The 2005 Outburst of the Halo Black Hole X‐Ray Transient XTE J1118+480

Zurita, C.; Torres, M. A. P.; Steeghs, D.; Rodríguez‐Gil, P.; Muñoz-Darias, T.; Casares, J.; Shahbaz, T.; Martínez‐País, I. G.; Zhao, Ping; Garcia, M. R.; Piccioni, A.; Bartolini, C.; Гуарниери, А.; Bloom, J.; Blake, Cullen H.; Falco, E.; Szentgyorgyi, Andrew; Skrutskie, M. F.

doi:10.1086/503286

Cited by 40 publications

(65 citation statements)

References 46 publications

(59 reference statements)

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“…The shape of the SED is similar to the one of the transient LMXB XTE J1118+480 (Chaty et al 2003;Zurita et al 2006): although in the LHS during its 2005 outburst, the latter work gave IR and optical slopes with different α values, softening from 0.49 at the peak, not far from our value but distinct, as XTE J1818−245 was in another spectral state, to 0.25 (decay). In the case of the 2000 outburst, the SED of XTE J1118+480 from radio to X-rays has been explained as a combination of synchrotron radiation from a jet and a truncated optically thick disc, whereas models assuming advection dominated accretion flows alone underestimated the optical and IR fluxes (Zurita et al 2006 and references therein).…”

Section: Spectral Energy Distribution (Sed)supporting

confidence: 72%

“…In the case of the 2000 outburst, the SED of XTE J1118+480 from radio to X-rays has been explained as a combination of synchrotron radiation from a jet and a truncated optically thick disc, whereas models assuming advection dominated accretion flows alone underestimated the optical and IR fluxes (Zurita et al 2006 and references therein). In 2005, discrepancies observed between the optical and IR SEDs suggested that the IR was dominated by a different component (a jet?)…”

Section: Spectral Energy Distribution (Sed)mentioning

confidence: 99%

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Detailed radio to softγ-ray studies of the 2005 outburst of the new X-ray transient XTE J1818-245

Bel¹,

Prat

Rodríguez

et al. 2009

A&A

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Context. XTE J1818−245 is an X-ray nova that experienced an outburst in 2005, as first seen by the RXTE satellite. The source was observed simultaneously at various wavelengths up to soft γ-rays with the INTEGRAL satellite, from 2005 February to September, during our INTEGRAL Target of Opportunity program dedicated to new X-ray novae and during Galactic Bulge observations. Aims. X-ray novae are extreme systems that often harbor a black hole, and are known to emit throughout the electromagnetic spectrum when in outburst. The goals of our programme are to understand the physical processes close to the black hole and to study the possible connection with the jets that are observed in the radio. Methods. We analysed radio, (N)IR, optical, X-ray and soft γ-ray observations. We constructed simultaneous broad-band X-ray spectra covering a major part of the outburst, which we fitted with physical models. Analyzing both the light curves in various energy ranges and the hardness-intensity diagram enabled us to study the long-term behaviour of the source. Results. Spectral parameters were typical of the Soft Intermediate States and the High Soft States of a black hole candidate. The source showed relatively small spectral variations in X-rays with considerable flux variation in radio. Spectral studies showed that the accretion disc cooled down from 0.64 to 0.27 keV in ∼100 days and that the total flux decreased while the relative flux of the hot medium increased. Radio emission was detected several times, and, interestingly, five days after entering the HSS. Modeling the spectral energy distribution from the radio to the soft γ-rays reveals that the radio flares arise from several ejection events. Conclusions. XTE J1818−245 probably belongs to the class of low-mass X-ray binaries and is likely a black hole candidate transient source that might be closer than the Galactic Bulge. The results from the data analysis trace the physical changes that took place in the system (disc, jet/corona) at a maximum bolometric luminosity of 0.4-0.9 ×10 38 erg s −1 (assuming a distance between 2.8-4.3 kpc) and they are discussed within the context of disc and jet models.

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Section: Spectral Energy Distribution (Sed)supporting

confidence: 72%

Section: Spectral Energy Distribution (Sed)mentioning

confidence: 99%

Detailed radio to softγ-ray studies of the 2005 outburst of the new X-ray transient XTE J1818-245

Bel¹,

Prat

Rodríguez

et al. 2009

A&A

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“…This could potentially result in re-acceleration of particles up to very high energies. In general, the shape of our SEDs during the LHS are similar to the ones of the transient LMXB XTE J1118+480 (Chaty et al 2003;Zurita et al 2006): in its 2000 outburst, the SED from radio to X-rays has been explained as a combination of synchrotron radiation from a jet and a truncated optically thick disc, whereas models assuming advection dominated accretion flows alone underestimated the optical and IR fluxes (Zurita et al 2006, and references therein). Discrepancies observed between the optical and IR SEDs of XTE J1118+480 in 2005 suggested that the IR was dominated possibly by a jet, whereas the optical was dominated by disc emission.…”

