An H <scp>i</scp> absorption distance to the black hole candidate X-ray binary MAXI J1535–571

Chauhan, Jaiverdhan; Miller-Jones, J. C. A.; Anderson, G. E.; Raja, Wasim; Bahramian, A.; Hotan, A. W.; Indermuehle, B.; Whiting, M. T.; Allison, J. R.; Anderson, Craig S.; Bunton, John D.; Koribalski, B. S.; Mahony, E. K.

doi:10.1093/mnrasl/slz113

Cited by 35 publications

(35 citation statements)

References 32 publications

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“…Tomsick et al 2014;Shaw et al 2016). We note that our luminosity estimations assumed the most likely distance value of 4.1 kpc from Chauhan et al (2019). However, these authors also estimated an upper limit for the distance of ∼7 kpc, which results in peak luminosities of ≤ 2×10 37 erg s −1 for the reflares [Sridhar et al (2019) estimated a distance of 5.4 +1.8 −1.1 kpc, which lies between the above-mentioned values].…”

Section: Outburst Reflares Of Maxi J1535-571: the State Transition Identificationsupporting

confidence: 59%

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A NICER look at the state transitions of the black hole candidate MAXI J1535−571 during its reflares

Cúneo

Alabarta

Zhang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The black hole candidate and X-ray binary MAXI J1535−571 was discovered in 2017 September. During the decay of its discovery outburst, and before returning to quiescence, the source underwent at least four reflaring events, with peak luminosities of ∼1035–36 erg s−1 (d/4.1 kpc)2. To investigate the nature of these flares, we analysed a sample of NICER (Neutron star Interior Composition Explorer) observations taken with almost daily cadence. In this work, we present the detailed spectral and timing analysis of the evolution of the four reflares. The higher sensitivity of NICER at lower energies, in comparison with other X-ray detectors, allowed us to constrain the disc component of the spectrum at ∼0.5 keV. We found that during each reflare the source appears to trace out a q-shaped track in the hardness–intensity diagram similar to those observed in black hole binaries during full outbursts. MAXI J1535−571 transits between the hard state (valleys) and softer states (peaks) during these flares. Moreover, the Comptonized component is undetected at the peak of the first reflare, while the disc component is undetected during the valleys. Assuming the most likely distance of 4.1 kpc, we find that the hard-to-soft transitions take place at the lowest luminosities ever observed in a black hole transient, while the soft-to-hard transitions occur at some of the lowest luminosities ever reported for such systems.

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Section: Outburst Reflares Of Maxi J1535-571: the State Transition Identificationsupporting

confidence: 59%

“…We estimated 1σ errors for all the spectral parameters. X-ray luminosities were estimated from the unabsorbed flux, calculated with the cflux convolution model within xspec (0.5−10 keV), assuming a distance of 4.1 +0.6 −0.5 kpc (Chauhan et al 2019), a value we adopt from now on.…”

Section: Energy Spectramentioning

confidence: 99%

A NICER look at the state transitions of the black hole candidate MAXI J1535−571 during its reflares

Cúneo

Alabarta

Zhang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Lower limits on the distance can be estimated by measuring either the interstellar extinction (Zdziarski et al 1998(Zdziarski et al , 2004 or the velocities of H absorption (e.g. Chauhan et al 2019) towards the source. X-ray dust scattering halo has also been used to constrain the distance to some the BHXBs (e.g.…”

Section: Introductionmentioning

confidence: 99%

A radio parallax to the black hole X-ray binary MAXI J1820+070

Atri

Miller-Jones

Bahramian

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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156

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Using the Very Long Baseline Array and the European Very Long Baseline Interferometry Network we have made a precise measurement of the radio parallax of the black hole Xray binary MAXI J1820+070, providing a model-independent distance to the source. Our parallax measurement of (0.348 ± 0.033) mas for MAXI J1820+070 translates to a distance of (2.96 ± 0.33) kpc. This distance implies that the source reached (15 ± 3) per cent of the Eddington luminosity at the peak of its outburst. Further, we use this distance to refine previous estimates of the jet inclination angle, jet velocity and the mass of the black hole in MAXI J1820+070 to be (63 ± 3) • , (0.89 ± 0.09) c and (9.2 ± 1.3) M , respectively.

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“…MAXI J1535−571 is a Galactic black hole candidate X-ray binary that was first discovered in 2017 September, in the early phase of its ∼1-year long outburst (Negoro et al 2017;Markwardt et al 2017). This outburst was extensively monitored at radio (Rus-sell et al 2019;Parikh et al 2019;Chauhan et al 2019), sub-mm (Tetarenko et al 2017b, IR and optical (Baglio et al 2018), and Xray (Tao et al 2018;Nakahira et al 2018;Huang et al 2018;Stevens et al 2018;Sreehari et al 2019;Bhargava et al 2019) wavelengths. See Tao et al (2018) and Nakahira et al (2018) for a full discussion on the X-ray states during the outburst.…”

Section: Introductionmentioning

confidence: 99%

“…See Tao et al (2018) and Nakahira et al (2018) for a full discussion on the X-ray states during the outburst. MAXI J1535−571 is located 4.1 +0.6 −0.5 kpc away (determined via an H I absorption study; Chauhan et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Rapid compact jet quenching in the Galactic black hole candidate X-ray binary MAXI J1535-571

Russell,

Lucchini,

Tetarenko

et al. 2020

Preprint

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We present results from six epochs of quasi-simultaneous radio, (sub-)millimetre, infrared, optical, and X-ray observations of the black hole X-ray binary MAXI J1535−571. These observations show that as the source transitioned through the hard-intermediate X-ray state towards the soft intermediate X-ray state, the jet underwent dramatic and rapid changes. We observed the frequency of the jet spectral break, which corresponds to the most compact region in the jet where particle acceleration begins (higher frequencies indicate closer to the black hole), evolve from the IR band into the radio band (decreasing by ≈3 orders of magnitude) in less than a day. During one observational epoch, we found evidence of the jet spectral break evolving in frequency through the radio band. Estimating the magnetic field and size of the particle acceleration region shows that the rapid fading of the high-energy jet emission was not consistent with radiative cooling; instead the particle acceleration region seems to be moving away from the black hole on approximately dynamical timescales. This result suggests that the compact jet quenching is not caused by local changes to the particle acceleration, rather we are observing the acceleration region of the jet travelling away from the black hole with the jet flow. Spectral analysis of the X-ray emission show a gradual softening in the few days before the dramatic jet changes, followed by a more rapid softening ∼1-2 days after the onset of the jet quenching.

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An H i absorption distance to the black hole candidate X-ray binary MAXI J1535–571

Cited by 35 publications

References 32 publications

A NICER look at the state transitions of the black hole candidate MAXI J1535−571 during its reflares

A NICER look at the state transitions of the black hole candidate MAXI J1535−571 during its reflares

A radio parallax to the black hole X-ray binary MAXI J1820+070

Rapid compact jet quenching in the Galactic black hole candidate X-ray binary MAXI J1535-571

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