binaries: general; binaries: spectroscopic; stars: early-type; stars: massive; supergiants; Binaries: spectroscopic; Binaries:general; Binarity; Binary fraction; Metallicities; Small magellanic clouds; Spectroscopic binary; Stars: massive; Stars:early type; Supergiant; Astronomy and Astrophysics; Space and Planetary Science; astro-ph.SR; astro-ph.GA
Abstract :
[en] Context. The blue supergiant (BSG) domain contains a large variety of stars whose past and future evolutionary paths are still highly uncertain. Since binary interaction plays a crucial role in the fate of massive stars, investigating the multiplicity among BSGs helps shed light on the fate of such objects. Aims. We aim to estimate the binary fraction of a large sample of BSGs in the Small Magellanic Cloud (SMC) within the Binarity at LOw Metallicity (BLOeM) survey. In total, we selected 262 targets with spectral types B0-B3 and luminosity classes I-II. Methods. This work is based on spectroscopic data collected by the flames instrument, mounted on the Very Large Telescope, which gathered nine epochs over three months. Our spectroscopic analysis for each target includes the individual and peak-to-peak radial velocity measurements, an investigation of the line profile variability, and a periodogram analysis to search for possible short- and long-period binaries. Results. By applying a 20 km s−1 threshold on the peak-to-peak radial velocities above which we would consider the star to be binary, the resulting observed spectroscopic binary fraction for our BSG sample is 23 ± 3%. An independent analysis of line profile variability reveals 11 (plus 5 candidates) double-lined spectroscopic binaries and 32 (plus 41 candidates) single-lined spectroscopic binaries. Based on these results, we estimated the overall observed binary fraction in this sample to be 34 ± 3%, which is close to the computed intrinsic binary fraction of 40 ± 4%. In addition, we derived reliable orbital periods for 41 spectroscopic binaries and potential binary candidates, among which there are 17 eclipsing binaries, including 20 SB1 and SB2 systems with periods of less than 10 days. We reported a significant drop in the binary fraction of BSGs with spectral types later than B2 and effective temperatures less than 18 kK, which could indicate the end of the main sequence phase in this temperature regime. We found no metallicity dependence in the binary fraction of BSGs, compared to existing spectroscopic surveys of the Galaxy and Large Magellanic Cloud.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Britavskiy, Mikola ; Université de Liège - ULiège > Département d'astrophysique, géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) ; ORB - Royal Observatory of Belgium
Mahy, L. ; Royal Observatory of Belgium, Brussels, Belgium
Lennon, D.J.; Instituto de Astrofísica de Canarias, La Laguna, Spain ; Universidad de La Laguna, Dpto. Astrofísica, La Laguna, Spain
Patrick, L.R. ; Centro de Astrobiología (CSIC-INTA), Torrejón de Ardoz, Spain
Sana, H.; Institute of Astronomy, KU Leuven, Leuven, Belgium
Villaseñor, J.I. ; Max-Planck-Institut für Astronomie, Heidelberg, Germany
Shenar, T. ; The School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel
Bodensteiner, J.; ESO – European Southern Observatory, Garching bei München, Germany
Bernini-Peron, M. ; Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Heidelberg, Germany
Berlanas, S.R. ; Instituto de Astrofísica de Canarias, La Laguna, Spain ; Universidad de La Laguna, Dpto. Astrofísica, La Laguna, Spain
Bowman, D.M. ; Institute of Astronomy, KU Leuven, Leuven, Belgium ; School of Mathematics, Statistics and Physics, Newcastle University, Newcastle upon Tyne, United Kingdom
Crowther, P.A. ; Department of Physics & Astronomy, University of Sheffield, Sheffield, United Kingdom
de Mink, S.E.; Max-Planck-Institute for Astrophysics, Garching, Germany
Evans, C.J. ; European Space Agency (ESA), ESA Office, Space Telescope Science Institute, Baltimore, United States
