The Arches cluster revisited – IV. Observational constraints on the binary properties of very massive stars
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Title: | The Arches cluster revisited – IV. Observational constraints on the binary properties of very massive stars |
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Authors: | Clark, J. Simon | Lohr, Marcus E. | Najarro de la Parra, Francisco | Patrick, Lee R. | Ritchie, Ben W. |
Research Group/s: | Astrofísica Estelar (AE) |
Center, Department or Service: | Universidad de Alicante. Departamento de Física Aplicada |
Keywords: | Binaries: spectroscopic | Stars: massive | Stars: Wolf–Rayet |
Issue Date: | 10-Feb-2023 |
Publisher: | Oxford University Press |
Citation: | Monthly Notices of the Royal Astronomical Society. 2023, 521(3): 4473-4489. https://doi.org/10.1093/mnras/stad449 |
Abstract: | Serving as the progenitors of electromagnetic and gravitational-wave transients, massive stars have received renewed interest in recent years. However, many aspects of their birth and evolution remain opaque, particularly in the context of binary interactions. The centre of our Galaxy hosts a rich cohort of very massive stars, which appear to play a prominent role in the ecology of the region. In this paper, we investigate the binary properties of the Arches cluster, which is thought to host a large number of very massive stars. A combination of multi-epoch near-IR spectroscopy and photometry was utilized to identify binaries. 13 from 36 cluster members meet our criteria to be classed as RV variable. Combining the spectroscopic data with archival radio and X-ray observations – to detect colliding wind systems – provides a lower limit to the binary fraction of ∼43 per cent; increasing to ≳50 per cent for the O-type hypergiants and WNLha. Dynamical and evolutionary masses reveal the primaries to be uniformly massive (≳50M⊙). Where available, orbital analysis reveals a number of short period, highly eccentric binaries, which appear to be pre-interaction systems. Such systems are X-ray luminous, with 80 per cent above an empirical bound of (Lx/Lbol) ∼ 10−7 and their orbital configurations suggest formation and evolution via a single-star channel; however, we cannot exclude a binary formation channel for a subset. Qualitative comparison to surveys of lower mass OB-type stars confirms that the trend to an extreme binary fraction (≥60 per cent) extends to the most massive stars currently forming in the local Universe. |
Sponsor: | FN acknowledges funding by grants PID2019-105552RB-C41 and MDM-2017-0737-19-3 Unidad de Excelencia ‘María de Maeztu’. LRP acknowledges the support of the Generalitat Valenciana through the grant APOSTD/2020/247. This research is partially supported by the Spanish Government under grant PGC2018-093741-B-C21 (MICIU/AEI/FEDER, UE). |
URI: | http://hdl.handle.net/10045/134000 |
ISSN: | 0035-8711 (Print) | 1365-2966 (Online) |
DOI: | 10.1093/mnras/stad449 |
Language: | eng |
Type: | info:eu-repo/semantics/article |
Rights: | © 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society |
Peer Review: | si |
Publisher version: | https://doi.org/10.1093/mnras/stad449 |
Appears in Collections: | INV - Astrofísica Estelar - Artículos de Revistas |
Files in This Item:
File | Description | Size | Format | |
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Clark_etal_2023_MNRAS.pdf | 1,99 MB | Adobe PDF | Open Preview | |
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