000007365 001__ 7365
000007365 005__ 20250117162434.0
000007365 0247_ $$2DOI$$a10.1051/0004-6361/202449763
000007365 037__ $$aSCART-2025-0040
000007365 100__ $$aGaia Collaboration
000007365 245__ $$aDiscovery of a dormant 33 solar-mass black hole in pre-release Gaia astrometry 
000007365 260__ $$c2024
000007365 520__ $$aContext. Gravitational waves from black-hole (BH) merging events have revealed a population of extra-galactic BHs residing in short-period binaries with masses that are higher than expected based on most stellar evolution models - and also higher than known stellar-origin black holes in our Galaxy. It has been proposed that those high-mass BHs are the remnants of massive metal-poor stars. Aims: Gaia astrometry is expected to uncover many Galactic wide-binary systems containing dormant BHs, which may not have been detected before. The study of this population will provide new information on the BH-mass distribution in binaries and shed light on their formation mechanisms and progenitors. Methods: As part of the validation efforts in preparation for the fourth Gaia data release (DR4), we analysed the preliminary astrometric binary solutions, obtained by the Gaia Non-Single Star pipeline, to verify their significance and to minimise false-detection rates in high-mass-function orbital solutions. Results: The astrometric binary solution of one source, Gaia BH3, implies the presence of a 32.70 ± 0.82 M⊙ BH in a binary system with a period of 11.6 yr. Gaia radial velocities independently validate the astrometric orbit. Broad-band photometric and spectroscopic data show that the visible component is an old, very metal-poor giant of the Galactic halo, at a distance of 590 pc. Conclusions: The BH in the Gaia BH3 system is more massive than any other Galactic stellar-origin BH known thus far. The low metallicity of the star companion supports the scenario that metal-poor massive stars are progenitors of the high-mass BHs detected by gravitational-wave telescopes. The Galactic orbit of the system and its metallicity indicate that it might belong to the Sequoia halo substructure. Alternatively, and more plausibly, it could belong to the ED-2 stream, which likely originated from a globular cluster that had been disrupted by the Milky Way. 
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000007365 594__ $$aNO
000007365 6531_ $$aastrometry
000007365 6531_ $$abinaries: spectroscopic
000007365 6531_ $$astars: black holes
000007365 6531_ $$astars: evolution
000007365 6531_ $$astars: massive
000007365 6531_ $$astars: Population II
000007365 700__ $$aPanuzzo, P.
000007365 700__ $$aMazeh, T.
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000007365 700__ $$aHoll, B.
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000007365 700__ $$aJorissen, A.
000007365 700__ $$aBabusiaux, C.
000007365 700__ $$aGavras, P.
000007365 700__ $$aSahlmann, J.
000007365 700__ $$aBastian, U.
000007365 700__ $$aWyrzykowski, Ł.
000007365 700__ $$aEyer, L.
000007365 700__ $$aLeclerc, N.
000007365 700__ $$aBauchet, N.
000007365 700__ $$aBombrun, A.
000007365 700__ $$aMowlavi, N.
000007365 700__ $$aSeabroke, G. M.
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000007365 700__ $$aBalbinot, E.
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000007365 773__ $$cL2, 23 pp.$$pAstronomy & Astrophysics$$v686$$y2024
000007365 8560_ $$fronny.blomme@ksb-orb.be
000007365 85642 $$ahttps://www.aanda.org/articles/aa/full_html/2024/06/aa49763-24/aa49763-24.html
000007365 85642 $$ahttps://arxiv.org/abs/2404.10486
000007365 905__ $$apublished in
000007365 980__ $$aREFERD