Abstract The candidate black hole X-ray binary Swift J1753.5−0127 faded to quiescence in 2016 November after a prolonged outburst that was discovered in 2005. Nearly three months later, the system displayed renewed activity that lasted through 2017 July. Here, we present radio and X-ray monitoring over ≈ 3 months of the renewed activity to study the coupling between the jet and the inner regions of the disk/jet system. Our observations cover low X-ray luminosities that have not historically been well-sampled ( L X ≈ 2 × 10 33 – 10 36 erg s − 1 ; 1–10 keV), including time periods when the system was both brightening and fading. At these low luminosities, Swift J1753.5−0127 occupies a parameter space in the radio/X-ray luminosity plane that is comparable to “canonical” systems (e.g., GX 339−4), regardless of whether the system was brightening or fading, even though during its ≳11 year outburst, Swift J1753.5−0127 emitted less radio emission from its jet than expected. We discuss implications for the existence of a single radio/X-ray luminosity correlation for black hole X-ray binaries at the lowest luminosities ( L X ≲ 10 35 erg s − 1 ), and we compare to supermassive black holes. Our campaign includes the lowest luminosity quasi-simultaneous radio/X-ray detection to date for a black hole X-ray binary during its rise out of quiescence, thanks to early notification from optical monitoring combined with fast responses from sensitive multiwavelength facilities.

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