Disentangling the NIR/optical emission of the black hole XTE J1650−500 during outburst

Curran, P. A.; Chaty, S.; Heras, J. A. Zurita

doi:10.1051/0004-6361/201219228

Cited by 12 publications

(14 citation statements)

References 51 publications

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“…It has been shown (Curran et al 2012) that sources deviate from this correlation early in the intermediate state so this agreement adds further weight to the suggestion that the system was in the hard state at the time of the optical observations. During the 2001 outburst, our observations span most of the X-ray activity (see Fig.…”

Section: Discussionsupporting

confidence: 53%

Near-infrared and optical observations of the failed outbursts of black hole binary XTE J1550−564

Curran

Chaty

2013

A&A

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Context. A number of low mass X-ray binaries (LMXBs) undergo "failed outbursts" in which, instead of evolving through the canonical states, they remain in a hard state throughout the outburst. While the sources of X-ray and radio emission in the hard state are relatively well understood, the origin of the near-infrared (NIR) and optical emission is more complex though it likely stems from an amalgam of different emission processes, occurring as it does, at the intersecting wavelengths of those processes. Aims. We aim to identify the NIR/optical emission region(s) during a number of failed outbursts of one such LMXB and black hole candidate, XTE J1550−564, in order to confirm or refute their classification as hard-state, failed outbursts. Methods. We present unique NIR/optical images and spectra, obtained with the ESO-New Technology Telescope, during the failed outbursts of 2001 and 2000. We compare the NIR/optical photometric, timing, and spectral properties with those expected for the different emission mechanisms in the various LMXB states. Results. The NIR/optical data are consistent with having come from reprocessing of X-rays in the accretion disk, with no evidence of direct thermal emission from the disk itself. However, the observed variability in high-cadence NIR light curves suggest that the radio jet extends and contributes to the NIR wavelengths. Conclusions. We find that these failed outbursts did not transition to an intermediate state but remained in a true, hard state where there was no sign of jet quenching or deviation from the observed hard state correlations.

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Section: Discussionsupporting

confidence: 53%

Near-infrared and optical observations of the failed outbursts of black hole binary XTE J1550−564

Curran

Chaty

2013

A&A

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“…4 lower panel), the radio-faint black hole X-ray binaries exhibit lower jet luminosity at the break frequency, compared to radio-loud ones. In other terms, our IR observations show that H 1743-322, instead of being X-ray loud, would rather be a radio-quiet and NIR-dim black hole in the LHS, and this would constitute, after the microquasar XTE J1650-500 (Curran et al 2012), the second clear example of an outlier in the NIR vs. X-ray correlation.…”

Section: Oir Vs X-ray Correlationmentioning

confidence: 77%

Infrared study of H 1743-322 in outburst: a radio-quiet and NIR-dim microquasar

Chaty

Arjonilla

Dubus

2015

A&A

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Context. Microquasars are accreting Galactic sources that are commonly observed to launch relativistic jets. One of the most important issues regarding these sources is the energy budget of ejections relative to the accretion of matter. Aims. The X-ray binary, black hole candidate, and microquasar H 1743-322 exhibited a series of X-ray outbursts between 2003 and 2008. We took optical and near-infrared (OIR) observations with the ESO/NTT telescope during three of these outbursts (2003, 2004, and 2008). The goals of these observations were to investigate the presence of a jet, and to disentangle the various contributions constituting the spectral energy distribution (SED): accretion, ejection, and stellar emission. Methods. Photometric and spectroscopic OIR observations allowed us to produce a high time-resolution lightcurve in K s -band, to analyze emission lines present in the IR spectra, to construct a multiwavelength SED including radio, IR, and X-ray data, and to complete the OIR vs. X-ray correlation of black hole binaries with H 1743-322 data points. Results. We detect rapid flares of duration ∼5 min in the high time-resolution IR lightcurve. We identify hydrogen and helium emission lines in the IR spectra, coming from the accretion disk. The IR SED exhibits the spectral index typically associated with the X-ray high, soft state in our observations taken during the 2003 and 2004 outbursts, while the index changes to one that is typical of the X-ray low, hard state during the 2008 outburst. During this last outburst, we detected a change of slope in the NIR spectrum between the J and K s bands, where the JH part is characteristic of an optically thick disk emission, while the HK s part is typical of optically thin synchrotron emission. Furthermore, the comparison of our IR data with radio and X-ray data shows that H 1743-322 exhibits a faint jet both in radio and NIR domains. Finally, we suggest that the companion star is a late-type main sequence star located in the Galactic bulge. Conclusions. These OIR photometric and spectroscopic observations of the microquasar H 1743-322, which are the first of this source to be published in a broad multiwavelength context, allow us to unambiguously identify two spectra of different origins in the OIR domain, evolving from optically thick thermal emission to optically thin synchrotron emission toward longer wavelengths. Comparing these OIR observations with other black hole candidates suggests that H 1743-322 behaves like a radio-quiet and NIR-dim black hole in the low, hard state. This study will be useful when quantitatively comparing the overall contribution of the compact jet and accretion flow in the energy budget of microquasars.

