The Arcminute Microkelvin Imager<sup>★</sup>

Zwart, Jonathan T. L.; Barker, R. W.; Biddulph, P.; Bly, Dennis; Boysen, Roger C.; Brown, A.; Clementson, Christopher; Crofts, M.; Culverhouse, T.; Czeres, J.; Dace, Roger; Davies, Matthew; D'Alessandro, R.; Doherty, Peter; Duggan, Kenneth; Ely, John; Felvus, Mike; Feroz, Farhan; Flynn, W.; Franzen, T. M. O.; Geisbüsch, Jörn; Génova-Santos, R. T.; Grainge, Keith; Grainger, William F.; Hammett, D.; Hills, R. E.; Hobson, M.; Holler, C. M.; Hurley‐Walker, N.; Jilley, R.; Jones, Michael E.; Kaneko, T.; Kneißl, R.; Lancaster, Katy; Lasenby, A.; Marshall, Phil; Newton, F.; Norris, O.; Northrop, I.; Odell, D. M.; Petencin, G.; Pober, Jonathan C.; Pooley, G. G.; Pospieszalski, M.W.; Quy, V.; Rodríguez‐Gonzálvez, Carmen; Saunders, Richard D. E.; Scaife, Anna M. M.; Schofield, Jack; Scott, Paul F.; Shaw, Clive; Shimwell, T. W.; Smith, Harry; Taylor, Angela C.; Titterington, D.; Velić, M.; Waldram, Elizabeth; West, S. C.; Wood, B. A.; Yassin, G.

doi:10.1111/j.1365-2966.2008.13953.x

Cited by 203 publications

(108 citation statements)

References 51 publications

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“…We take advantage of the large set of measurements provided by the AMI Large array (Cambridge, UK), consisting of a set of eight 13-m antennas with a maximum baseline of ∼120 m. AMI observations are conducted with a 6-GHz bandwidth centred at 15 GHz (Zwart et al 2008). We also used the 11.2-GHz data of Cyg X-3 from a monitoring programme (Trushkin et al 2006) with the RATAN-600 telescope located near Zelenchurskaya village on the North Caucas (Russia).…”

Section: Radiomentioning

confidence: 99%

A giant radio flare from Cygnus X-3 with associated γ-ray emission

Corbel

Dubus

Tomsick

et al. 2012

Monthly Notices of the Royal Astronomical Society

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With frequent flaring activity of its relativistic jets, Cygnus X‐3 (Cyg X‐3) is one of the most active microquasars and is the only Galactic black hole candidate with confirmed high‐energy γ‐ray emission, thanks to detections by Fermi Large Area Telescope (Fermi/LAT) and AGILE. In 2011, Cyg X‐3 was observed to transit to a soft X‐ray state, which is known to be associated with high‐energy γ‐ray emission. We present the results of a multiwavelength campaign covering a quenched state, when radio emission from Cyg X‐3 is at its weakest and the X‐ray spectrum is very soft. A giant (∼20 Jy) optically thin radio flare marks the end of the quenched state, accompanied by rising non‐thermal hard X‐rays. Fermi/LAT observations (E≥ 100 MeV) reveal renewed γ‐ray activity associated with this giant radio flare, suggesting a common origin for all non‐thermal components. In addition, current observations unambiguously show that the γ‐ray emission is not exclusively related to the rare giant radio flares. A three‐week period of γ‐ray emission is also detected when Cyg X‐3 was weakly flaring in radio, right before transition to the radio quenched state. No γ‐rays are observed during the ∼1‐month long quenched state, when the radio flux is weakest. Our results suggest transitions into and out of the ultrasoft X‐ray (radio‐quenched) state trigger γ‐ray emission, implying a connection to the accretion process, and also that the γ‐ray activity is related to the level of radio flux (and possibly shock formation), strengthening the connection to the relativistic jets.

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Section: Radiomentioning

confidence: 99%

A giant radio flare from Cygnus X-3 with associated γ-ray emission

Corbel

Dubus

Tomsick

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…The next generation of CMB instruments is currently being commissioned, and is expected to provide more data at multipoles comparable to those probed by the CBI. The Planck spacecraft will measure the power spectrum from the whole sky out to multipoles of 2500 within the next few years, and instruments such as the South Pole Telescope (Ruhl et al 2004), the Arcminute Microkelvin Imager (Zwart et al 2008) and the Atacama Cosmology Telescope (Fowler 2004) will observe large numbers of galaxy clusters using the SZ effect. These measurements will provide much more information on the SZ effect and may provide a resolution to the discrepancy in σ 8 from the measurements to date.…”

