INTEGRAL observations of the black hole candidate H 1743-322 in outburst

Parmar, A. N.; Kuulkers, E.; Oosterbroek, T.; Barr, P.; Much, R.; Orr, A.; Williams, O. R.; Winkler, Christoph

doi:10.1051/0004-6361:20031140

Cited by 35 publications

(40 citation statements)

References 19 publications

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“…This suggests that the column density we use here (N H = 1.8 × 10 22 cm −2 , Prat et al 2009) seems to be more reliable than higher ones, such as N H = 2.3 × 10 22 cm −2 (Miller et al 2006) or N H = 2.5 × 10 22 cm −2 (Parmar et al 2003).…”

Section: Infrared Jhk S Photometrymentioning

confidence: 63%

“…The OIR observations #1 to #4, reported in Table 1, were carried out after this radio flare, during a phase that several authors identified as a soft, intermediate state (Joinet et al 2005;Homan et al 2005b;Capitanio et al 2005). Nevertheless, a previous work by Parmar et al (2003) reported three observations Table 1) were taken at the end of July 2004 and suggest that the source was then still in the high, soft state, while the optical observation #7 was carried out one day after this last radio detection, with the source transiting to a harder state. INTEGRAL data covered the final part of the outburst and showed that the source, which seemed to harden after the peak of the emission, suddenly fell to a softer state (Capitanio et al 2006).…”

Section: The 2003 Outburst (I)mentioning

confidence: 99%

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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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Section: Infrared Jhk S Photometrymentioning

confidence: 63%

Section: The 2003 Outburst (I)mentioning

confidence: 99%

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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“…H 1743-322 has very frequent outbursts, unlike most of the other black hole transients (BHTs). It showed its brightest outburst in 2003 (∼100 cts/s in RXTE/ASM) that was studied by RXTE and INTEGRAL (Parmar et al 2003;Capitanio et al 2005;Joinet et al 2005;McClintock et al 2009), followed by outbursts in September 2004, September 2005, and January 2008(Kalemci et al 2008. After the Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.…”

Section: Introductionmentioning

confidence: 99%

UsingXMM–Newtonto study the energy-dependent variability of H 1743-322 during its 2014 outburst

Stiele

2016

Mon. Not. R. Astron. Soc.

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Black hole transients during bright outbursts show distinct changes of their spectral and variability properties as they evolve during an outburst, that are interpreted as evidence for changes in the accretion flow and X-ray emitting regions. We obtained an anticipated XMMNewton ToO observation of H 1743-322 during its outburst in September 2014. Based on data of eight outbursts observed in the last 10 years we expected to catch the start of the hardto-soft state transition. The fact that neither the general shape of the observed power density spectrum nor the characteristic frequency show an energy dependence implies that the source still stays in the low-hard state at the time of our observation near outburst peak. The spectral properties agree with the source being in the low-hard state and a Swift/XRT monitoring of the outburst reveals that H 1743-322 stays in the low-hard state during the entire outburst (a. k. a. 'failed outburst'). We derive the averaged QPO waveform and obtain phase-resolved spectra. Comparing the phase-resolved spectra to the phase averaged energy spectrum reveals spectral pivoting. We compare variability on long and short time scales using covariance spectra and find that the covariance ratio does not show an increase towards lower energies as has been found in other black hole X-ray binaries. There are two possible explanations: either the absence of additional disc variability on longer time scales is related to the rather high inclination of H 1743-322 compared to other black hole X-ray binaries or it is the reason why we observe H 1743-322 during a failed outburst. More data on failed outbursts and on high-inclination sources will be needed to investigate these two possibilities further.

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“…One can find After almost two decades, in 2003, the INTEGRAL satellite discovered signatures of renewed activity in hard X-rays (Revnivtsev et al, 2003) and later, RXTE also verified the presence of such an activity (Markwardt & Swank, 2003). During the 2003 outburst, the source was continuously and extensively monitored in X-rays (Parmar et al, 2003;Homan et al, 2005b;McClintock et al, 2009), IR (Steeghs et al, 2003), and in Radio bands (Rupen et al, 2003) to reveal the multi-wavelength properties of the source. The multiwavelength campaign on this source during its 2003 and 2009 outbursts were also carried out by McClintock et al (2009);Miller-Jones et al (2012) respectively.…”

Section: Introductionmentioning

confidence: 99%

Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

Debnath

Chakrabarti

Nandi

2013

Advances in Space Research

111

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The Galactic black hole candidate H 1743-322 exhibited two X-ray outbursts in rapid succession: one in August 2010 and the other in April 2011. We analyze archival data of this object from the PCA instrument on board RXTE (2-25 keV energy band) to study the evolution of its temporal and spectral characteristics during both the outbursts, and hence to understand the behavioral change of the accretion flow dynamics associated with the evolution of the various X-ray features. We study the evolution of QPO frequencies during the rising and the declining phases of both the outbursts. We successfully fit the variation of QPO frequency using the Propagating Oscillatory Shock (POS) model in each of the outbursts and obtain the accretion flow parameters such as the instantaneous shock locations, the shock velocity and the shock strength. Based on the degree of importance of the thermal (disk black body) and the non-thermal (power-law) components of the spectral fit and properties of the QPO (if present), the entire profiles of the 2010 and 2011 outbursts are subdivided into four different spectral states: hard, hard-intermediate, soft-intermediate and soft. We attempt to explain the nature of the outburst profile (i.e., hardness-intensity diagram) with two different types of mass accretion flow.

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INTEGRAL observations of the black hole candidate H 1743-322 in outburst

Cited by 35 publications

References 19 publications

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

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

UsingXMM–Newtonto study the energy-dependent variability of H 1743-322 during its 2014 outburst

Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

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