Optical and Near-Infrared Spectroscopy of the Black Hole Swift J1753.5-0127Reportar como inadecuado

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1 ESO - European Southern Observatory 2 Department of Astronomy 3 SSL - Space Sciences Laboratory Berkeley 4 IRAP - Institut de recherche en astrophysique et planétologie 5 Laboratoire AIM 6 USN - Unité Scientifique de la Station de Nançay 7 CALTECH - California Institute of Technology 8 Department of Physics, Durham University 9 European Space Astronomy Centre, Apartado 10 Sabanci University Istanbul 11 JPL - Jet Propulsion Laboratory 12 CSIRO Astronomy & Space Science

Abstract : We report on a multiwavelength observational campaign of the black hole X-ray binary Swift J1753.5-0127 that consists of an ESO-X-shooter spectrum supported by contemporaneous Swift-XRT+UVOT and ATCA data. ISM absorption lines in the X-shooter spectrum allows us to determine EB-V=0.45+-0.02 along the line-of-sight to the source. We also report detection of emission signatures of He II at 4686 angstrom, H alpha, and, for the first time, H I at 10906 angstrom and Paschen Beta. The double-peaked morphology of these four lines is typical of the chromosphere of a rotating accretion disk. Nonetheless, the paucity of disk features points towards a low level of irradiation in the system. This is confirmed through spectral energy distribution modeling and we find that the UVOT+X-shooter continuum mostly stems from the thermal emission of a viscous disk. We speculate that the absence of reprocessing is due to the compactness of an illumination-induced envelope that fails to reflect enough incoming hard X-ray photons back to the outer regions. The disk also marginally contributes to the Compton-dominated X-ray emission and is strongly truncated, with an inner radius about a thousand times larger than the black hole-s gravitational radius. A near-infrared excess is present, and we associate it with synchrotron radiation from a compact jet. However, the measured X-ray flux is significantly higher than what can be explained by the optically thin synchrotron jet component. We discuss these findings in the framework of the radio quiet versus X-ray bright hypothesis, favoring the presence of a residual disk, predicted by evaporation models, that contributes to the X-ray emission without enhancing the radio flux.

Keywords : accretion discs Stars: individual: Swift J1753.5 0127 ISM: jets and outflows binaries: close X-rays: binaries Infrared: stars accretion

Autor: Farid Rahoui - John A. Tomsick - Mickael Coriat - Stéphane Corbel - Felix Fürst - Poshak Gandhi - Simone Migliari - Emrah Kalem

Fuente: https://hal.archives-ouvertes.fr/


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