Limits on the quiescent radio emission from the black hole binaries GRO J1655−40 and XTE J1550−564

Calvelo, D. E.; Fender, R. P.; Russell, D. M.; Gallo, Elena; Corbel, S.; Tzioumis, A. K.; Bell, M. E.; Lewis, Fraser; Maccarone, Thomas J.

doi:10.1111/j.1365-2966.2010.17348.x

Cited by 31 publications

(43 citation statements)

References 45 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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“…This may not be the case though for all black-hole XRBs in the quiescent state. For example, for GRO J1655-40 and XTE J1550-564, upper limits on the radio emission in the quiescent state were placed (Calvelo et al 2010). In the source V404 Cyg, the radio emission is, in contrast, stronger than expected in the quiescent state (Gallo et al 2005).…”

Section: Jets In Black-hole X-ray Binariesmentioning

confidence: 99%

Formation and destruction of jets in X-ray binaries

Kylafis

Contopoulos

Kazanas

et al. 2012

A&A

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Context. Neutron-star and black-hole X-ray binaries (XRBs) exhibit radio jets, whose properties depend on the X-ray spectral state and history of the source. In particular, black-hole XRBs emit compact, steady radio jets when they are in the so-called hard state. These jets become eruptive as the sources move toward the soft state, disappear in the soft state, and then re-appear when the sources return to the hard state. The jets from neutron-star X-ray binaries are typically weaker radio emitters than the black-hole ones at the same X-ray luminosity and in some cases radio emission is detected in the soft state. Aims. Significant phenomenology has been developed to describe the spectral states of neutron-star and black-hole XRBs, and there is general agreement about the type of the accretion disk around the compact object in the various spectral states. We investigate whether the phenomenology describing the X-ray emission on one hand and the jet appearance and disappearance on the other can be put together in a consistent physical picture. Methods. We consider the so-called Poynting-Robertson cosmic battery (PRCB), which has been shown to explain in a natural way the formation of magnetic fields in the disks of AGNs and the ejection of jets. We investigate whether the PRCB can also explain the formation, destruction, and variability of jets in XRBs. Results. We find excellent agreement between the conditions under which the PRCB is efficient (i.e., the type of the accretion disk) and the emission or destruction of the radio jet. Conclusions. The disk-jet connection in XRBs can be explained in a natural way using the PRCB.

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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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Limits on the quiescent radio emission from the black hole binaries GRO J1655−40 and XTE J1550−564

Cited by 31 publications

References 45 publications

Radio emission from the Be/black hole binary MWC 656

Radio emission from the Be/black hole binary MWC 656

Formation and destruction of jets in X-ray binaries

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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