The Mass of the Black Hole in Xte J1118+480

Khargharia, Juthika; Froning, Cynthia S.; Robinson, E. L.; Gelino, Dawn

doi:10.1088/0004-6256/145/1/21

Cited by 60 publications

(52 citation statements)

References 51 publications

(84 reference statements)

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“…Cantrell et al (2010) obtained robust estimates of i and M for A0620−00 using nearly simultaneous spectroscopic and photometric data to constrain the disk fraction. Khargharia et al (2013) likewise obtained highquality constraints on i and M for XTE J1118+480 based on NIR photometry and spectroscopy performed on the same night. GS 2000+25 appears to be a very favorable system; the disk fraction is minimal, and the orbital modulation almost purely ellipsoidal.…”

Section: Distance Of Novamusmentioning

confidence: 82%

The Mass of the Black Hole in the X-Ray Binary Nova Muscae 1991

Chen

Gou

McClintock

et al. 2016

ApJ

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The optical counterpart of the black-hole soft X-ray transient Nova Muscae 1991 has brightened by ∆V ≈ 0.8 mag since its return to quiescence 23 years ago. We present the first clear evidence that the brightening of soft X-ray transients in quiescence occurs at a nearly linear rate. This discovery, and our precise determination of the disk component of emission obtained using our simultaneous photometric and spectroscopic data, have allowed us to identify and accurately model archival ellipsoidal light curves of the highest quality. The simultaneity, and the strong constraint it provides on the component of disk emission, is a key element of our work. Based on our analysis of the light curves, and our earlier measurements of the mass function and mass ratio, we have obtained for Nova Muscae 1991 the first accurate estimates of its systemic inclination i = 43.2 −0.65 kpc. We discuss the implications of our work for future dynamical studies of black-hole soft X-ray transients.

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Section: Distance Of Novamusmentioning

confidence: 82%

The Mass of the Black Hole in the X-Ray Binary Nova Muscae 1991

Chen

Gou

McClintock

et al. 2016

ApJ

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“…Then, the difference in radio normalisation attributed to Doppler beaming depends only on the orbital inclination of the system (assuming the jet axis is perpendicular to the orbital plane). Both XTE J1118+480 and V404 Cyg have well-determined orbital inclinations, of i = 68 • ± 2 • (Gelino et al 2006; see also Khargharia et al 2013 for a somewhat broader constraints and Farr et al 2011;Kreidberg et al 2012 for a comprehensive statistical analysis) and i = 67 Khargharia, Froning & Robinson 2010;Farr et al 2011;Kreidberg et al 2012), respectively. The inclination of GX 339-4 is only known to be < ∼ 60 • (Cowley et al 2002), and we assume a range from 45−60 • here (see Zdziarski et al 2004).…”

Section: Summary and Discussionmentioning

confidence: 93%

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

153

200

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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.

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“…Quiescent BHXBs are known to experience a lowlevel of flux variability (e.g., Khargharia et al 2013;Shahbaz et al 2013;Bernardini & Cackett 2014, and references therein). Muno & Mauerhan (2006) estimate that a level of flux variability in the IR of ∼30% could be reasonable.…”

Section: Non-simultaneous Infrared Datamentioning

confidence: 99%

“…The companion star to J1118 is known to have a late-type spectral class (Khargharia et al 2013). So we include a blackbody component at a fixed temperature T * = 3400 K, and we normalize this component by assuming an emitting sphere with radius R * = 0.56 R⊙.…”

Section: Multi-zone Jet Modelmentioning

confidence: 99%

“…Results from our best model-fit are presented in Section 4, which are then discussed in Section 5. Throughout, we adopt the following parameters for J1118: black hole mass MBH = 7.5 M ⊙ , orbital inclination i = 68 • (Khargharia et al 2013), and distance d = 1.72 ± 0.10 kpc (Gelino et al 2006). The orbital period is P orb = 4.08(±5 × 10 −6 ) h (Torres et al 2004).…”

Section: Introductionmentioning

confidence: 99%

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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 Mass of the Black Hole in Xte J1118+480

Cited by 60 publications

References 51 publications

The Mass of the Black Hole in the X-Ray Binary Nova Muscae 1991

The Mass of the Black Hole in the X-Ray Binary Nova Muscae 1991

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

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

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