Complete and Simultaneous Spectral Observations of the Black Hole X‐Ray Nova XTE J1118+480

McClintock, Jeffrey E.; Haswell, C. A.; Garcia, M. R.; Drake, J. J.; Hynes, R. I.; Marshall, H. L.; Muno, M. P.; Chaty, S.; Garnavich, P.; Groot, P.; Lewin, W. H. G.; Mauche, Christopher W.; Miller, J. M.; Pooley, G. G.; Shrader, C. R.; Vrtilek, S. D.

doi:10.1086/321449

Cited by 152 publications

(181 citation statements)

References 24 publications

Supporting

Mentioning

169

Contrasting

Order By: Relevance

“…The synchrotron spectrum, which is thought to be the jet signature, is frequently seen at radio but also up to higher frequencies in the infrared and possibly in the optical. In the case of J1118, the SED from radio to X-rays during the 2000 outburst has been explained as a combination of synchrotron radiation from a jet and a truncated optically thick disk (Hynes et al 2000;Markoff et al 2001;Yuan et al 2005), whereas models assuming ADAF alone ( McClintock et al 2001b;Esin et al 2001) underestimated the optical and the infrared fluxes. The spectrum from infrared to UV is flat (F $ const; Hynes et al 2000), although the optical spectrum alone has blue continuum slopes of ¼ 1/3, as expected for an optically thick accretion disk ( Dubus et al 2001;Torres et al 2002).…”

Section: Summary and Discussionmentioning

confidence: 99%

See 1 more Smart Citation

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

Zurita

Torres

Steeghs

et al. 2006

ApJ

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Section: Summary and Discussionmentioning

confidence: 99%

“…These observations have been of great significance in the effort to build a physical model of the accretion flow. XTE J1118+480 has been described in terms of an ADAF ( McClintock et al 2001b;Esin et al 2001), an accretion disk corona model , and a jet model ( Markoff et al 2001;Malzac et al 2004;Yuan et al 2005).…”

Section: Introductionmentioning

confidence: 99%

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

Zurita

Torres

Steeghs

et al. 2006

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Our analysis of the historical optical plates reveals that in the years 1995 and 1996 it had optical outbursts of ∼2 mag that passed without notice, although could have been easily measured. We point out that XTE J1118+480 was a black hole nova with a remarkably large optical-to-X-ray flux ratio 10 that reached a peak luminosity of about 10 36 erg s −1 in the 1-160 keV band 6 . Presently it is close to the Sun, but at the distance of the Galactic centre it would have not been detected in most surveys with X-ray instruments of large field of view.…”

mentioning

confidence: 81%

A high-velocity black hole on a Galactic-halo orbit in the solar neighbourhood

Mirabel

Dhawan

Mignani

et al. 2001

Nature

152

161

View full text Add to dashboard Cite

Only a few of the dozen or so stellar-mass black holes have been observed away from the plane of the Galaxy 1 . Those few could have been ejected from the plane as a result of a "kick" received during a supernova explosion, or they could be remnants of the population of massive stars formed in the early stages of evolution of the Galaxy. Determining their orbital motion should help to distinguish between these options. Here we report the transverse motion (in the plane of the sky) for the black hole Xray nova XTE J1118+480 (refs 2-5), from which we derive a large space velocity. This X-ray binary has an eccentric orbit around the Galactic Centre, like most objects in the halo of the Galaxy, such as ancient stars and globular clusters. The properties of the system suggest that its age is comparable to or greater than the age of the Galactic disk. Only an extraordinary "kick" from a supernova could have launched the black hole into an orbit like this from a birth place in the disk of the Galaxy.The high galactic latitude (l = 157.7 • , b = +62.3 • ) X-ray nova XTE J1118+480 was discovered 2 with the RXTE All-Sky Monitor on 2000 March 29. It exhibited slow outbursts that lasted ∼7 months with a peak X-ray luminosity of 4 x 10 35 (D/kpc) 2 erg s −1 and energy spectra typical of black hole binaries in low/hard state 6 . From observations of the ∼19 mag optical counterpart 3 in quiescence a mass function for the compact object f(M) ∼ 6.0±0.4 M ⊙ and an average distance of ∼ 1.85±0.36 kpc were determined 4,5 . For ∼100 days the source exhibited a steady and slowly variable unresolved radio counterpart 7,8 with persistent inverted radio spectrum, which is interpreted as optically thick emission from a compact, powerful synchrotron jet 8,9 , that could have a size ≤0.03 AU 9 . 1To measure the transverse motion on the plane of the sky of XTE J1118+480 we carried out observations of the radio counterpart with the Very Long Baseline Array (VLBA) at 15.4 GHz (λ2 cm) and 8.4 GHz (λ3.6 cm) on 2000 May 4 and July 24; afterwards it faded below detection. In both epochs the source was unresolved by the synthesized beams of 1×0.6 milli arc sec (mas) and 2×1 mas respectively, which correspond to physical dimensions smaller than ∼0.7 D/kpc AU, and a brightness temperature ≥10 9 K. Because of the high galactic latitude and low column of interstellar gas along the line of sight (N H ∼ 10 20 cm −2 ) 10 , the VLBA images are relatively unaffected by Galactic electron scattering, allowing us to determine in each epoch the position of the compact, unresolved radio source with relative errors ≤0.35 mas.The observations were done in cycles that included the target, the strong calibrator 3C273, a primary calibrator (Cal. 1) used as phase-reference source, and a second extragalactic calibrator (Cal.2). Their high elevation and good weather ensured that the phase connection was successful. The epoch, source, frequency, bandwidth, position, and flux for the VLBA observations of XTE J1118+480 and the two extragalactic sources used as references ...

