Disc–jet quenching of the galactic black hole Swift J1753.5−0127

Abstract

We report on radio and X-ray monitoring observations of the BHC Swift J1753.5-0127 taken over a ∼ 10 year period. Presented are daily radio observations at 15 GHz with the AMI-LA and X-ray data from Swift XRT and BAT. Also presented is a deep 2hr JVLA observation taken in an unusually low-luminosity soft-state (with a low disk temperature). We show that although the source has remained relatively radio-quiet compared to XRBs with a similar X-ray luminosity in the hard-state, the power-law relationship scales as ζ = 0.96 ± 0.06 i.e. slightly closer to what has been considered for radiatively inefficient accretion disks. We also place the most stringent limit to date on the radio-jet quenching in an XRB soft-state, showing the connection of the jet quenching to the X-ray power-law component; the radio flux in the soft-state was found to be < 21 µJy, which is a quenching factor of 25.

Up and Down the Black Hole Radio/X-Ray Correlation: The 2017 Mini-outbursts from Swift J1753.5−0127

“…Data points during the rise out of quiescence (three epochs) are circumscribed by squares. The cyan upside down triangles show the location of J1753 in the "radio-faint" hard state during its 11  year outburst (data taken from Rushton et al 2016). For uniformity, all X-ray error bars are rescaled to 68% confidence.…”

“…The distance to J1753 is suggested to fall between 2 and 8 kpc Froning et al 2014). Following Rushton et al (2016), we adopt 8 kpc here, although adopting a lower value does not (qualitatively) alter our conclusions. Unless stated otherwise, we define X-ray luminosities from 1 to 10 keV, and we report uncertainties on radio and X-ray parameters at the 68% and 90% confidence levels, respectively.…”

“…We therefore add uncertainties to the radio luminosity error bars in Figure 2 to account for a radio spectrum that could be as inverted as 0.3 r a = . For comparison, we also display radio and X-ray observations of J1753 during its 2005-2016 outburst in Figure 2, when J1753 was in the radio-faint hard state (Rushton et al 2016). To illustrate the "standard" track in Figure 2, we adopt the best-fit to the BHXB GX 339−4 from Gallo et al (2014; we use GX 339−4 as a representative example because it has the most data coverage for any "standard" track BHXB, taken over multiple outbursts; Corbel et al 2013a).…”

“…We also highlight the path H1743−322 took through the L R -L X plane to emphasize that J1753 appears to occupy a similar parameter space. Figure 2 shows that during the 2017 mini-outbursts, J1753 occupies a region of the L R -L X plane that is inconsistent with the L L R X 0.96 µ correlation it followed during its outburst (Rushton et al 2016). Even though J1753 appears to always fall below the radio/X-ray correlation defined by GX 339−4 (dashed solid line), its path through the radio/X-ray plane is clearly different above and below L 10 erg s…”

“…J1753 is also an intriguing target because it was established as a "radio-faint" BHXB (e.g., Cadolle Soleri et al 2010) where it followed L L R X 0.96 Rushton et al 2016) while in the hard state. J1753 is likely to host a black hole instead of a neutron star.…”