The compact jets of the black hole X-ray binary Swift J1753.5-0127 during its 2023-2024 outburst
Abstract
X-ray binaries are excellent laboratories to study the coupling between accretion and ejection phenomena around compact objects through multiwavelength observations. Swift J1753.5-0127 is a black hole low-mass X-ray binary discovered in outburst in 2005 that remained active for 11 years, followed by two mini-outbursts. We investigate the behavior of the compact jets of Swift J1753.5-0127 during its 2023-2024 outburst. We report a dense multiwavelength monitoring in the radio, NIR/optical/UV and X-ray bands. Using new and archival luminosity measurements, we construct a refined, smoother radio/X-ray plane that covers the steep/outlier and shallow/transition branches of the radio/X-ray correlation. We also present spectral energy distributions (SEDs) constructed using quasi-simultaneous observations from four epochs. Swift J1753.5-0127 underwent a faint, hard-only, double-peaked outburst, followed by a re-brightening in the optical. The updated radio/X-ray plane offers a clear view on the region occupied by this source, similar to MAXI J1348-630, but at lower radio luminosities than H 1743-322, and we confirm its hybrid behavior. The broad-band SED fitting reveals that a cool, truncated accretion disk dominates the NIR/optical/UV band. We find that the compact jets have a variable but weak contribution in the NIR, with a break frequency νbreak ≲ 5 × 1012 Hz, providing additional evidence that radio-quiet sources are also infrared-quiet. We also find evidence that the radio spectral index evolves with X-ray luminosity, transitioning from inverted values near quiescence to flatter or negative values at higher luminosities. In the context of adiabatic jet models, this trend may indicate that the jet geometry becomes increasingly confined as the accretion rate rises.
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BibTeX
@misc{grollimund2026compact,
title = {{The compact jets of the black hole X-ray binary Swift J1753.5-0127 during its 2023-2024 outburst}},
author = {Noa Grollimund and Stéphane Corbel and Lauren Rhodes and David M. Russell and M. Cristina Baglio and Francesco Carotenuto and Tristan Bouchet and Payaswini Saikia and Rob P. Fender and Sara E. Motta and Piergiorgio Casella and Kevin Alabarta and Fraser Lewis and Andrew K. Hughes and Fraser J. Cowie and Justine Crook-Mansour and Xian Zhang},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.18687},
eprint = {2610.18687},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.18687},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - The compact jets of the black hole X-ray binary Swift J1753.5-0127 during its 2023-2024 outburst
AU - Noa Grollimund
AU - Stéphane Corbel
AU - Lauren Rhodes
AU - David M. Russell
AU - M. Cristina Baglio
AU - Francesco Carotenuto
AU - Tristan Bouchet
AU - Payaswini Saikia
AU - Rob P. Fender
AU - Sara E. Motta
AU - Piergiorgio Casella
AU - Kevin Alabarta
AU - Fraser Lewis
AU - Andrew K. Hughes
AU - Fraser J. Cowie
AU - Justine Crook-Mansour
AU - Xian Zhang
PY - 2026
DA - 2026/10/13
PB - arXiv
DO - 10.48550/arxiv.2610.18687
UR - https://arxiv.org/abs/2610.18687
AB - X-ray binaries are excellent laboratories to study the coupling between accretion and ejection phenomena around compact objects through multiwavelength observations. Swift J1753.5-0127 is a black hole low-mass X-ray binary discovered in outburst in 2005 that remained active for 11 years, followed by two mini-outbursts. We investigate the behavior of the compact jets of Swift J1753.5-0127 during its 2023-2024 outburst. We report a dense multiwavelength monitoring in the radio, NIR/optical/UV and X-ray bands. Using new and archival luminosity measurements, we construct a refined, smoother radio/X-ray plane that covers the steep/outlier and shallow/transition branches of the radio/X-ray correlation. We also present spectral energy distributions (SEDs) constructed using quasi-simultaneous observations from four epochs. Swift J1753.5-0127 underwent a faint, hard-only, double-peaked outburst, followed by a re-brightening in the optical. The updated radio/X-ray plane offers a clear view on the region occupied by this source, similar to MAXI J1348-630, but at lower radio luminosities than H 1743-322, and we confirm its hybrid behavior. The broad-band SED fitting reveals that a cool, truncated accretion disk dominates the NIR/optical/UV band. We find that the compact jets have a variable but weak contribution in the NIR, with a break frequency ν_break ≲ 5 × 10^12 Hz, providing additional evidence that radio-quiet sources are also infrared-quiet. We also find evidence that the radio spectral index evolves with X-ray luminosity, transitioning from inverted values near quiescence to flatter or negative values at higher luminosities. In the context of adiabatic jet models, this trend may indicate that the jet geometry becomes increasingly confined as the accretion rate rises.
ER -