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On the Distances to the X-ray Binaries Cygnus X-3 and GRS 1915+105

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arxiv 2309.15027 v1 pith:ZVEGJLND submitted 2023-09-26 astro-ph.HE

M. J. Reid , J. C. A. Miller-Jones This is my paper · ORCID
classification astro-ph.HE
keywords distancesx-raydistanceparallaxpeculiarsourcesystemsassumption
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In this paper we significantly improve estimates of distance to the X-ray binary systems Cyg X-3 and GRS 1915+105. We report a highly accurate trigonometric parallax measurement for Cyg X-3 using the VLBA at 43 GHz, placing the source at a distance of 9.67+0.53-0.48 kpc. We also use Galactic proper motions and line-of-sight radial velocity measurements to determine 3-dimensional (3D) kinematic distances to both systems, under the assumption that they have low peculiar velocities. This yields distances of 8.95+-0.96 kpc for Cyg X-3 and 9.4+-0.6 (statistical)+-0.8 (systematic) for GRS 1915+105. The good agreement between parallax and 3D kinematic distances validates the assumption of low peculiar velocities, and hence small natal kicks, for both of the systems. For a source with a low peculiar velocity, given its parallax distance, Cyg X-3 should have a Vlsr near -64+-5 km/s. Our measurements imply a slightly higher inclination angle, and hence lower black hole mass for GRS 1915+105 than found from previous work by Reid et al (2014) and strengthen arguments from X-ray polarization that Cyg X-3 would be an ultraluminous X-ray source if viewed face-on.

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Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Simulation-based inference for AGN jet population modelling: Towards more robust comparisons of black hole jet speeds

    astro-ph.HE 2026-08 conditional novelty 6.0 of 10

    Using neural-posterior-estimation simulation-based inference on the MOJAVE FSRQ sample, the authors infer a Lorentz factor distribution slope b = -1.32 (+0.20, -0.19), consistent with X-ray binary jets at 2 sigma.

  2. Distinct Jet Properties in the X-Ray-Obscured State of GRS 1915+105

    astro-ph.HE 2026-07 conditional novelty 6.0 of 10

    VLBI observations during 2025 radio flares find no detectable jet motion in GRS 1915+105, implying its obscured-state jets are slower (βΓ≲0.40) than the pre-2019 relativistic jets.

  3. PeV extended emission around Galactic PeVatrons and echos of their flares

    astro-ph.HE 2026-07 conditional novelty 6.0 of 10

    The extended PeV source in Cygnus can be explained as a pair-creation halo around Cygnus X-3, possibly the delayed echo of a flare from about 50 years ago.

  4. An intrinsic decline of accretion activity in GRS 1915+105

    astro-ph.HE 2026-07 conditional novelty 6.0 of 10

    Deep X-ray, radio, and infrared non-detections of GRS 1915+105 imply an intrinsic decline in accretion activity rather than enhanced obscuration, likely driven by 2023-2024 outflows clearing the inner disc.

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