Optical and Infrared Photometry of the Microquasar GRO J1655–40 in Quiescence

By Jenny E. Greene, C. Bailyn, J. Orosz. 2001

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We present BVIJK photometry of the black hole candidate GRO J1655-40 in full quiescence. We report a refined orbital period of 2.62191 ± 0.00020 days. The light curves are dominated by ellipsoidal variations from the secondary star. We model the light curves with an upgraded code that includes a more accurate treatment of limb darkening. Previous models containing a large cool disk are ruled out, and, indeed, our data can be fitted with a pure ellipsoidal light curve without any disk contribution. In general agreement with previous results, we derive a confidence region of the correlated quantities inclination and mass ratio, centered on an inclination of 70.°2 ± 1.°9 and mass ratio of 2.6 ± 0.3, resulting in a primary mass M1 = 6.3 ± 0.5 M☉ (all 95% confidence). The complex limits and errors on these values and on the possible disk contribution to the light curve are discussed.

Subfields: Astronomy and Astrophysics, Biomedical Engineering

View Paper: https://www.semanticscholar.org/paper/459b34b302cd7106227a50547e94c36818729251

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Citations in the corpus

The Masses and Spins of Neutron Stars and Stellar-Mass Black Holes (2014, background): “Studies of some black holes conclude that the alignment is good, such as for XTE J1550-564 [225], whereas for other sources such as GRO J1655-40 (see [226] for the jet orientation and [106] for the”
The orbital resonance model for twin peak kHz quasi periodic oscillations in microquasars (2005, background): “McClintock & Remillard (2004), state νupp/νlow = 242 (±3 Hz) /166 (±5 Hz). d Twin peak kHz QPOs reported by Remillard et al. (2003). e See Greene et al. (2001); Orosz et al. (2002); Greiner et al. (2001), and McClintock & Remillard (2003). general accretion flows, the idea may be best illustrated…”
Global optical/infrared-X-ray correlations in X-ray binaries: quantifying disc and jet contributions (2006, unknown): “…(32) Hynes (2005); (33) McClintock, Horne & Remillard (1995); (34) Torres et al. (2004); (35) Orosz et al. (1996); (36) Orosz et al. (1998); (37) Greene et al. (2001); (38) Shahbaz, Fender & Charles (2001); (39) Zurita et al. (2002); (40) Casares et al. (1993); (41) Brocksopp et al. (2004);…”
Do X-ray binary spectral state transition luminosities vary? (2003, background): “The mass estimates come from Greene et al. (2001).”
Evidence for Harmonic Relationships in the High-Frequency Quasi-periodic Oscillations of XTE J1550–564 and GRO J1655–40 (2002, methodology): “On the other hand, the inverse ratio of black hole masses is 1:59 0:27 (Orosz et al. 2002; Greene et al. 2001), suggesting that the fundamental frequencies scale as M 1.”
MASS MEASUREMENTS OF BLACK HOLES IN X-RAY TRANSIENTS: IS THERE A MASS GAP? (2012, methodology): “We therefore adopt the Beer & Podsiadlowski (2002) measurement, which is compatible with the Greene et al. (2001) result, and assume the source was passive during the observations, thus taking i ∼ N(69.0◦, 3.0◦).”
WATCHDOG: A COMPREHENSIVE ALL-SKY DATABASE OF GALACTIC BLACK HOLE X-RAY BINARIES (2015, background): “Studies of the orbital parameters in full quiescence published by Orosz & Bailyn (1997), Greene et al. (2001) and Beer & Podsiadlowski (2002), all of which are consistent, providedPorb andMBH, and confirmed the BH nature of the primary.”