What is recorded here?
Gaia’s preliminary astrometric binary solution identified a metal-poor giant in an approximately 11.6-year orbit around an unseen massive companion. Gaia radial velocities and ground-based spectroscopy supported the orbital solution. Assuming the visible star’s modeled mass and a single dark companion, the team inferred a companion mass of 32.70±0.82 solar masses and identified a dormant black hole as the simplest explanation.
Source-linked catalogue note. A detailed explanatory guide has not yet been prepared for this entry.
Scientific scope
The companion is inferred from orbital motion rather than directly imaged. The astrometric data span roughly half an orbit, use preliminary calibrations and have possible parallax bias; the authors employ a combined spectroscopic solution to mitigate its effect on the mass function. The stellar mass depends on isochrone and extinction models. A compact inner binary containing black holes is not excluded by the observations. Association with an old stellar stream and implications for black-hole formation are interpretations, not direct measurements of the progenitor. The cited preprint precedes the final publication. Credit here is to the Gaia Collaboration; its full list of individual contributors is not shown.
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People and systems
Credit belongs to the cited collaborations. The individual author list is incomplete; no sole discoverer or individual effort share is inferred. The recorded author list is incomplete.
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English catalogue narrative
Gaia identifies a massive dark companion in the BH3 binary
Gaia’s preliminary astrometric binary solution identified a metal-poor giant in an approximately 11.6-year orbit around an unseen massive companion. Gaia radial velocities and ground-based spectroscopy supported the orbital solution. Assuming the visible star’s modeled mass and a single dark companion, the team inferred a companion mass of 32.70±0.82 solar masses and identified a dormant black hole as the simplest explanation.
Scientific scope
The companion is inferred from orbital motion rather than directly imaged. The astrometric data span roughly half an orbit, use preliminary calibrations and have possible parallax bias; the authors employ a combined spectroscopic solution to mitigate its effect on the mass function. The stellar mass depends on isochrone and extinction models. A compact inner binary containing black holes is not excluded by the observations. Association with an old stellar stream and implications for black-hole formation are interpretations, not direct measurements of the progenitor. The cited preprint precedes the final publication. Credit here is to the Gaia Collaboration; its full list of individual contributors is not shown.
Reading status
This is a source-linked WRS catalogue note. A full explanatory guide and independent scientific reconstruction have not been completed for this entry. Read the identified original work for its complete narrative and arguments.
People and systems
Credit belongs to the cited collaborations. The individual author list is incomplete; no sole discoverer or individual effort share is inferred.