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

• DOI: 10.1093/mnras/stw2020
• Publication Date: 2016-08-13T00:07:24Z
• Authors: A. P. Rushton; A. W. Shaw; R. P. Fender; D. Altamirano; P. Gandhi; P. Uttley; P. A. Charles; M. Kolehmainen; G. E. Anderson; C. Rumsey; D. J. Titterington
• Keywords: stars: jets; High Energy Astrophysical Phenomena (astro-ph.HE); X-rays: binaries; accretion discs - time; accretion; FOS: Physical sciences; [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]; [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]; Astrophysics - High Energy Astrophysical Phenomena; 530; radio continuum: stars; 520; stars: black holes

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 $��=0.96\pm0.06$ 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 $<21~��$Jy, which is a quenching factor of $\gtrsim25$<br/>8 pages, 4 figures, Accepted for publication in MNRAS<br/>