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Evidence for quiescent synchrotron emission in the black hole X-ray transient Swift J1357.2-0933
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Shahbaz, T., Russell, D. M., Zurita, C., Casares, J., Corral-Santana, J. M., Dhillon, V. S. and Marsh, Tom (2013) Evidence for quiescent synchrotron emission in the black hole X-ray transient Swift J1357.2-0933. Monthly Notices of the Royal Astronomical Society, 434 (3). pp. 2696-2706. doi:10.1093/mnras/stt1212 ISSN 0035-8711.
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Official URL: http://dx.doi.org/10.1093/mnras/stt1212
Abstract
We present high time resolution ULTRACAM optical and NOTCam infrared observations of the edge-on black hole X-ray transient Swift J1357.2−0933. Our data taken in 2012 and 2013 show 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 light curve is dominated by variability with an optical fractional rms of ∼35 per cent, a factor of >3 larger than what is observed in other systems at similar time resolution. Optical flare events lasting 2–10 min with amplitudes of up to ∼1.5 mag are seen as well as numerous rapid ∼0.8 mag dip events which are similar to the optical dips seen in outburst. Similarly, the infrared J-band light curve is dominated by variability with a fractional rms of ∼21 per cent, and flare events lasting 10–30 min with amplitudes of up to ∼1.5 mag are observed.
The quiescent optical to mid-infrared spectral energy distribution (SED) in quiescence is dominated by a non-thermal 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 most likely originating in a weak jet; the lack of a peak in the SED rules out advection-dominated models.
Using the outburst amplitude–period relation for X-ray transients, we estimate the quiescent magnitude of the secondary star to lie in the range Vmin = 22.7–25.6, which when combined with the absolute magnitude of the expected M4.5 V secondary star allows us to constrain the distance to lie in the range 0.5–6.3 kpc. The short orbital period argues for a nuclearly evolved star with an initial mass ∼1.5 M⊙, which has evolved to a 0.17 M⊙ star. The high Galactic latitude of Swift J1357.2−0933 implies a scaleheight in the range 0.4–4.8 kpc above the Galactic plane, possibly placing Swift J1357.2−0933 in a sub-class of high-z short-period black hole X-ray transients in the Galactic halo.
| Item Type: | Journal Article | ||||||||
|---|---|---|---|---|---|---|---|---|---|
| Divisions: | Faculty of Science, Engineering and Medicine > Science > Physics | ||||||||
| Journal or Publication Title: | Monthly Notices of the Royal Astronomical Society | ||||||||
| Publisher: | Oxford University Press | ||||||||
| ISSN: | 0035-8711 | ||||||||
| Official Date: | 21 September 2013 | ||||||||
| Dates: |
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| Volume: | 434 | ||||||||
| Number: | 3 | ||||||||
| Page Range: | pp. 2696-2706 | ||||||||
| DOI: | 10.1093/mnras/stt1212 | ||||||||
| Status: | Peer Reviewed | ||||||||
| Publication Status: | Published | ||||||||
| Access rights to Published version: | Restricted or Subscription Access |
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