Spectral States of the X‐Ray Binary IGR J17091−3624 Observed by<i>INTEGRAL</i>and<i>RXTE</i>

Capitanio, Fiamma; Bazzano, A.; Ubertini, P.; Zdziarski, A. A.; Bird, A. J.; Cesare, G. De; Dean, A. J.; Stephen, J. B.; Tarana, A.

doi:10.1086/502641

Cited by 26 publications

(36 citation statements)

References 22 publications

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“…It exhibits a large variability in X-rays, and it is uncertain if this source is a Be/X-ray binary or an LMXB. Capitanio et al (2006) confirm the low absorption (N H ≤ 1 × 10 22 cm −2 ) and Comptonised spectrum of this source. Negueruela & Schurch (2007) proposed the 2MASS J17090199-3623260 source as a candidate counterpart, based on photometric catalogues.…”

Section: Igr J17091-3624supporting

confidence: 80%

Multi-wavelength observations of Galactic hard X-ray sources discovered byINTEGRAL

Chaty¹,

Rahoui²,

Foellmi

et al. 2008

A&A

145

198

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Context. The INTEGRAL hard X-ray observatory has revealed an emerging population of highly obscured X-ray binary systems through multi-wavelength observations. Previous studies have shown that many of these sources are high-mass X-ray binaries hosting neutron stars orbiting around luminous and evolved companion stars. Aims. To better understand this newly-discovered population, we have selected a sample of sources for which an accurate localisation is available to identify the stellar counterpart and reveal the nature of the companion star and of the binary system. Methods. We performed an intensive study of a sample of thirteen INTEGRAL sources, through multi-wavelength optical to NIR photometric and spectroscopic observations, using EMMI and SofI instruments at the ESO NTT telescope. We performed accurate astrometry and identified candidate counterparts for which we give the optical and NIR magnitudes. We detected many spectral lines allowing us to determine the spectral type of the companion star. We fitted with stellar black bodies the mid-infrared to optical spectral energy distributions of these sources. From the spectral analysis and SED fitting we identified the nature of the companion stars and of the binary systems.Results. Through spectroscopic analysis of the most likely candidates we found the spectral types of IGR J16320-4751, IGR J16358-4726, IGR J16479-4514, IGR J17252-3616, IGR J18027-2016: They all host OB type supergiant companion stars, with IGR J16358-4726 likely hosting an sgB[e]. Our spectra also confirm the supergiant O and B nature of IGR J17391-3021 and IGR J19140+0951. From SED fitting we found that IGR J16418-4532 is a (likely OB supergiant) HMXB, IGR J16393-4643 a (likely BIV-V star) HMXB, and IGR J18483-0311 a likely HMXB system. Through accurate astrometry, we rejected the proposed counterparts of IGR J17091-3624 and IGR J17597-2201, and we discovered two new candidate counterparts for each source, both suggesting an LMXB from SED fitting. We confirm the AGN nature of IGR J16558-5203. Finally, we report that NIR fields of four sources of our sample exhibit large-scale regions of absorption. Conclusions. The majority of these systems are high-mass X-ray binaries hosting supergiant companion stars. We therefore confirm that INTEGRAL reveals a dominant class of obscured and short-lived high-energy binary systems, and we suggest an association of these systems with regions of the Galaxy exhibiting large-scale absorption. Stellar population models should take these systems into account for realistic estimates of high-energy binary systems in our Galaxy.

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Section: Igr J17091-3624supporting

confidence: 80%

Multi-wavelength observations of Galactic hard X-ray sources discovered byINTEGRAL

Chaty¹,

Rahoui²,

Foellmi

et al. 2008

A&A

145

198

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“…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). Our observations #8 and #9 correspond to this high, soft state.…”

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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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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“…According to Capitanio et al (2006), the source has not been active since 2004. Perhaps the JHK observations were made at a time when the source was active and the colours dominated by an accretion disk, mimicking the flat IR spectrum of an early type star.…”

Section: Igr J17091-3624mentioning

confidence: 99%

A search for counterparts to massive X-ray binaries using photometric catalogues

Negueruela

Schurch

2006

A&A

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Context. The X-ray and γ-ray observatory INTEGRAL has discovered large numbers of new hard X-ray sources, many of which are believed to be high mass X-ray binaries. However, for a significant fraction, their counterparts remain unidentified. Aims. We explore the use of photometric catalogues to find optical counterparts to high mass X-ray binaries and search for objects likely to be early-type stars within the error circles of several INTEGRAL sources. Methods. Candidates were selected from 2MASS photometry by means of a reddening free Q parameter. Sufficiently bright candidates were spectroscopically observed. Results. Many of the candidates selected turned out to be moderately reddened late A or early F stars. Optically visible OB stars are very scarce even in these Galactic Plane fields. Our method is able to identify the counterpart to IGR J16207−5129, confirmed by a Chandra localisation. We classify this object as a B0 supergiant. In the field of AX J1820.5−1434, we find a mid or early B-type star, but we cannot confirm it as the counterpart. For IGR J16320−4751 we rule out the optically visible candidate as a possible counterpart. For AX J1700.2−4220, we do not find any suitable candidate within the ASCA error circle. We classify HD 153295, a marginal candidate to be the counterpart, as B0.5 IVe, and find a distance compatible with membership in Sco OB1. In the case of IGR J17091−3624, the object associated with a variable radio source in the field is a late F star. We derive a spectral type B0 IIIe for HD 100199, previously identified as the counterpart to IGR J11305−6256. Conclusions. The procedure used is able to correctly identify OB stars and, in about one third of the cases, may lead to the localisation of the correct counterpart. However, the majority of INTEGRAL error circles do not contain any suitable optically visible counterpart. Deep infrared searches are going to be necessary in order to locate the counterparts to these sources.

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Spectral States of the X‐Ray Binary IGR J17091−3624 Observed byINTEGRALandRXTE

Cited by 26 publications

References 22 publications

Multi-wavelength observations of Galactic hard X-ray sources discovered byINTEGRAL

Multi-wavelength observations of Galactic hard X-ray sources discovered byINTEGRAL

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

A search for counterparts to massive X-ray binaries using photometric catalogues

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