Section: O N C L U S I O N Smentioning

confidence: 99%

Statistics of the Sunyaev-Zel'dovich effect power spectrum

Peel¹,

Battye²,

Kay³

2009

Monthly Notices of the Royal Astronomical Society

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Using large numbers of simulations of the microwave sky, incorporating the cosmic microwave background (CMB) and the Sunyaev–Zel'dovich (SZ) effect due to clusters, we investigate the statistics of the power spectrum at microwave frequencies between spherical multipoles of 1000 and 10 000. From these virtual sky maps, we find that the spectrum of the SZ effect has a larger standard deviation by a factor of 3 than would be expected from purely Gaussian realizations, and has a distribution that is significantly skewed towards higher values, especially when small map sizes are used. The standard deviation is also increased by around 10 per cent compared to the trispectrum calculation due to the clustering of galaxy clusters. We also consider the effects of including residual point sources and uncertainties in the gas physics. This has implications for the excess power measured in the CMB power spectrum by the Cosmic Background Imager (CBI) and Berkeley–Illinois–Maryland Association (BIMA) experiments. Our results indicate that the observed excess could be explained using a lower value of σ8 than previously suggested, however the effect is not enough to match σ8= 0.825. The uncertainties in the gas physics could also play a substantial role. We have made our maps of the SZ effect available online.

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“…Next, we present extensive follow-up observations, including R-band photometry from the P48, multicolor photometry from the P60, spectroscopy (acquired with the P200, Keck, Gemini, APO, Magellan, Very Large Telescope (VLT), and GTC), and radio observations with the Very Large Array 35 (VLA), the Combined Array for Research in Millimeter-wave Astronomy (CARMA; Bock et al 2006;Corder et al 2010), the Australia Telescope Compact Array (ATCA; Frater et al 1992), and the Arcminute Microkelvin Imager (AMI; Zwart et al 2008). We provide basic physical interpretations of the broadband spectral energy distributions (SEDs)of these afterglows.…”

Section: Introductionmentioning

confidence: 99%

THE NEEDLE IN THE 100 deg²HAYSTACK: UNCOVERING AFTERGLOWS OFFERMIGRBs WITH THE PALOMAR TRANSIENT FACTORY

Singer

Kasliwal

Cenko

et al. 2015

ApJ

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The Fermi Gamma-ray Space Telescope has greatly expanded the number and energy window of observations of gamma-ray bursts (GRBs). However, the coarse localizations of tens to a hundred square degrees provided by the Fermi GRB Monitor instrument have posed a formidable obstacle to locating the bursts' host galaxies, measuring their redshifts, and tracking their panchromatic afterglows. We have built a target-of-opportunity mode for the intermediate Palomar Transient Factory in order to perform targeted searches for Fermi afterglows. Here, we present the results of one year of this program: 8 afterglow discoveries out of 35 searches. Two of the bursts with detected afterglows (GRBs 130702A and 140606B) were at low redshift (z = 0.145 and 0.384, respectively) and had spectroscopically confirmed broad-line Type Ic supernovae. We present our broadband follow-up including spectroscopy as well as X-ray, UV, optical, millimeter, and radio observations. We study possible selection effects in the context of the total Fermi and Swift GRB samples. We identify one new outlier on the Amati relation. We find that two bursts are consistent with a mildly relativistic shock breaking out from the progenitor star rather than the ultra-relativistic internal shock mechanism that powers standard cosmological bursts. Finally, in the context of the Zwicky Transient Facility, we discuss how we will continue to expand this effort to find optical counterparts of binary neutron starmergers that may soon be detected by Advanced LIGO and Virgo.

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The Arcminute Microkelvin Imager^★

Cited by 203 publications

References 51 publications

A giant radio flare from Cygnus X-3 with associated γ-ray emission

A giant radio flare from Cygnus X-3 with associated γ-ray emission

Statistics of the Sunyaev-Zel'dovich effect power spectrum

THE NEEDLE IN THE 100 deg²HAYSTACK: UNCOVERING AFTERGLOWS OFFERMIGRBs WITH THE PALOMAR TRANSIENT FACTORY

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About

The Arcminute Microkelvin Imager★

Cited by 203 publications

References 51 publications

A giant radio flare from Cygnus X-3 with associated γ-ray emission

A giant radio flare from Cygnus X-3 with associated γ-ray emission

Statistics of the Sunyaev-Zel'dovich effect power spectrum

THE NEEDLE IN THE 100 deg2HAYSTACK: UNCOVERING AFTERGLOWS OFFERMIGRBs WITH THE PALOMAR TRANSIENT FACTORY

Contact Info

Product

Resources

About

The Arcminute Microkelvin Imager^★

THE NEEDLE IN THE 100 deg²HAYSTACK: UNCOVERING AFTERGLOWS OFFERMIGRBs WITH THE PALOMAR TRANSIENT FACTORY