10C survey of radio sources at 15.7 GHz - I. Observing, mapping and source extraction★

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

doi:10.1111/j.1365-2966.2011.18887.x

Cited by 46 publications

(6 citation statements)

References 16 publications

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“…At the central operating frequency of 15.7 GHz, AMI has a primary beam of 5.5 arcmin and a ≈ 30 arcsec resolution (Zwart et al 2008). During each AMI observation a bright unresolved source within a few degrees of the target of interest is visited for 1 minute in every 11 minutes to provide phase and amplitude calibration (for further details on the absolute flux calibration of AMI see Franzen et al 2011).…”

Section: Ami Strategy and Observationsmentioning

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: Ami Strategy and Observationsmentioning

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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“…However, several recent surveys have allowed for huge advances in the understanding of the radio sky at greater than 10 GHz (e.g. 10C at 15.7 GHz, Franzen et al 2011;AT20G at 20 GHz, Murphy et al 2010 and the AT20-deep (pilot) also at 20 GHz, Massardi et al 2011;Franzen et al 2014). Consequently, only a few of the brightest BCGs have well-characterized radio-spectra in this crucial spectral range.…”

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confidence: 99%

High radio-frequency properties and variability of brightest cluster galaxies

Hogan¹,

Edge²,

Geach³

et al. 2015

Mon. Not. R. Astron. Soc.

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Citation for published item:rognD wFF nd idgeD eFgF nd qehD tFiF nd qringeD uFtFfF nd rlvekEvrrondoD tF nd rovttD F nd urimD eF nd wxmrD fFF nd umseyD gF nd ussellD rFF nd lom¡ eD F nd ellerD rFhF nd ellerD wFpF nd fenfordD hFtF nd pinD eFgF nd edhedD eFgFF nd dlerD iFwF nd undersD FhFiF @PHISA 9righ rdioEfrequeny properties nd vriility of rightest luster glxiesF9D wonthly noties of the oyl estronomil oietyFD RSQ @PAF ppF IPPQEIPRHF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe consider the high radio-frequency (15-353 GHz) properties and variability of 35 brightest cluster galaxies (BCGs). These are the most core-dominated sources drawn from a parent sample of more than 700 X-ray selected clusters, thus allowing us to relate our results to the general population. We find that ≥6.0 per cent of our parent sample (≥15.1 per cent if only cool-core clusters are considered) contain a radio source at 150 GHz of at least 3 mJy (≈1×10 23 W Hz −1 at our median redshift of z ≈ 0.13). Furthermore, ≥3.4 per cent of the BCGs in our parent sample contain a peaked component (Gigahertz Peaked Spectrum, GPS) in their spectra that peaks above 2 GHz, increasing to ≥8.5 per cent if only cool-core clusters are considered. We see little evidence for strong variability at 15 GHz on short (week-month) time-scales although we see variations greater than 20 per cent at 150 GHz over six-month time frames for 4 of the 23 sources with multi-epoch observations. Much more prevalent is long-term (year-decade time-scale) variability, with average annual amplitude variations greater than 1 per cent at 15 GHz being commonplace. There is a weak trend towards higher variability as the peak of the GPS-like component occurs at higher frequency. We demonstrate the complexity that is seen in the radio spectra of BCGs and discuss the potentially significant implications of these high-peaking components for Sunyaev-Zel'dovich cluster searches.

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“…We extracted source components from the two AT-LAS fields using BLOBCAT , AEGEAN , pyBDSM 3 and the AMI SOURCE FIND software (AMI Consortium: Franzen et al 2011). When using BLOBCAT, AEGEAN and pyBDSM, we searched both mosaics down to an SNR 4 in order to include all sources with fitted peak SNRs 5.…”

Section: Source Extractionmentioning

confidence: 99%

ATLAS – I. Third release of 1.4 GHz mosaics and component catalogues

Franzen

Banfield

Hales

et al. 2015

Mon. Not. R. Astron. Soc.

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We present the third data release from the Australia Telescope Large Area Survey (ATLAS). These data combine the observations at 1.4 GHz before and after upgrades to the Australia Telescope Compact Array reaching a sensitivity of 14 µJy beam −1 in 3.6 deg 2 over the Chandra Deep Field South (CDFS) and of 17 µJy beam −1 in 2.7 deg 2 over the European Large Area ISO Survey South 1 (ELAIS-S1). We used a variety of array configurations to maximise the uv coverage resulting in a resolution of 16 by 7 arcsec in CDFS and of 12 by 8 arcsec in ELAIS-S1. After correcting for peak bias and bandwidth smearing, we find a total of 3034 radio source components above 5σ in CDFS, of which 514 (17 per cent) are considered to be extended. The number of components detected above 5σ in ELAIS-S1 is 2084, of which 392 (19 per cent) are classified as extended. The catalogues include reliable spectral indices (∆α < 0.2) between 1.40 and 1.71 GHz for ∼ 350 of the brightest components.

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10C survey of radio sources at 15.7 GHz - I. Observing, mapping and source extraction★

Cited by 46 publications

References 16 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

High radio-frequency properties and variability of brightest cluster galaxies

ATLAS – I. Third release of 1.4 GHz mosaics and component catalogues

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