The 2005 Outburst of the Halo Black Hole X‐Ray Transient XTE J1118+480
Torres, M. A. P.
Martinez-Pais, I. G.
Garcia, M. R.
Bloom, J. S.
Blake, C. H.
Falco, E. E.
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CitationZurita, C., M. A. P. Torres, D. Steeghs, P. Rodriguez‐Gil, T. Munoz‐Darias, J. Casares, T. Shahbaz, et al. 2006. “The 2005 Outburst of the Halo Black Hole X‐Ray Transient XTE J1118+480.” The Astrophysical Journal 644 (1): 432–38. https://doi.org/10.1086/503286.
AbstractWe 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 similar to 5.7 +/- 0.1 mag in the R band and similar to 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 +/- 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 GROJ0422+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 = 19.02 +/- 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-nu proportional to nu(alpha) increasing toward the blue. At the peak of the outburst, we derived alpha = 0.49 +/- 0.04 for the optical data alone and alpha = 0.1 +/- 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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