Section: Spectral Energy Distributionssupporting

confidence: 59%

Overview of an extensive multi-wavelength study of GX 339−4 during the 2010 outburst

Bel

Rodríguez

D’Avanzo

et al. 2011

A&A

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Context. The microquasar GX 339−4 experienced a new outburst in 2010: it was observed simultaneously at various wavelengths from radio up to soft γ-rays. We focus on observations that are quasi-simultaneous with those made with the INTEGRAL and RXTE satellites: these were collected in 2010 March-April during our INTEGRAL target of opportunity programme, and during some of the other INTEGRAL observing programmes with GX 339−4 in the field-of-view. Aims. X-ray transients are extreme systems that often harbour a black hole, and are known to emit throughout the whole electromagnetic spectrum when in outburst. The goals of our programme are to understand the evolution of the physical processes close to the black hole and to study the connections between the accretion and ejection. Methods. We analysed radio, NIR, optical, UV, X-ray and soft γ-ray observations. We studied the source evolution in detail by producing light curves, hardness-intensity diagrams and spectra. We fitted the broadband data with phenomenological, then physical, models to study the emission coming from the distinct components. Results. Based on the energy spectra, the source evolved from the canonical hard state to the canonical soft state. The source showed X-ray spectral variations that were correlated with changes in radio, NIR and optical emission. The bolometric flux increased from 0.8 to 2.9 × 10 −8 erg cm −2 s −1 while the relative flux and contribution of the hot medium decreased on the average. Reprocessing in the disc was likely to be strong at the end of our observations. Conclusions. The source showed a behaviour similar to that of previous outbursts, with some small deviations in the hard X-ray parameter evolution. The radio, NIR and optical emission from jets was detected and observed to fade as the source softened. The results are discussed within the context of disc and jet models.

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“…With an Eddington ratio of LX /L Edd ∼ 10 −8.5 , J1118 is one of our best probes of black hole accretion flows at the lowest detectable luminosities. A special aspect of J1118 is that it has also been well-studied at higher luminosities during previous outbursts (e.g., Esin et al 2001;Markoff, Falcke & Fender 2001;McClintock et al 2001;Hynes et al 2000Hynes et al , 2003Chaty et al 2003;Malzac, Merloni & Fabian 2004;Zurita et al 2006;Maitra et al 2009;Brocksopp et al 2010;Vila et al 2012;Zhang & Xie 2013).…”

Section: Introductionmentioning

confidence: 99%

Constraints on relativistic jets in quiescent black hole X-ray binaries from broad-band spectral modelling

Plotkin

Gallo

Markoff

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The nature of black hole jets at the lowest detectable luminosities remains an open question, largely due to a dearth of observational constraints. Here, we present a new, nearly-simultaneous broadband spectrum of the black hole X-ray binary (BHXB) XTE J1118+480 at an extremely low Eddington ratio (L X ∼ 10 −8.5 L Edd ). Our new spectral energy distribution (SED) includes the radio, near-infrared, optical, ultraviolet, and X-ray wavebands. XTE J1118+480 is now the second BHXB at such a low Eddington ratio with a well-sampled SED, thereby providing new constraints on highly sub-Eddington accretion flows and jets, and opening the door to begin comparison studies between systems. We apply a multi-zone jet model to the new broadband SED, and we compare our results to previous fits to the same source using the same model at 4-5 decades higher luminosity. We find that after a BHXB transitions to the so-called quiescent spectral state, the jet base becomes more compact (by up to an order of magnitude) and slightly cooler (by at least a factor of two). Our preferred model fit indicates that jet particle acceleration is much weaker after the transition into quiescence. That is, accelerated non-thermal particles no longer reach high enough Lorentz factors to contribute significant amounts of synchrotron X-ray emission. Instead, the X-ray waveband is dominated by synchrotron self-Compton emission from a population of mildly relativistic electrons with a quasi-thermal velocity distribution that are associated with the jet base. The corresponding (thermal) synchrotron component from the jet base emits primarily in the infrared through ultraviolet wavebands. Our results on XTE J1118+480 are consistent with broadband modeling for A0620-00 (the only other comparably low Eddington ratio BHXB with a well-sampled SED) and for Sgr A* (the quiescent supermassive black hole at the Galactic center). The above could therefore represent a canonical baseline geometry for accreting black holes in quiescence. We conclude with suggestions for future studies to further investigate the above scenario.

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The 2005 Outburst of the Halo Black Hole X‐Ray Transient XTE J1118+480

Cited by 40 publications

References 46 publications

Detailed radio to softγ-ray studies of the 2005 outburst of the new X-ray transient XTE J1818-245

Detailed radio to softγ-ray studies of the 2005 outburst of the new X-ray transient XTE J1818-245

Overview of an extensive multi-wavelength study of GX 339−4 during the 2010 outburst

Constraints on relativistic jets in quiescent black hole X-ray binaries from broad-band spectral modelling

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