000008061 001__ 8061
000008061 005__ 20260313093753.0
000008061 0247_ $$2DOI$$a10.1051/0004-6361/202554344
000008061 037__ $$aSCART-2026-0134
000008061 100__ $$aFrost, A. J.
000008061 245__ $$aAn interferometric study of B star multiplicity
000008061 260__ $$c2025
000008061 520__ $$aContext. Massive stars can have extreme effects on their environments from local to galactic scales. Their multiplicity can affect this influence by altering how they evolve over time by causing dynamical interactions, common-envelope evolution, mergers and more. While O star multiplicity has been studied over a broad separation range (to the point where absolute masses of these systems have been determined and investigations into multiple system formation and interactions have been performed), studies of B star multiplicity are lacking, even though they dominate the production of core-collapse supernovae and neutron stars. Aims. Using interferometry, we investigated the multiplicity of a statistically significant sample of B stars over a range of separations (∼0.5─35 au, given that the average distance to our sample is 412 pc). Methods. We analysed high angular resolution interferometric taken with the PIONIER (Precision Integrated-Optics Near-infrared Imaging ExpeRiment) instrument at the Very Large Telescope Interferometer (VLTI) for a sample of 32 B stars. Using parametric modelling of the closure phases and visibilities, we determined best-fitting models to each of the systems and investigated whether each source was best represented by a single star or a higher-order system. The detection limits were calculated for companions to determine whether they were significant. We then combined our findings from the interferometric data with results from a literature search to determine whether other companions were reported at different separation ranges. Results. Within the interferometric range 72 ± 8% of the B stars are resolved as multiple systems. The most common type of system are binary systems, followed by single stars, triple systems, and quadruple systems. The interferometric companion fraction derived for the sample is 1.88 ± 0.24. When we accounted for spectroscopic companions that have been confirmed in the literature and wide companions inferred from Gaia data in addition to the companions we found with interferometry, we obtain multiplicity and companion fractions of 0.88 ± 0.06 and 2.31 ± 0.27, respectively, for our sample. The number of triple systems increases significantly to the second-most populous system when we account for spectroscopic companions. This suggests that binarity and higher-order multiplicity are as integral to the evolution of B stars as they are for O stars. ⋆ Based on observations made with ESO Telescopes at the Paranal Observatory under programmes ID 093.C-0503(A) and 112.2624.
000008061 594__ $$aNO
000008061 700__ $$aSana, H.
000008061 700__ $$aLe Bouquin, J.-B.
000008061 700__ $$aPerets, H. B.
000008061 700__ $$aBodensteiner, J.
000008061 700__ $$aIgoshev, A. P.
000008061 700__ $$aBanyard, G.
000008061 700__ $$aMahy, L.
000008061 700__ $$aMérand, A.
000008061 700__ $$aRamírez-Agudelo, O. H.
000008061 773__ $$c15$$nA171$$pAstronomy & Astrophysics$$v701$$y2025
000008061 8560_ $$flaurent.mahy@ksb-orb.be
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000008061 905__ $$apublished in
000008061 980__ $$aREFERD