The complex evolution of the X-ray binary transient MAXI J1807+132 along the decay of its discovery outburst

Jiménez-Ibarra, F.; Muñoz-Darias, T.; Padilla, M. Armas; Russell, D. M.; Casares, J.; Torres, M. A. P.; Sánchez, D. Mata; Jonker, P. G.; Lewis, Fraser

doi:10.1093/mnras/sty3457

Cited by 17 publications

(11 citation statements)

References 85 publications

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“…Although is not the usual behaviour for LMXBs, the nearly periodic occurrence of the reflares of J1535 resemble those observed in dwarf novae. Moreover, the reflaring light curves we obtain for J1535 are similar to the one observed at optical wavelengths in GRO J0422+32 (Kuulkers et al 1996) and MAXI J1807+132 (Jiménez-Ibarra et al 2019). Zhang et al (2019) noticed that the extrapolation of the decaying phase of the main outburst in the light curve coincides with the peaks of the reflares for both dwarf novae and LMXBs, implying the existence of a critical temperature of the disc.…”

Section: Origin Of Reflaressupporting

confidence: 80%

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

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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: Origin Of Reflaressupporting

confidence: 80%

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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“…These features can sometimes show very complex profiles due to e.g. the presence of outflows or changes in the disc opacity (Jiménez-Ibarra et al 2019;Dubus et al 2001). Finally, ejection processes in the form of jets are ubiquitously observed in the low energy part of the spectrum, from radio waves to (at least) the near-infrared (e.g.…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength spectroscopy of the black hole candidate MAXI J1813-095 during its discovery outburst

Padilla

Muñoz-Darias

Sánchez-Sierras

et al. 2019

Monthly Notices of the Royal Astronomical Society

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MAXI J1813-095 is an X-ray transient discovered during an outburst in 2018. We report on X-ray and optical observations obtained during this event, which indicate that the source is a new low-mass X-ray binary. The outburst lasted ∼70 d and peaked at L X (0.5-10keV)∼ 7.6 × 10 36 erg s −1 , assuming a distance of 8 kpc. Swift/XRT follow-up covering the whole activity period shows that the X-ray emission was always dominated by a hard power-law component with a photon index in the range of 1.4-1.7. These values are consistent with MAXI J1813-095 being in the hard state, in agreement with the ∼30 per cent fractional root-mean-square amplitude of the fast variability (0.1-50 Hz) inferred from the only XMM-Newton observation available. The X-ray spectra are well described by a Comptonization emission component plus a soft, thermal component (kT ∼0.2 keV), which barely contributes to the total flux ( 8 per cent). The Comptonization y-parameter (∼1.5), together with the low temperature and small contribution of the soft component supports a black hole accretor. We also performed optical spectroscopy using the VLT and GTC telescopes during outburst and quiescence, respectively. In both cases the spectrum lack emission lines typical of X-ray binaries in outburst. Instead, we detect the Ca ii triplet and Hα in absorption. The absence of velocity shifts between the two epochs, as well as the evolution of the Hα equivalent width, strongly suggest that the optical emission is dominated by an interloper, likely a G-K star. This favours a distance 3 kpc for the X-ray transient.

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“…Bottom panels: 12 June (top) and 16 June (bottom) light curves obtained from red and blue continuum windows in the spectra (orange and purple points, respectively), normalised to the non-dip level. The regions defining these two spectral windows are indicated as shaded areas in the top panel, following the same colour code as above.XTE J1118+480, and recently MAXI J1807+132(Casares et al 1995;Dubus et al 2001; Jiménez-Ibarra et al 2019, respectively) but evolving at longer time scales (e.g Jiménez- Ibarra et al 2019,. detected them in a 3600 s exposure spectrum).…”

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confidence: 98%

An equatorial outflow in the black hole optical dipper Swift J1357.2−0933

Jiménez-Ibarra

Muñoz-Darias

Casares

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present high-time resolution optical spectroscopy and imaging of the black hole transient Swift J1357.2-0933 during its 2017 outburst. The light curves show recurrent dips resembling those discovered during the 2011 outburst. The dip properties (e.g duration and depth) as well as the evolution of their recurrence time are similar to those seen in 2011. Spectra obtained during the dips are characterised by broad and blue-shifted absorptions in Balmer and He ii. The absorptions show core velocities of ∼ −800 km s −1 and terminal velocities approaching ∼3000 km s −1 i.e. in the upper-end of wind velocities measured in other black hole transients (both at optical and X-ray wavelengths). Our observations suggest that the dips are formed in a dense and clumpy outflow, produced near the disc equatorial plane and seen at high inclination. We also study the colour evolution and observe that, as it has been previously reported, the source turns bluer during dips. We show that this is due to a gradual change in the slope of the optical continuum and discuss possible implications of this behaviour.

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The complex evolution of the X-ray binary transient MAXI J1807+132 along the decay of its discovery outburst

Cited by 17 publications

References 85 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

Multiwavelength spectroscopy of the black hole candidate MAXI J1813-095 during its discovery outburst

An equatorial outflow in the black hole optical dipper Swift J1357.2−0933

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