Radio emission from the Be/black hole binary MWC 656

Dzib, S. A.; Massi, M.; Jaron, F.

doi:10.1051/0004-6361/201526867

Cited by 27 publications

(35 citation statements)

References 22 publications

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“…Romero et al 2007). The fact that MWC 656 seems to adhere to the low-luminosity end of the X-ray/radio correlation for hard state compact jets also points in this direction (Dzib et al 2015).…”

Section: Discussionmentioning

confidence: 87%

Optical spectroscopy of Be/gamma-ray binaries

Zamanov

Stoyanov

Martı́

et al. 2016

A&A

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We report optical spectroscopic observations of the Be/γ-ray binaries LSI+61303, MWC 148 and MWC 656. The peak separation and equivalent widths of prominent emission lines (Hα, Hβ, Hγ, HeI, and FeII) are measured. We estimated the circumstellar disc size, compared it with separation between the components, and discussed the disc truncation. We find that in LSI+61• 303 the compact object comes into contact with the outer parts of the circumstellar disc at periastron, in MWC 148 the compact object goes deeply into the disc during the periastron passage, and in MWC 656 the black hole is accreting from the outer parts of the circumstellar disc along the entire orbit. The interstellar extinction was estimated using interstellar lines. The rotation of the mass donors appears to be similar to the rotation of the mass donors in Be/X-ray binaries. We suggest that X-ray/optical periodicity ∼1 day deserves to be searched for.

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Section: Discussionmentioning

confidence: 87%

Optical spectroscopy of Be/gamma-ray binaries

Zamanov

Stoyanov

Martı́

et al. 2016

A&A

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“…15 The position of MWC656 in Figure3 of Dzib et al (2015) is based on their VLA data obtained in 2015 Feb-Apr and the non-simultaneous XMM-Newton data obtained in 2013 June. In addition, our Chandra observation shows that the XMM-Newton flux corresponds to two sources and that the X-ray luminosity of MWC656 is significantly variable.…”

Section: Discussionmentioning

confidence: 99%

“…Recently, Dzib et al (2015) have reported a detection with VLA at a peak flux density of 10±3μJy beam −1 . Observations at TeV energies with the MAGIC telescopes have only led to upper limits (Aleksić et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The First Simultaneous X-Ray/Radio Detection of the First Be/BH System MWC 656

Ribó

Munar-Adrover

Paredes

et al. 2017

ApJL

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MWC656 is the first known Be/black hole (BH) binary system. Be/BH binaries are important in the context of binary system evolution and sources of detectable gravitational waves because they are possible precursors of coalescing neutron star/BH binaries. X-ray observations conducted in 2013 revealed that MWC656 is a quiescent high-mass X-ray binary (HMXB), opening the possibility to explore X-ray/radio correlations and the accretion/ ejection coupling down to low luminosities for BH HMXBs. Here we report on a deep joint Chandra/VLA observation of MWC656 (and contemporaneous optical data) conducted in 2015 July that has allowed us to unambiguously identify the X-ray counterpart of the source. The X-ray spectrum can be fitted with a power law with Γ∼2, providing a flux of ;4×10 −15 ergcm −2 s −1 in the 0.5-8keV energy range and a luminosity of L X ;3×10 30 ergs −1 at a 2.6kpc distance. For a 5M e BH this translates into ;5×10 −9 L Edd . These results imply that MWC656 is about 7 times fainter in X-rays than it was two years before and reaches the faintest X-ray luminosities ever detected in stellar-mass BHs. The radio data provide a detection with a peak flux density of 3.5±1.1μJybeam −1 . The obtained X-ray/radio luminosities for this quiescent BH HMXB are fully compatible with those of the X-ray/radio correlations derived from quiescent BH low-mass X-ray binaries. These results show that the accretion/ejection coupling in stellar-mass BHs is independent of the nature of the donor star.

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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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Radio emission from the Be/black hole binary MWC 656

Cited by 27 publications

References 22 publications

Optical spectroscopy of Be/gamma-ray binaries

Optical spectroscopy of Be/gamma-ray binaries

The First Simultaneous X-Ray/Radio Detection of the First Be/BH System MWC 656

Polarized synchrotron emission in quiescent black hole X-ray transients

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