show abstract

“…The star in XTE J1118+480, which is of spectral type between K5V and K8 (McClintock et al 2001b;Wagner et al 2001;Torres et al 2004), is rotating on the orbital period of 4.08 hr since the orbit is tidally locked. In the catalog of coronally active RS CVn stars of Drake, Simon & Linsky (1989), the most luminous system with a rotation period of < ∼ 10 days, and containing a K5-8 star, would be 1.04±0.06 µJy (at 5 GHz) at a distance of 1.7 kpc.…”

Section: Xte J1118+480 In the Radio/x-ray Domainmentioning

confidence: 99%

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

Gallo¹,

Miller-Jones²,

Russell³

et al. 2014

Monthly Notices of the Royal Astronomical Society

155

200

View full text Add to dashboard Cite

We report on deep, coordinated radio and X-ray observations of the black hole X-ray binary XTE J1118+480 in quiescence. The source was observed with the Karl G. Jansky Very Large Array for a total of 17.5 hrs at 5.3 GHz, yielding a 4.8±1.4 µJy radio source at a position consistent with the binary system. At a distance of 1.7 kpc, this corresponds to an integrated radio luminosity between 4-8 ×10 25 erg s −1 , depending on the spectral index. This is the lowest radio luminosity measured for any accreting black hole to date. Simultaneous observations with the Chandra X-ray Telescope detected XTE J1118+480 at 1.2 × 10 −14 erg s −1 cm −2 (1-10 keV), corresponding to an Eddington ratio of ∼4 × 10 −9 for a 7.5 M black hole. Combining these new measurements with data from the 2005 and 2000 outbursts available in the literature, we find evidence for a relationship of the form r =α+β X (where denotes logarithmic luminosities), with β = 0.72 ± 0.09. XTE J1118+480 is thus the third system -together with GX339-4 and V404 Cyg -for which a tight, non-linear radio/X-ray correlation has been reported over more than 5 dex in X . Confirming previous results, we find no evidence for a dependence of the correlation normalisation of an individual system on orbital parameters, relativistic boosting, reported black hole spin and/or black hole mass. We then perform a clustering and linear regression analysis on what is arguably the most up-to-date collection of coordinated radio and X-ray luminosity measurements from quiescent and hard state black hole X-ray binaries, including 24 systems. At variance with previous results, a two-cluster description is statistically preferred only for random errors < ∼ 0.3 dex in both r and X , a level which we argue can be easily reached when the known spectral shape/distance uncertainties and intrinsic variability are accounted for. A linear regression analysis performed on the whole data set returns a best-fitting slope β = 0.61 ± 0.03 and intrinsic scatter σ 0 = 0.31 ± 0.03 dex.

show abstract

Complete and Simultaneous Spectral Observations of the Black Hole X‐Ray Nova XTE J1118+480

Cited by 152 publications

References 24 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

A high-velocity black hole on a Galactic-halo orbit in the solar neighbourhood

The radio/X-ray domain of black hole X-ray binaries at the lowest radio luminosities

Contact Info

Product

Resources

About