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| Main Authors: | , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2506.20536 |
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| _version_ | 1866918134704766976 |
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| author | Borowski, E. S. Hynes, R. I. Hunt, Q. Tetarenko, A. J. Plotkin, R. M. Shahbaz, T. Gandhi, P. Maccarone, T. J. Miller-Jones, J. C. A. Heinke, C. O. Shaw, A. W. Russell, T. D. Sivakoff, G. R. Charles, P. A. Palaiologou, E. V. Reig, P. |
| author_facet | Borowski, E. S. Hynes, R. I. Hunt, Q. Tetarenko, A. J. Plotkin, R. M. Shahbaz, T. Gandhi, P. Maccarone, T. J. Miller-Jones, J. C. A. Heinke, C. O. Shaw, A. W. Russell, T. D. Sivakoff, G. R. Charles, P. A. Palaiologou, E. V. Reig, P. |
| contents | Observations of some quiescent black hole X-ray binaries have revealed an excess of mid-infrared (MIR) emission above that expected from their donor stars. In one system, V404 Cygni, this excess has been variously suggested to arise from the accretion disk, circumbinary material, or a compact relativistic jet. Here we present simultaneous James Webb Space Telescope (JWST), Atacama Large Millimeter/submillimeter Array (ALMA), and complementary multi-wavelength observations undertaken to resolve this uncertainty. We observed large-amplitude 21 $μ$m variability on short timescales with JWST, particularly a dramatic flare which swiftly rose to $\approx2.4$ mJy, over 10 times the lowest observed MIR flux density. Similar variability was simultaneously observed from radio to X-ray wavelengths with other facilities throughout the campaign. This variability and the flat radio/mm/MIR spectral index ($α= 0.04 \pm 0.01$) suggest that the MIR excess at and longward of 21 $μ$m in V404 Cyg does not arise from the accretion disk or circumbinary material. Instead, the emission at 21 $μ$m is dominated by synchrotron radiation from a jet which persists into quiescence. This result reinforces the ubiquity of the disk-jet connection in accreting black holes across a range of masses and accretion rates. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2506_20536 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The Mid-infrared Emitting Jet in the Black Hole V404 Cygni in Quiescence Borowski, E. S. Hynes, R. I. Hunt, Q. Tetarenko, A. J. Plotkin, R. M. Shahbaz, T. Gandhi, P. Maccarone, T. J. Miller-Jones, J. C. A. Heinke, C. O. Shaw, A. W. Russell, T. D. Sivakoff, G. R. Charles, P. A. Palaiologou, E. V. Reig, P. High Energy Astrophysical Phenomena Observations of some quiescent black hole X-ray binaries have revealed an excess of mid-infrared (MIR) emission above that expected from their donor stars. In one system, V404 Cygni, this excess has been variously suggested to arise from the accretion disk, circumbinary material, or a compact relativistic jet. Here we present simultaneous James Webb Space Telescope (JWST), Atacama Large Millimeter/submillimeter Array (ALMA), and complementary multi-wavelength observations undertaken to resolve this uncertainty. We observed large-amplitude 21 $μ$m variability on short timescales with JWST, particularly a dramatic flare which swiftly rose to $\approx2.4$ mJy, over 10 times the lowest observed MIR flux density. Similar variability was simultaneously observed from radio to X-ray wavelengths with other facilities throughout the campaign. This variability and the flat radio/mm/MIR spectral index ($α= 0.04 \pm 0.01$) suggest that the MIR excess at and longward of 21 $μ$m in V404 Cyg does not arise from the accretion disk or circumbinary material. Instead, the emission at 21 $μ$m is dominated by synchrotron radiation from a jet which persists into quiescence. This result reinforces the ubiquity of the disk-jet connection in accreting black holes across a range of masses and accretion rates. |
| title | The Mid-infrared Emitting Jet in the Black Hole V404 Cygni in Quiescence |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2506.20536 |