A late jet rebrightening revealed from multi-wavelength monitoring of the black hole candidate XTE J1752-223

TL;DR

This study monitors the black hole candidate XTE J1752-223 across multiple wavelengths during its 2009-2010 outburst, revealing a late jet rebrightening linked to optical and X-ray flares, and providing insights into jet and accretion processes.

Contribution

It presents multi-wavelength observations that identify the origin of a late optical flare as a synchrotron jet and isolates jet and disc components in the spectral energy distributions.

Findings

Optical flare coincides with X-ray rebrightening, suggesting a common origin.

Jet spectral index is nearly flat between radio and optical frequencies.

Mid-infrared data constrain the jet break to occur in the infrared.

Abstract

We present optical monitoring of the black hole candidate XTE J1752-223 during its 2009 - 2010 outburst and decay to quiescence. The optical light curve can be described by an exponential decay followed by a plateau, then a more rapid fade towards quiescence. The plateau appears to be due to an extra component of optical emission that brightens and then fades over ~ 40 days. We show evidence for the origin of this optical 'flare' to be the synchrotron jet during the decaying hard state, and we identify and isolate both disc and jet components in the spectral energy distributions. The optical flare has the same morphology and amplitude as a contemporaneous X-ray rebrightening. This suggests a common origin, but no firm conclusions can be made favouring or disfavouring the jet producing the X-ray flare. The quiescent optical magnitudes are B >= 20.6, V >= 21.1, R >= 19.5, i' >= 19.2. From the optical outburst amplitude we estimate a likely orbital period of < 22 h. We also present near-infrared (NIR) photometry and polarimetry and rare mid-infrared imaging (8 - 12 microns) when the source is nearing quiescence. The fading jet component, and possibly the companion star may contribute to the NIR flux. We derive deep mid-IR flux upper limits and NIR linear polarization upper limits. With the inclusion of radio data, we measure an almost flat jet spectral index between radio and optical; F_nu ~ nu^(~ +0.05). The data favour the jet break to optically thin emission to reside in the infrared, but may shift to frequencies as high as the optical or UV during the peak of the flare.