A Deep Radio Survey of Hard State and Quiescent Black Hole X-Ray Binaries

Miller-Jones, J. C. A.; Jonker, P. G.; Maccarone, Thomas J.; Nelemans, G.; Calvelo, D. E.

doi:10.1088/2041-8205/739/1/l18

Cited by 53 publications

(62 citation statements)

References 43 publications

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“…Along with a level of emission of 3.7 ± 1.4 µJy, determined combining six observations at the different orbital phases Φ = 0.58-0.72 and Φ = 0.15-0.30, we detected in a single observation around apastron (Φ = 0.49) the flux density of 14.2 ± 2.9 µJy. Several works have placed significant constrains on the L X -L R luminosities of quiescent systems (e.g., Gallo et al 2006;Gallo et al 2014;Calvelo et al 2010;Miller-Jones et al 2011). The nonsimultaneous XMM-Newton X-ray observation by Munar-Adrover et al (2014) at orbital phase Φ = 0.08, also allowed us to test for MWC 656 the X-ray/radio correlation for black holes.…”

Section: Discussionmentioning

confidence: 99%

Radio emission from the Be/black hole binary MWC 656

Dzib

Massi

Jaron

2015

A&A

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Context. MWC 656 is the recently discovered first binary system case composed of a Be-type star and an accreting black hole. Its low X-ray luminosity indicates that the system is in a quiescent X-ray state. Aims. The aim of our investigation is to establish if the MWC 656 system has detectable radio emission and if the radio characteristics are consistent with those of quiescent black hole systems. Methods. We used three archived VLA data sets, one hour each at 3 GHz, and seven new VLA observations, two hours each at 10 GHz, to produce very high sensitivity images down to ∼1 µJy. Results. We detected the source twice in the new observations: in the first VLA run, at apastron passage, with a flux density of 14.2 ± 2.9 µJy and by combining all together the other six VLA runs, with a flux density of 3.7 ± 1.4 µJy. The resulting combined map of the archived observations has the sensitivity of 1σ = 6.6 µJy, but no radio emission is detected there. Conclusions. The radio and X-ray luminosities agree with the behaviour of accreting binary black holes in the hard and quiescent state. In particular, MWC 656 in the L X , L R plane occupies the same region as A0620−00 and XTE J1118+480, the faintest known black holes up to now.

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Section: Discussionmentioning

confidence: 99%

Radio emission from the Be/black hole binary MWC 656

Dzib

Massi

Jaron

2015

A&A

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“…Xie, Yang & Ma 2014;Markoff et al 2015;Plotkin et al 2015Plotkin et al , 2016. Several X-ray binaries have confirmed radio detections in quiescence (Gallo, Fender & Hynes 2005;Gallo et al 2006Gallo et al , 2014Miller-Jones et al 2011Strader et al 2012;Chomiuk et al 2013;Dzib, Massi, & Jaron 2015;Tetarenko et al 2016) and they are all black hole candidate systems. Spectral evidence for synchrotron emission in the optical-infrared (OIR) regime in quiescence has been found in some black hole LMXBs (Gallo et al 2007;Gelino, Gelino & Harrison 2010;Froning et al 2011;Shahbaz et al 2013;Plotkin et al 2016) and one neutron star system (Baglio et al 2013).…”

Section: Introductionmentioning

confidence: 98%

Polarized synchrotron emission in quiescent black hole X-ray transients

Russell¹,

Shahbaz²,

Lewis³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present near-infrared polarimetric observations of the black hole X-ray binaries Swift J1357.2-0933 and A0620-00. In both sources, recent studies have demonstrated the presence of variable infrared synchrotron emission in quiescence, most likely from weak compact jets. For Swift J1357.2-0933 we find that the synchrotron emission is polarized at a level of 8.0 ± 2.5 per cent (a 3.2 σ detection of intrinsic polarization). The mean magnitude and rms variability of the flux (fractional rms of 19-24 per cent in K S -band) agree with previous observations. These properties imply a continuously launched (stable on long timescales), highly variable (on short timescales) jet in the Swift J1357.2-0933 system in quiescence, which has a moderately tangled magnetic field close to the base of the jet. We find that for A0620-00, there are likely to be three components to the optical-infrared polarization; interstellar dust along the line of sight, scattering within the system, and an additional source that changes the polarization position angle in the reddest (H and K S ) wave-bands. We interpret this as a stronger contribution of synchrotron emission, and by subtracting the line-of-sight polarization, we measure an excess of ∼ 1.25±0.28 per cent polarization and a position angle of the magnetic field vector that is consistent with being parallel with the axis of the resolved radio jet. These results imply that weak jets in low luminosity accreting systems have magnetic fields which possess similarly tangled fields compared to the more luminous, hard state jets in X-ray binaries.

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“…Our currently limited knowledge on quiescent BHXB accretion flows/jets stems primarily from their low luminosities levels, combined with the small number of known BHXBs located close to the Earth (e.g., Calvelo et al 2010;Miller-Jones et al 2011). There are currently only three lowmass BHXB systems (with a confirmed black hole accretor) that have meaningful, simultaneous radio and X-ray constraints on their jets in quiescence, V404 Cyg (LX /L Edd ≈ 10 −6 ; Hjellming et al 2000;Gallo, Fender & Hynes 2005;Hynes et al 2009), A0620−00 (LX /L Edd ≈ 10 −8.5 ; Gallo et al 2006), and XTE J1118+480 (LX /L Edd ≈ 10 −8.5 ; Gallo et al 2014).…”

Section: Introductionmentioning

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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A Deep Radio Survey of Hard State and Quiescent Black Hole X-Ray Binaries

Cited by 53 publications

References 43 publications

Radio emission from the Be/black hole binary MWC 656

Radio emission from the Be/black hole binary MWC 656

Polarized synchrotron emission in quiescent black hole X-ray transients

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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