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“…Radio, IR, and other optical/UV data in this work are taken from the literature on each source [for XTE J1650-500: Corbel et al (2004), Curran, Chaty & Heras (2012); XTE J1752-223: Brocksopp et al (2013); MAXI J1659-152: van der Horst et al (2013)]. We perform the de-reddening of IR/optical/UV data ourselves to make sure the The thermal photons from the accretion disc are IC up-scattered by the synchrotronproducing electrons inside the jet; the jet cyclo-synchrotron emission is also subject to self-Comptonization (SSC).…”

Section: Data Reduction and Collectionmentioning

confidence: 99%

“…The radio data were published and tabulated in Corbel et al (2004), Brocksopp et al (2013), van der Horst et al (2013). The infrared, optical, and UV data were published in Curran et al (2012), van der Horst et al (2013). The X-ray data are publicly available from HEASARC (ht tps://heasarc.gsfc.nasa.gov/).…”

Section: Ac K N Ow L E D G E M E N T Smentioning

confidence: 99%

Evidence for an expanding corona based on spectral-timing modelling of multiple black hole X-ray binaries

Cao

Lucchini

Markoff

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Galactic black hole X-ray binaries (BHXBs) provide excellent laboratories to study accretion, as their relatively quick evolution allows us to monitor large changes in the in-flowing and/or out-flowing material over human timescales. However, the details of how the inflow-outflow coupling evolves during a BHXB outburst remain an area of active debate. In this work we attempt to probe the physical changes underlying the system evolution, by performing a systematic analysis of the multi-wavelength data of three BHXB sources: XTE J1752-223, MAXI J1659-152, and XTE J1650-500, during hard and hard-intermediate states. Using the power spectral hue which characterises the X-ray variability properties, we identify several clusters of BHXB epochs and perform the joint multi-wavelength spectral modelling to test their commonality with a physical jet model. Under the assumption that the corona is related to the base of the jet, we find that the power spectral hue traces the variation of the coronal radius (from ∼10Rg − ∼ 40Rg) in multiple BHXBs at hard and hard-intermediate states, and that the data are consistent with moderately truncated accretion discs (<25Rg) during hard-intermediate states. We also find that all epochs of low disc reflection have high hue located near the hard-intermediate to soft-intermediate state transition, indicating that in these states the vertical extent of the corona and/or its bulk speed are increasing. Our results link the geometrical similarity in the corona among multiple BHXB sources to their timing characteristics, and probe the corona responding to the disc-jet interactions at hard and intermediate states during outbursts.

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Disentangling the NIR/optical emission of the black hole XTE J1650−500 during outburst

Cited by 12 publications

References 51 publications

Near-infrared and optical observations of the failed outbursts of black hole binary XTE J1550−564

Near-infrared and optical observations of the failed outbursts of black hole binary XTE J1550−564

Infrared study of H 1743-322 in outburst: a radio-quiet and NIR-dim microquasar

Evidence for an expanding corona based on spectral-timing modelling of multiple black hole X-ray binaries

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