AN ACCURATE FLUX DENSITY SCALE FROM 1 TO 50 GHz

Perley, R. A.; Butler, B. J.

doi:10.1088/0067-0049/204/2/19

Cited by 428 publications

(371 citation statements)

References 24 publications

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“…The gains for all the calibrators were then combined, solving for the J0011-2612 flux density. We used the flux scale of Perley & Butler (2013). As a final step all relevant calibration solutions were applied to the target field data (A2744).…”

Section: Vla Observationsmentioning

confidence: 99%

VLA Radio Observations of the HST Frontier Fields Cluster Abell 2744: The Discovery of New Radio Relics

Pearce

Weeren

Andrade-Santos

et al. 2017

ApJ

117

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Cluster mergers leave distinct signatures in the intracluster medium (ICM) in the form of shocks and diffuse cluster radio sources that provide evidence for the acceleration of relativistic particles. However, the physics of particle acceleration in the ICM is still not fully understood. Here we present new 1-4 GHz Jansky Very Large Array (VLA) and archival Chandra observations of the HST Frontier Fields Cluster Abell2744. In our new VLA images, we detect the previously known ∼2.1Mpc radio halo and ∼1.5Mpc radio relic. We carry out a radio spectral analysis from which we determine the relic's injection spectral index to be a = - 1.12 0. 0.31 under the assumption of diffusive shock acceleration. We also find evidence for spectral steepening in the post-shock region. We do not find evidence for a significant correlation between the radio halo's spectral index and ICM temperature. In addition, we observe three new polarized diffuse sources and determine two of these to be newly discovered giant radio relics. These two relics are located in the southeastern and northwestern outskirts of the cluster. The corresponding integrated spectral indices measure −1.81±0.26 and −0.63±0.21 for the SE and NW relics, respectively. From an X-ray surface brightness profile we also detect a possible density jump of = -+ R 1.39 0.22 0.34 co-located with the newly discovered SE relic. This density jump would correspond to a shock front Mach number of  = -+ 1.26 0.15 0.25 .

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Section: Vla Observationsmentioning

confidence: 99%

VLA Radio Observations of the HST Frontier Fields Cluster Abell 2744: The Discovery of New Radio Relics

Pearce

Weeren

Andrade-Santos

et al. 2017

ApJ

117

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“…The data were Hanning smoothed, and then edited to remove radio frequency interference. Bandpass calibration was carried out before the amplitude and phase gains were derived for both calibrator sources, using the 'Perley-Butler 2010' coefficients within the CASA task SETJY to set the amplitude scale (Perley & Butler 2013). The complex gain solutions derived for the secondary calibrator were interpolated to the target source, before averaging the resulting calibrated data by a factor of three in frequency to reduce the data volume.…”

Section: Karl G Jansky Very Large Arraymentioning

confidence: 99%

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

Gallo¹,

Miller-Jones²,

Russell³

et al. 2014

Monthly Notices of the Royal Astronomical Society

154

200

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We report on deep, coordinated radio and X-ray observations of the black hole X-ray binary XTE J1118+480 in quiescence. The source was observed with the Karl G. Jansky Very Large Array for a total of 17.5 hrs at 5.3 GHz, yielding a 4.8±1.4 µJy radio source at a position consistent with the binary system. At a distance of 1.7 kpc, this corresponds to an integrated radio luminosity between 4-8 ×10 25 erg s −1 , depending on the spectral index. This is the lowest radio luminosity measured for any accreting black hole to date. Simultaneous observations with the Chandra X-ray Telescope detected XTE J1118+480 at 1.2 × 10 −14 erg s −1 cm −2 (1-10 keV), corresponding to an Eddington ratio of ∼4 × 10 −9 for a 7.5 M black hole. Combining these new measurements with data from the 2005 and 2000 outbursts available in the literature, we find evidence for a relationship of the form r =α+β X (where denotes logarithmic luminosities), with β = 0.72 ± 0.09. XTE J1118+480 is thus the third system -together with GX339-4 and V404 Cyg -for which a tight, non-linear radio/X-ray correlation has been reported over more than 5 dex in X . Confirming previous results, we find no evidence for a dependence of the correlation normalisation of an individual system on orbital parameters, relativistic boosting, reported black hole spin and/or black hole mass. We then perform a clustering and linear regression analysis on what is arguably the most up-to-date collection of coordinated radio and X-ray luminosity measurements from quiescent and hard state black hole X-ray binaries, including 24 systems. At variance with previous results, a two-cluster description is statistically preferred only for random errors < ∼ 0.3 dex in both r and X , a level which we argue can be easily reached when the known spectral shape/distance uncertainties and intrinsic variability are accounted for. A linear regression analysis performed on the whole data set returns a best-fitting slope β = 0.61 ± 0.03 and intrinsic scatter σ 0 = 0.31 ± 0.03 dex.

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“…The data were processed using the Common Astronomy Software Application (CASA; McMullin et al 2007). We used 3C 286 to set the amplitude scale according to the Perley & Butler (2013) coefficients within CASA's setjy task, and we used the extragalactic calibrator source J1408-0752 to determine the complex gain solutions in the direction of the target. Our on-source time was 508 min.…”

Section: Radio Observationsmentioning

confidence: 99%

A clean sightline to quiescence: multiwavelength observations of the high Galactic latitude black hole X-ray binary Swift J1357.2−0933

Plotkin

Gallo

Jonker

et al. 2015

Mon. Not. R. Astron. Soc.

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We present coordinated multiwavelength observations of the high Galactic latitude (b=+50 • ) black hole X-ray binary (BHXB) Swift J1357.2−0933 in quiescence. Our broadband spectrum includes strictly simultaneous radio and X-ray observations, and near-infrared, optical, and ultraviolet data taken 1-2 days later. We detect Swift J1357.2−0933 at all wavebands except for the radio (f 5GHz <3.9 µJy beam −1 ; 3σ rms ). Given current constraints on the distance (2.3-6.3 kpc), its 0.5-10 keV X-ray flux corresponds to an Eddington ratio L X /L Edd = 4 × 10 −9 − 3 × 10 −8 (assuming a black hole mass of 10M ⊙ ). The broadband spectrum is dominated by synchrotron radiation from a relativistic population of outflowing thermal electrons, which we argue to be a common signature of short-period quiescent BHXBs. Furthermore, we identify the frequency where the synchrotron radiation transitions from optically thick-to-thin (ν b ≈ 2 − 5 × 10 14 Hz, which is the most robust determination of a 'jet break' for a quiescent BHXB to date. Our interpretation relies on the presence of steep curvature in the ultraviolet spectrum, a frequency window made observable by the low amount of interstellar absorption along the line of sight. High Galactic latitude systems like Swift J1357.2−0933 with clean ultraviolet sightlines are crucial for understanding black hole accretion at low luminosities.

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AN ACCURATE FLUX DENSITY SCALE FROM 1 TO 50 GHz

Cited by 428 publications

References 24 publications

VLA Radio Observations of the HST Frontier Fields Cluster Abell 2744: The Discovery of New Radio Relics

VLA Radio Observations of the HST Frontier Fields Cluster Abell 2744: The Discovery of New Radio Relics

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

A clean sightline to quiescence: multiwavelength observations of the high Galactic latitude black hole X-ray binary Swift J1357.2−0933

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