Automated rapid follow-up of Swift gamma-ray burst alerts at 15 GHz with the AMI Large Array

Staley, T. D.; Titterington, D.; Fender, R. P.; Swinbank, J.; Horst, A. J. van der; Rowlinson, A.; Scaife, Anna M. M.; Grainge, Keith; Pooley, G. G.

doi:10.1093/mnras/sts259

Cited by 45 publications

(60 citation statements)

References 39 publications

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“…However, it is also possible this source is an artefact produced by the nearby radio sources NVSS 141009+084149 and NVSS 140957+084108. This single epoch detection was not reported in Staley et al (2013) likely due to differences in the reduction procedure and our use of an automatic source finder. No source was blindly detected in the followup observation that occurred 15.6 days later or in the concatenated image, with 4σs upper limits of 0.36 and 0.25 mJy/beam, respectively.…”

Section: Appendix A: Description Of New Possible Grb Radio Afterglowsmentioning

confidence: 87%

“…The AMI flux measurements of GRB 120326A were first reported by Staley et al (2013). However, the flux values for GRB 120326A presented in this publication, calculated using our new and improved reduction and analysis pipeline, are slightly different due to updated scripts for the AMI data reduction process used in AMI-REDUCE and the application of more stringent protocols for acceptable datasets.…”

Section: Grb 120326amentioning

confidence: 94%

“…The calibration stage of AMISURVEY calls on the Python library DRIVE-AMI (first introduced by Staley et al 2013) built upon AMI REDUCE. AMI REDUCE is designed to take the raw AMI dataset and automatically flag for interference, shadowing, and hardware errors, apply phase and amplitude calibration, and Fourier transform the data.…”

Section: Pipeline Reduction and Analysismentioning

confidence: 99%

“…However, the flux values for GRB 120326A presented in this publication, calculated using our new and improved reduction and analysis pipeline, are slightly different due to updated scripts for the AMI data reduction process used in AMI-REDUCE and the application of more stringent protocols for acceptable datasets. For example, the AMI observation of GRB 120326A that took place on 2012-04-04 and 2012-04-08, which are mentioned in Staley et al (2013), were rejected from further analysis due to being rain affected data-sets.…”

Section: Grb 120326amentioning

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: Appendix A: Description Of New Possible Grb Radio Afterglowsmentioning

confidence: 87%

Section: Grb 120326amentioning

confidence: 94%

Section: Pipeline Reduction and Analysismentioning

confidence: 99%

Section: Grb 120326amentioning

confidence: 99%

See 2 more Smart Citations

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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“…It then analyses the alert information, and decides whether or not the event is worthy of follow-up observation with pt5m. Currently, new cataclysmic variables, new AGN-variability, and new unknown transients are followed up, as well as any new gamma-ray bursts which have also triggered immediate radio follow-up with the AMI Large Array radio telescope (Staley et al 2013). Transients classified as anything else are not followed up at this stage.…”

Section: Alert Listenermentioning

confidence: 99%

pt5m– a 0.5 m robotic telescope on La Palma

Hardy

Butterley

Dhillon

et al. 2015

Mon. Not. R. Astron. Soc.

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The radio/X‐ray correlation in Swift J1753.5–0127

et al. 2016

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Great effort has gone into trying to explain the two observed radio/X-ray correlation tracks seen in the low/hard state of black hole X-ray binaries in recent years. The original, "standard" correlation of the form L R ∝ L b X , where b = 0.7 ± 0.1, is paired with a separate, lower correlation track with a steeper slope of ∼ 1-1.4, at least at high luminosities. These outlier sources seem to show fainter radio emission than expected for a given X-ray luminosity, thus acquiring the term "radio-quiet". While most sources seem to maintain their intrinsic correlation slopes over decades in luminosity, a growing sample of sources have recently been reported to move from one correlation to the other. We present preliminary results from a coordinated radio/X-ray monitoring campaign of the radio-quiet black hole binary Swift J1753.5−0127, spanning nearly two years in time. Our observations add lower-luminosity coverage to an existing sample of observations, and we observe the radio-quiet track to proceed horizontally towards the standard correlation as the X-ray luminosity slowly starts to decrease. The source stays on the transition track for ∼ 60 days, during which its X-ray luminosity is observed to drop by more than an order of magnitude while its radio luminosity stays constant. Time-averaged X-ray energy spectra show very little change during this phase, leaving no obvious parameters to explain the observed transition behaviour.

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Automated rapid follow-up of Swift gamma-ray burst alerts at 15 GHz with the AMI Large Array

Cited by 45 publications

References 39 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

pt5m– a 0.5 m robotic telescope on La Palma

The radio/X‐ray correlation in Swift J1753.5–0127

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