AMI Galactic Plane Survey at 16 GHz - I. Observing, mapping and source extraction

Perrott, Y. C.; Scaife, Anna M. M.; Green, D. A.; Davies, Matthew; Franzen, T. M. O.; Grainge, Keith; Hobson, M.; Hurley‐Walker, N.; Lasenby, A.; Olamaie, Malak; Pooley, G. G.; Rodríguez‐Gonzálvez, Carmen; Rumsey, C.; Saunders, Richard D. E.; Schammel, Michel P.; Scott, Paul F.; Shimwell, T. W.; Titterington, D.; Waldram, E. M.

doi:10.1093/mnras/sts589

Cited by 53 publications

(29 citation statements)

References 35 publications

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“…Flagging and calibration of the data were performed with the AMI REDUCE software (32,33). The calibrated data were then imported into CASA (34) and the flux densities of V404 Cygni were extracted by vector averaging over all baselines at multiple frequencies within the passband.…”

Section: Radio Observationsmentioning

confidence: 99%

A precise measurement of the magnetic field in the corona of the black hole binary V404 Cygni

Dallilar

Eikenberry

Garner

et al. 2017

Science

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Conditions in a black hole outburst The binary system V404 Cygni consists of a red giant star orbiting a black hole. In 2015, a surge of accretion by the black hole caused the surrounding plasma to brighten suddenly for the first time since 1989, briefly becoming the brightest x-ray source in the sky. Dallilar et al. combined observations from radio, infrared, optical, and x-ray telescopes taken during the outburst. They compared how fast the flux decayed at each wavelength, which allowed them to constrain the size of the emitting region, determine that the plasma within it cooled through synchrotron radiation, and measure the magnetic field around the black hole. Science , this issue p. 1299

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Section: Radio Observationsmentioning

confidence: 99%

A precise measurement of the magnetic field in the corona of the black hole binary V404 Cygni

Dallilar

Eikenberry

Garner

et al. 2017

Science

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“…Otherwise the reported peak fluxes are obtained by performing forced Gaussian fits at the position of either the radio counterpart seen in another AMI epoch, or at the best known Swift position of the GRB. The flux errors are the errors output by PYSE, added in quadrature to the AMI 5% calibration error (Perrott et al 2013) and are also primary beam corrected. The significance of the peak fluxes reported by PYSE are also included in these Tables.…”

Section: The Ami Grb Cataloguementioning

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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“…drive-ami utilises the REDUCE software package, which is designed to take the raw AMI-LA data and automatically flag for interference, shadowing, and hardware errors, conduct phase and amplitude calibrations, and Fourier transforms the data into uv -FITS format (Perrott et al 2013). Short, interleaved observations of J1856+0610 were used for phase calibration.…”

Section: Ami-lamentioning

confidence: 99%

“…Imaging was conducted using the chimenea data reduction pipeline that has been specifically designed to deal with multi-epoch radio observations of transients (Staley & Anderson 2015). The resulting peak AMI-LA flux densities of XTE J1908+094 (Table 1) were measured using MIRIAD (Sault et al 1995) and systematic errors of 5% (Perrott et al 2013) should be added in quadrature. Note that the flux errors may be underestimated due to uncleanable artefacts resulting from the nearby off-axis radio-bright source that may be associated with the star forming region W49A (Webster et al 1971).…”

Section: Ami-lamentioning

confidence: 99%

Radio polarimetry as a probe of unresolved jets: the 2013 outburst of XTE J1908+094

Curran

Miller-Jones

Rushton

et al. 2015

Mon. Not. R. Astron. Soc.

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XTE J1908+094 is an X-ray transient black hole candidate in the Galactic plane that was observed in outburst in 2002 and 2013. Here we present multi-frequency radio and X-ray data, including radio polarimetry, spanning the entire period of the 2013 outburst. We find that the X-ray behaviour of XTE J1908+094 traces the standard black hole hardness-intensity path, evolving from a hard state, through a soft state, before returning to a hard state and quiescence. Its radio behaviour is typical of a compact jet that becomes quenched before discrete ejecta are launched during the late stages of X-ray softening. The radio and X-ray fluxes, as well as the light curve morphologies, are consistent with those observed during the 2002 outburst of this source. The polarisation angle during the rise of the outburst infers a jet orientation in agreement with resolved observations but also displays a gradual drift, which we associate with observed changes in the structure of the discrete ejecta. We also observe an unexpected 90• rotation of the polarisation angle associated with a second component.

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AMI Galactic Plane Survey at 16 GHz - I. Observing, mapping and source extraction

Cited by 53 publications

References 35 publications

A precise measurement of the magnetic field in the corona of the black hole binary V404 Cygni

A precise measurement of the magnetic field in the corona of the black hole binary V404 Cygni

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

Radio polarimetry as a probe of unresolved jets: the 2013 outburst of XTE J1908+094

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