EPJ Web of Conferences
Volume 61, 2013The Innermost Regions of Relativistic Jets and Their Magnetic Fields
|Number of page(s)||4|
|Section||Jet from stellar-mass objects|
|Published online||09 December 2013|
Evidence for quiescent synchrotron emission in the black hole X-ray transient Swift J1357.2–0933
1 Instituto de Astrofísica de Canarias (IAC), E-38200 La Laguna, Tenerife, Spain
2 Dept. Astrofísica Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain
3 Department of Physics and Astronomy, University of Sheffield, Sheffield, S3 7RH, UK
4 Department of Physics, University of Warwick, Coventry CV4 7AL, UK
a e-mail: firstname.lastname@example.org
Published online: 9 December 2013
We present high time-resolution optical and infrared observations of the edge-on black hole X-ray transient Swift J1357.2-0933. Our data taken in 2012 shows the system to be at its pre-outburst magnitude and so the system is in quiescence. In contrast to other X-ray transients, the quiescent light curves of Swift J1357.2-0933 do not show the secondary star’s ellipsoidal modulation. The optical and infrared light curves is dominated by variability with an optical fractional rms of about 20 per cent, much larger than what is observed in other systems. The quiescent ultraviolet to mid-IR spectral energy distribution in quiescence is dominated by a nonthermal component with a power–law index of −1.4, (the broad-band rms SED has a similar index) which arises from optically thin synchrotron emission from a jet; the lack of a peak in the spectral energy distribution rules out advection-dominated models (based on ).
© Owned by the authors, published by EDP Sciences, 2013
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