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Zurita, C.; Torres, M. A. P.; Steeghs, D.; Rodriguez-Gil, P.; Munoz-Darias, T.; Casares, J.; Shahbaz, T.; Martinez-Pais, I. G.; Zhao, P.; Garcia, M. R.; Piccioni, A.; Bartolini, C.; Guarnieri, A.; Bloom, J. S.; Blake, C. H.; Falco, E. E.; Szentgyorgyi, A.; Skrutskie, M. (2006)
Publisher: Institute of Physics Publishing Ltd.
Languages: English
Types: Preprint
Subjects: QB, Astrophysics

Classified by OpenAIRE into

arxiv: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
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+-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+-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 mini-outbursts 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=19.02+-0.03 about three 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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    • Buxton, M. M., & Bailyn, C. D., 2004, ApJ, 615, 880 Callanan, P. J., Garcia, M. R., McClintock, J. E., Zhao, P., Remillard R. A., Bailyn, C. D., Orosz, J. A., Harmon, B. A.; Paciesas, W. S. 1995, ApJ, 441 786
    • Cannizzo, J. K.; Chen, W., & Livio, M. 1995, ApJ, 454, 880 Castro-Tirado, A. J., Ortiz, J. L., & Gallego, J., 1997, A&A, 322,507 Charles, P. A., & Coe, M. J. 2004, in Compact Stellar X-Ray Sources, ed. W. H. G. Lewin & M. van der Klis (Cambridge: Cambridge Univ. Press), in press (astro-ph/0308020) Chaty, S., Haswell, C. A., Malzac, J., Hynes, R. I., Shrader, C. R., & Cui, W. 2003, MNRAS, 346, 689
    • Chen, W., Shrader, C.R. & Livio, M. 1997, ApJ, 491, 312 Chevalier, C., & Ilovaisky, S. A. 1995, A&A, 297, 103 Chou, Y., Chen, A., Chiang, P. S., Hu, C. P., Hu, R. H. 2005, The Astronomer's Telegram, 412
    • Della Valle, M., Jarvis, B. J., & West, R. M., 1991, A&A, 247, 33 Dubus, G., Kim, R.S.J., Menou, K., Szkody, P., Bowen, D.V. 2001, ApJ, 553, 307 Eggleton, P. P. 1983, ApJ, 268, 368 Esin, A. A., McClintock, J. E., Drake, J. J., Garcia, M. R., Haswell, C. A., Hynes, R. I., Muno, M. P. 2001, ApJ, 555, 483
    • Fender, R. P., Hjellming, R. M., Tilanus, R. P. J., Pooley, G. G., Deane, J. R., Ogley, R. N., & Spencer, R. E. 2001, MNRAS, 322, 23
    • Garcia, M., Brown, W., Pahre, M., McClintock, J., Callanan, P., & Garnavich, P. 2000, IAU Circ., 7392, 2
    • Hameury, J. M., Lasota, J. P., McClintock, J. E., & Narayan, R. 1997, ApJ, 489, 234 Hauschildt, P.H., Allard, F., & Baron, E. 1999, ApJ, 512, 377 Homan, J., Buxton, M., Markoff, S., Bailyn C.D., Nespoli, E., & Belloni T. 2005, ApJ, 624, 295
    • Hynes, R. I., Mauche, C. W., Haswell, C. A., Shrader, C. R., Cui, W., & Chaty, S. 2000, ApJ, 539, 37
    • Hynes, R. I. 2005, ApJ, 623, 1026 Landolt, A. U. 1992, AJ, 104, 340 Levine, A. M., Bradt, H., Cui, W., Jernigan, J. G., Morgan, E. H., Remillard, R., Shirey, R. E., & Smith, D. A. 1996, ApJ, 469, 33L
