Infrared contamination in Galactic X-ray novae

Reynolds, M. T.; Callanan, P. J.; Robinson, E. L.; Froning, Cynthia S.

doi:10.1111/j.1365-2966.2008.13272.x

Cited by 11 publications

(12 citation statements)

References 51 publications

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“…Nevertheless, it has often been found that the accretion disc contributes 10–45 per cent to the optical R ‐band light in black hole transients (BHTs) in quiescence (see references above and e.g. Reynolds et al 2008 and references therein). Conservatively, assuming an accretion disc contribution of 50 per cent to the R ‐band luminosity and an M2 V companion star, we derive a distance of 5.9 kpc, which we round to 6 kpc.…”

Section: Discussionmentioning

confidence: 99%

The black hole candidate MAXI J1659-152 in and towards quiescence in X-ray and radio

Jonker

Miller-Jones

Homan

et al. 2012

Monthly Notices of the Royal Astronomical Society

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In this paper we report on Expanded Very Large Array radio and Chandra and Swift X‐ray observations of the outburst decay of the transient black hole candidate MAXI J1659–152 in 2011. We discuss the distance to the source taking the high inclination into account and conclude that the source distance is probably 6 ± 2 kpc. The lowest observed flux corresponds to a luminosity of erg s−1. This, together with the orbital period of 2.4 h reported in the literature, suggests that the quiescent X‐ray luminosity is higher than predicted on the basis of the orbital period–quiescent X‐ray luminosity relationship. It is more in line with that expected for a neutron star, although the outburst spectral and timing properties reported in the literature strongly suggest that MAXI J1659–152 harbours a black hole. This conclusion is subject to confirmation of the lowest observed flux as the quiescent flux. The relation between the accretion and ejection mechanisms can be studied using the observed correlation between the radio and X‐ray luminosities as these evolve over an outburst. We determine the behaviour of MAXI J1659–152 in the radio–X‐ray diagram at low X‐ray luminosities using the observations reported in this paper and at high X‐ray luminosities using values reported in the literature. At high X‐ray luminosities, the source lies closer to the sources that follow a correlation index steeper than 0.6–0.7. However, when compared to other sources that follow a steeper correlation index, the X‐ray luminosity in MAXI J1659–152 is also lower. The latter can potentially be explained by the high inclination of MAXI J1659–152 if the X‐ray emission comes from close to the source and the radio emission is originating in a more extended region. However, it is probable that the source was not in the canonical low‐hard state during these radio observations and this may affect the behaviour of the source as well. At intermediate X‐ray luminosities, the source makes the transition from the radio underluminous sources in the direction of the relation traced by the ‘standard’ correlation similar to what has been reported for H 1743−322 in the literature. However, MAXI J1659–152 remains underluminous with respect to this ‘standard’ correlation.

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Section: Discussionmentioning

confidence: 99%

The black hole candidate MAXI J1659-152 in and towards quiescence in X-ray and radio

Jonker

Miller-Jones

Homan

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…The extragalactic sources may also be contaminated by supernova remnants along the line of sight, though this can be mitigated by going to higher frequencies. Stellar mass uncertainties are dominated by uncertainties in distance, inclination, and light from accretion (see Reynolds et al 2008).…”

Section: 3mentioning

confidence: 99%

The Fundamental Plane of Accretion Onto Black Holes With Dynamical Masses

Gültekin

Cackett

Miller

et al. 2009

ApJ

207

288

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Black hole accretion and jet production are areas of intensive study in astrophysics. Recent work has found a relation between radio luminosity, X-ray luminosity, and black hole mass. With the assumption that radio and X-ray luminosity are suitable proxies for jet power and accretion power, respectively, a broad fundamental connection between accretion and jet production is implied. In an effort to refine these links and enhance their power, we have explored the above relations exclusively among black holes with direct, dynamical massmeasurements. This approach not only eliminates systematic errors incurred through the use of secondary mass measurements, but also effectively restricts the range of distances considered to a volume-limited sample. Further, we have exclusively used archival data from the Chandra X-ray Observatory to best isolate nuclear sources. We find log L R = (4.80 ± 0.24) + (0.78 ± 0.27)log M BH + (0.67 ± 0.12)log L X , in broad agreement with prior efforts. Owing to the nature of our sample, the plane can be turned into an effective mass predictor. When the full sample is considered, masses are predicted less accurately than with the well-known M-σ relation. If obscured AGN are excluded, the plane is potentially a better predictor than other scaling measures.

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“…However, in no case has the disk contribution to the optical/NIR light curves been robustly constrained. In the most recent work, Gelino et al (2001) obtained an estimate of i = 54 • ± 1.5 • by modeling the J and K band light curves assuming that the disk contribution is negligible, an assumption that was subsequently shown to be ill-founded (Reynolds et al 2008;Kreidberg et al 2012). Based on the mass measurement of Gelino et al, Morningstar et al (2014) found a retrograde spin (a * = −0.25 +0.05 −0.64 ) for the black hole in NovaMus, which is a remarkable result for a black hole in a BHSXT, given that the spin of the black hole is believed to be accrued gradually over the lifetime of the system via accretion torques (Fragos & McClintock 2015).…”

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confidence: 99%

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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Infrared contamination in Galactic X-ray novae

Cited by 11 publications

References 51 publications

The black hole candidate MAXI J1659-152 in and towards quiescence in X-ray and radio

The black hole candidate MAXI J1659-152 in and towards quiescence in X-ray and radio

The Fundamental Plane of Accretion Onto Black Holes With Dynamical Masses

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

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