The X-Ray Transient XTE J1118+480: Multiwavelength Observations of a Low-State Minioutburst

Hynes, R. I.; Mauche, Christopher W.; Haswell, C. A.; Shrader, C. R.; Cui, Wei; Chaty, S.

doi:10.1086/312836

Cited by 133 publications

(179 citation statements)

References 22 publications

(18 reference statements)

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“…These light curves have comparable length and brightness, and the X-ray-to-optical ratio measured in J1118 is also similar to what has been seen in minioutbursts, i.e., it is much lower than in normal outbursts (e.g., Zurita et al 2002b). These facts support the suggestion of Hynes et al (2000) that the outbursts in J1118 are indeed minioutbursts rather than full XRT events.…”

Section: Long-term Light Curvesupporting

confidence: 87%

“…The low interstellar absorption toward XTE J1118+480 allowed a detailed multiwavelength study during the 2000 outburst and quiescence, being the only XRT for which extreme ultraviolet observations could be achieved ( Hynes et al 2000;Chaty et al 2003;McClintock et al 2003). In fact, the best observations of an XRT in the LH state have been made for this system (together with GX 339À4).…”

Section: Introductionmentioning

confidence: 98%

“…In addition, the ratio L X /L opt ' 5 was extremely low, so it has been suggested that XTE J1118+480 may be an accretion disk corona source seen at high inclination (Garcia et al 2000). However, no eclipse has ever been recorded, and consequently, the source should have been intrinsically faint in X-rays ( Hynes et al 2000) during the outburst. Finally, associated radio emission from this source has been reported ( Pooley & Waldram 2000) with jet interpretation .…”

Section: Introductionmentioning

confidence: 99%

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

Zurita

Torres

Steeghs

et al. 2006

ApJ

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We present optical and infrared monitoring of the 2005 outburst of the halo black hole X-ray transient XTE J1118+480. We measured a total outburst amplitude of $5:7 AE 0:1 mag in the R band and $5 mag in the infrared J, H, and K s bands. The hardness ratio HR2 (5 12 keV : 3 5 keV ) from the RXTE ASM data is 1:53 AE 0:02 at the peak of the outburst, indicating a hard spectrum. Both the shape of the light curve and the ratio L X (1 10 keV)/L opt resemble the minioutbursts observed in GRO J0422+32 and XTE J1859+226. During early decline, we find a 0.02 mag amplitude variation consistent with a superhump modulation, like the one observed during the 2000 outburst. Similarly, XTE J1118+480 displayed a double-humped ellipsoidal modulation distorted by a superhump wave when settled into a near-quiescence level, suggesting that the disk expanded to the 3:1 resonance radius after outburst, where it remained until early quiescence. The system reached quiescence at R ¼ 19:02 AE 0:03, about 3 months after the onset of the outburst. The optical rise preceded the X-ray rise by at most 4 days. The spectral energy distributions (SEDs) at the different epochs during outburst are all quasi-power laws with F / increasing toward the blue. At the peak of the outburst, we derived ¼ 0:49 AE 0:04 for the optical data alone and ¼ 0:1 AE 0:1 when fitting solely the infrared. This difference between the optical and the infrared SEDs suggests that the infrared is dominated by a different component (a jet?), whereas the optical is presumably showing the disk evolution.

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Section: Long-term Light Curvesupporting

confidence: 87%

Section: Introductionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

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

Zurita

Torres

Steeghs

et al. 2006

ApJ

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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 optical/infrared (OIR) spectra of black hole (BH) low-mass X-ray binaries often show an excess above the standard (Shakura & Sunyaev 1973) accretion disc emission (e.g., Hynes et al 2000Hynes et al , 2002Gelino, Gelino, & Harrison 2010). In some cases, the spectrum can be described by a power law of index close to zero (i.e.…”

Section: Introductionmentioning

confidence: 99%

Colours of black holes: infrared flares from the hot accretion disc in XTE J1550–564

Poutanen

Veledina

Revnivtsev

2014

Monthly Notices of the Royal Astronomical Society

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Outbursts of the black hole (BH) X-ray binaries are dramatic events occurring in our Galaxy approximately once a year. They are detected by the X-ray telescopes and often monitored at longer wavelengths. We analyse the X-ray and optical/infrared (OIR) light-curves of the BH binary XTE J1550-564 during the 2000 outburst. By using the observed extreme colours as well as the characteristic decay time-scales of the OIR and X-ray light curves, we put strong constraints on the extinction towards the source. We accurately separate the contributions to the OIR flux of the irradiated accretion disc and a non-thermal component. We show that the OIR non-thermal component appears during the X-ray state transitions both during the rising and the decaying part of the outburst at nearly the same X-ray hardness but at luminosities differing by a factor of 3. The line marking the quenching/recovery of the non-thermal component at the X-ray hardness-flux diagram seems to coincide with the 'jet line' that marks the presence of the compact radio jet. The inferred spectral shape and the evolution of the non-thermal component during the outburst, however, are not consistent with the jet origin, but are naturally explained in terms of the hybrid hot flow scenario, where non-thermal electrons emit synchrotron radiation in the OIR band. This implies a close, possibly causal connection between the presence of the hot flow and the compact jet. We find that the non-thermal component is hardening during the hard state at the decaying stage of the outburst, which indicates that the acceleration efficiency is a steep function of radius at low accretion rate.

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The X-Ray Transient XTE J1118+480: Multiwavelength Observations of a Low-State Minioutburst

Cited by 133 publications

References 22 publications

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

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

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

Colours of black holes: infrared flares from the hot accretion disc in XTE J1550–564

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