    • Malzac, Julien, Merloni, Andrea, & Fabian, Andrew C. 2004, ApJ, 614, 641 Markoff, S., Falcke, H., & Fender, R. 2001, A&A, 372, 25 McClintock, J. E., Garcia, M. R., Caldwell, N., Falco, E. E., Garnavich, P. M., & Zhao, P. 2001, ApJ, 551, L147
    • McClintock, J. E., Haswell, C. A., Garcia, M. R., Drake, J. J., Hynes, R. I., Marshall, H. L., Muno, M. P., Chaty, S., Garnavich, P. M., Groot, P. J., and 6 coauthors 2001, ApJ, 555, 477
    • McClintock, Jeffrey E., Narayan, Ramesh, Garcia, Michael R., Orosz, Jerome A., Remillard, Ronald A., Murray & Stephen S., 2003, ApJ, 593, 435
    • McClintock, Jeffrey E., Remillard & Ronald A., 2005, to appear in Compact Stellar Xray Sources, ed. W. H. G. Lewin, & M. van der Klis (Cambridge University Press) [astro-ph/0306213]
    • Merloni, A., & Fabian, A. C. 2001, MNRAS, 332, 165 Merloni, A., Di Matteo, T. & Fabian, A. C. 2001, A&AS, 276, 213 Merloni, A.,& Fabian, A. C. 2002, MNRAS, 321, 549 Mirabel I. F., Dhawan, V., Mignani, R. P., Rodrigues, I., Guglielmetti, F. 2001, Nature, 413, 139
    • Orosz, J. A., Remillard, R. A., Bailyn, C. D., & McClintock, J. E., 1997,ApJ, 478, 830 Orosz, J. A. 2001, The Astronomer's Telegram, 67 Patterson, J. et al. 2000, IAU Circ., 7412, 2 Pooley, G. G., & Waldram, E. M. 2000, IAU Circ., 7390, 2 Pringle, J. E., Verbunt, F., & Wade, R. A. 1986, MNRAS, 221, 169 Remillard, R., Morgan, E., Smith, D., & Smith E. 2000, IAU Circ., 7389, 2 Rieke, G.H., & Lebofsky, M.J. 1985, ApJ, 288, 618 Shahbaz, T., Bandyopadhyay, R.M., Charles, P.A., Wagner, R.M., Mulhi, P., Hakala, P., Casares, J., & Greenhill, J. 1998, MNRAS, 300, 1035
    • Shakura, N.I., & Sunyaev, R. A. 1973, A&A, 24, 337 Torres, M. A. P., Callanan, P. J., Garcia, M. R., McClintock, J.E., Garnavich, P., Balog, Z., Berlind, P., Brown, W.R., Calkins, M., Mahdavi, A. 2002, ApJ, 569, 423
    • Torres, M. A. P., Callanan, P. J., Garcia, M. R., Zhao, P., Laycock, S., & Kong, A. K. H. 2004, ApJ, 612, 225
    • Wagner, R. M., Foltz, C. B., Shahbaz, T., Casares, J., Charles, P. A., Starrfield, S. G., & Hewett, P. 2001 ApJ, 556, 42
    • Wood, K. S., Titarchuk, L., Ray, P. S., Wolff, M. T., Lovellette, M. N., & Bandyopadhyay, R. M. 2001 ApJ, 563, 246
    • Wren, J., Akerlof, C., Balsano, R., Bloch, J., Borozdin, K., Casperson, D., Gisler, G., Kehoe, R., Lee, B. C., 2001, ApJ, 557, 97
    • Zurita, C., Casares, J., Shahbaz, T., Wagner, R. M., Foltz, C. B., Rodr´ıguez-Gil, P., Hynes, R. I., Charles, P. A., Ryan, E., Schwarz, G., & Starrfield, S. G. 2002, MNRAS, 333, 791
    • Zurita, C., S´anchez-Fern´andez, C., Casares, J., Charles, P. A., Abbott, T. M., Hakala, P., Rodr´ıguez-Gil, P., Bernabei, S., Piccioni, A., Guarnieri, A., and 5 coauthors 2002, MNRAS, 334, 999
    • Zurita, C., Rodr´ıguez, D., Rodr´ıguez-Gil, P., Casares, J., Shahbaz, T., Acosta, J., G´omezVelarde, G., Abajas, C., Mun˜oz-Darias, T. 2002, The Astronomer's Telegram, 383
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