Götberg, Y. ; Institute of Science and Technology Austria (ISTA), Klosterneuburg, Austria
Holgado, G. ; Instituto de Astrofísica de Canarias, La Laguna, Spain ; Universidad de La Laguna, Dpto. Astrofísica, La Laguna, Spain
Johnston, C. ; Max-Planck-Institute for Astrophysics, Garching, Germany
Keszthelyi, Z.; Center for Computational Astrophysics, Division of Science, National Astronomical Observatory of Japan, Tokyo, Japan
Klencki, J.; ESO – European Southern Observatory, Garching bei München, Germany
Langer, N.; Argelander-Institut für Astronomie, Universität Bonn, Bonn, Germany
Mandel, I. ; School of Physics and Astronomy, Monash University, Clayton, Australia ; ARC Centre of Excellence for Gravitational-wave Discovery (OzGrav), Melbourne, Australia
Menon, A. ; Department of Astronomy, Pupin Hall, Columbia University, New York City, United States
Moe, M. ; Department of Physics and Astronomy, University of Wyoming, Laramie, United States
Oskinova, L.M. ; Institut für Physik und Astronomie, Universität Potsdam, Potsdam, Germany
Pauli, D. ; Institute of Astronomy, KU Leuven, Leuven, Belgium ; Institut für Physik und Astronomie, Universität Potsdam, Potsdam, Germany
Pawlak, M. ; Lund Observatory, Division of Astrophysics, Department of Physics, Lund University, Lund, Sweden
Ramachandran, V.; Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Heidelberg, Germany
Renzo, M. ; Department of Astronomy, Steward Observatory, Tucson, United States
Sander, A.A.C. ; Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Heidelberg, Germany
Schneider, F.R.N. ; Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Heidelberg, Germany ; Heidelberger Institut für Theoretische Studien, Heidelberg, Germany
Schootemeijer, A. ; Argelander-Institut für Astronomie, Universität Bonn, Bonn, Germany
Sen, K. ; Department of Astronomy, Steward Observatory, Tucson, United States ; Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Torun, Poland
Simón-Díaz, S. ; Instituto de Astrofísica de Canarias, La Laguna, Spain ; Universidad de La Laguna, Dpto. Astrofísica, La Laguna, Spain
van Loon, J.T. ; Lennard-Jones Laboratories, Keele University, Newcastle, United Kingdom
Vink, J.S. ; Armagh Observatory, Armagh, United Kingdom
We thank the anonymous referee for helpful comments that have improved the manuscript. This project has received funding from the European Research Council (ERC) under the European Union\u2019s Horizon 2020 research and innovation programme (grant agreement 101164755/METAL) and was supported by the Israel Science Foundation (ISF) under grant number 2434/24. NB acknowledges support from the Belgian federal government grant for Ukrainian postdoctoral researchers (contract UF/2022/10). TS acknowledges support by the Israel Science Foundation (ISF) under grant number 0603225041. DP acknowledges financial support from the Deutsches Zentrum f\u00FCr Luft und Raumfahrt (DLR) grant FKZ 50OR2005 and the FWO junior postdoctoral fellowship No. 1256225N. DMB gratefully acknowledges UK Research and Innovation (UKRI) in the form of a Frontier Research grant under the UK government\u2019s ERC Horizon Europe funding guarantee (SYMPHONY; PI Bowman; grant number: EP/Y031059/1), and a Royal Society University Research Fellowship (PI Bowman; grant number: URF\\R1\\231631). KS is funded by the National Science Center (NCN), Poland, under grant number OPUS 2021/41/B/ST9/00757. IM acknowledges support from the Australian Research Council (ARC) Centre of Excellence for Gravitational Wave Discovery (OzGav), through project number CE230100016. JIV acknowledges support from the European Research Council through ERC Advanced Grant No. 101054731. SS-D, and GH acknowledge support from the Spanish Ministry of Science and Innovation and Universities (MICIU) through the Spanish State Research Agency (AEI) through grants PID2021-122397NB-C21, and the Severo Ochoa Program 2020-2023 (CEX2019-000920-S).
Commentary :
18 pages, 14 figures, accepted for publication in Astronomy & Astrophysics
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