The radio/X‐ray correlation in Swift J1753.5–0127

Abstract

Great effort has gone into trying to explain the two observed radio/X-ray correlation tracks seen in the low/hard state of black hole X-ray binaries in recent years. The original, "standard" correlation of the form L R ∝ L b X , where b = 0.7 ± 0.1, is paired with a separate, lower correlation track with a steeper slope of ∼ 1-1.4, at least at high luminosities. These outlier sources seem to show fainter radio emission than expected for a given X-ray luminosity, thus acquiring the term "radio-quiet". While most sources seem to maintain their intrinsic correlation slopes over decades in luminosity, a growing sample of sources have recently been reported to move from one correlation to the other. We present preliminary results from a coordinated radio/X-ray monitoring campaign of the radio-quiet black hole binary Swift J1753.5−0127, spanning nearly two years in time. Our observations add lower-luminosity coverage to an existing sample of observations, and we observe the radio-quiet track to proceed horizontally towards the standard correlation as the X-ray luminosity slowly starts to decrease. The source stays on the transition track for ∼ 60 days, during which its X-ray luminosity is observed to drop by more than an order of magnitude while its radio luminosity stays constant. Time-averaged X-ray energy spectra show very little change during this phase, leaving no obvious parameters to explain the observed transition behaviour.

Properties of X-Ray Flux of Jets during the 2005 Outburst of Swift J1753.5−0127 Using the TCAF Solution

“…Instead of the 2.5 − 25 keV total Xray flux (F X ), using the 3 − 9 keV soft X-ray flux, we find a less steep exponent of b ∼ 1.05 ± 0.14. Our result is consistent with several other authors, who also have found a steeper exponent for this particular BHC with b ∼ 1.0 − 1.4 (Soleri et al 2010, Rushton et al 2016, Kolehmainen et al 2016. This BHC candidate is less luminous in radio which may be the reason behind getting a steeper index (Soleri et al 2010).…”

“…Several authors have found radio/X-ray correlation for this source. This does not fall on the traditional correlation track, rather, it shows power-law index to be steeper ∼ 1 − 1.4 (Soleri et al 2010, Rushton et al 2016, Kolehmainen et al 2016.…”