeri Salvatore Capozziello 1 Dipartimento di Fisica, Università di Napoli "Federico II", Compl. Univ. Monte S. Angelo, Via Cinthia 9, I -80126, Napoli, Italy. 2 I.N.F.N., Sez. di Napoli, Compl. Univ. Monte S. Angelo, Edificio G, Via Cintia, Napoli, Italy. 3 Gran Sasso Science Institute (INFN), Viale F. Crispi, 7, I-67100, L'Aquila, Italy. * acruggeri@na.infn.it; capozziello@na.infn.it based on previous works and observations, we deduce the minimum fluence in the range 15 -150 keV. This is the energy interval where a GRB should emit to be detectable in the radio band by the SKA. Results seem consistent with observational capabilities.

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Probing the bright radio flare and afterglow of GRB 130427A with the Arcminute Microkelvin Imager

Cited by 46 publications

References 41 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

GRB Observational Properties

Possible gamma-ray burst radio detections by the Square Kilometre Array. New perspectives

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