---
DOAJ_listed: '1'
OA_place: publisher
OA_type: diamond
PlanS_conform: '1'
_id: '21450'
abstract:
- lang: eng
text: Stellar wind mass loss of massive stars is often assumed to depend on their
metallicity Z. Therefore, evolutionary models predict that massive stars in lower-Z
environments are able to retain more of their hydrogen-rich layers and evolve
into brighter cool supergiants (cool SGs; Teff < 7 kK). Surprisingly, in galaxies
in the metallicity range 0.2 ≲ Z/Z⊙ ≲ 1.5, previous studies have not found a metallicity
dependence on the upper luminosity limit Lmax of cool SGs. Here, we add four galaxies
to the sample studied for this purpose with data from the Hubble Space Telescope
and the James Webb Space Telescope (JWST). Observations of the extremely metal-poor
dwarf galaxy I Zw 18 from JWST allow us to extend the studied metallicity range
down to Z/Z⊙ ≈ 1/40. For cool SGs in all studied galaxies, including I Zw 18,
we find a constant value of Lmax ≈ 105.6 L⊙, similar to literature results for
0.2 ≲ Z/Z⊙ ≲ 1.5. In I Zw 18 and the other studied galaxies, the presence of Wolf-Rayet
stars has been previously inferred. Although we cannot rule out that some of them
become intermediate-temperature objects, this paints a picture in which evolved
stars with L > 105.6 L⊙ burn helium as hot, helium-rich stars down to extremely
low metallicity. We argue that metallicity-independent late-phase mass loss would
be the most likely mechanism responsible for this. Regardless of the exact stripping
mechanism (winds or, for example, binary interaction), for the Early Universe
our results imply a limitation on black hole masses and a contribution of stars
born with M ≳ 30 M⊙ to its surprisingly strong nitrogen enrichment. We propose
a scenario in which single stars at low metallicity emit sufficiently hard ionizing
radiation to produce He II and C IV lines. In this scenario, late-phase metallicity-independent
mass loss produces hot, helium-rich stars. Due to the well-understood metallicity
dependence on the radiation-driven winds of hot stars, a window of opportunity
would open below 0.2 Z⊙, where self-stripped helium-rich stars can exist without
dense Wolf-Rayet winds that absorb hard ionizing radiation.
acknowledgement: "We thank our anonymous referee for carefully reading the manuscript
and providing a constructive report with helpful feedback. This work is based in
part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The
data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope
Science Institute, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations
are associated with program #1233. The specific observations analyzed can be accessed
via DOI: 10.17909/3c1d-6182. Moreover, this research is based in part on observations
made with the NASA/ESA Hubble Space Telescope obtained from the\r\nSpace Telescope
Science Institute, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated
with programs #13664, GO-10915, and DD-11307. This research was supported in part
by grant NSF PHY-2309135 to the Kavli Institute for Theoretical Physics (KITP).
LRP acknowledges support by grants PID2019-105552RB-C41 and PID2022-137779OB-C41
funded\r\nby MCIN/AEI/10.13039/501100011033 by “ERDF A way of making Europe”. LRP
acknowledges support from grant PID2022-140483NB-C22 funded by MCIN/AEI/10.13039/501100011033."
article_number: A116
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Abel
full_name: Schootemeijer, Abel
last_name: Schootemeijer
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: Norbert
full_name: Langer, Norbert
last_name: Langer
- first_name: Giacomo
full_name: Bortolini, Giacomo
last_name: Bortolini
- first_name: Alec S.
full_name: Hirschauer, Alec S.
last_name: Hirschauer
- first_name: Lee
full_name: Patrick, Lee
last_name: Patrick
citation:
ama: Schootemeijer A, Götberg YLL, Langer N, Bortolini G, Hirschauer AS, Patrick
L. A constant upper luminosity limit of cool supergiant stars down to the extremely
low metallicity of I Zw 18. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202557675
apa: Schootemeijer, A., Götberg, Y. L. L., Langer, N., Bortolini, G., Hirschauer,
A. S., & Patrick, L. (2026). A constant upper luminosity limit of cool supergiant
stars down to the extremely low metallicity of I Zw 18. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202557675
chicago: Schootemeijer, Abel, Ylva Louise Linsdotter Götberg, Norbert Langer, Giacomo
Bortolini, Alec S. Hirschauer, and Lee Patrick. “A Constant Upper Luminosity Limit
of Cool Supergiant Stars down to the Extremely Low Metallicity of I Zw 18.” Astronomy
& Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557675.
ieee: A. Schootemeijer, Y. L. L. Götberg, N. Langer, G. Bortolini, A. S. Hirschauer,
and L. Patrick, “A constant upper luminosity limit of cool supergiant stars down
to the extremely low metallicity of I Zw 18,” Astronomy & Astrophysics,
vol. 707. EDP Sciences, 2026.
ista: Schootemeijer A, Götberg YLL, Langer N, Bortolini G, Hirschauer AS, Patrick
L. 2026. A constant upper luminosity limit of cool supergiant stars down to the
extremely low metallicity of I Zw 18. Astronomy & Astrophysics. 707, A116.
mla: Schootemeijer, Abel, et al. “A Constant Upper Luminosity Limit of Cool Supergiant
Stars down to the Extremely Low Metallicity of I Zw 18.” Astronomy & Astrophysics,
vol. 707, A116, EDP Sciences, 2026, doi:10.1051/0004-6361/202557675.
short: A. Schootemeijer, Y.L.L. Götberg, N. Langer, G. Bortolini, A.S. Hirschauer,
L. Patrick, Astronomy & Astrophysics 707 (2026).
date_created: 2026-03-15T23:01:35Z
date_published: 2026-03-01T00:00:00Z
date_updated: 2026-03-16T09:07:55Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202557675
external_id:
arxiv:
- '2510.12594'
file:
- access_level: open_access
checksum: 02a0cd932340207c96fdd3059490ad29
content_type: application/pdf
creator: dernst
date_created: 2026-03-16T09:05:06Z
date_updated: 2026-03-16T09:05:06Z
file_id: '21455'
file_name: 2026_AstronomyAstrophysics_Schootemeijer.pdf
file_size: 2102107
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success: 1
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intvolume: ' 707'
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- iso: eng
month: '03'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: A constant upper luminosity limit of cool supergiant stars down to the extremely
low metallicity of I Zw 18
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 707
year: '2026'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '21714'
abstract:
- lang: eng
text: Be stars are rapidly rotating main-sequence stars that play a crucial role
in understanding stellar evolution and binary interactions. In this Letter, we
propose a new formation scenario for black hole (BH) + Be star binaries (hereafter
BHBe binaries), where the Be star is produced through the wind Roche lobe overflow
(WRLOF) mechanism. Our analysis is based on numerical simulations of the WRLOF
process in massive binaries, building on recent theoretical work. We demonstrate
that the WRLOF model can efficiently form BHBe binaries under reasonable assumptions
on stellar wind velocities. Using rapid binary population synthesis, we estimate
the population of such systems in the Milky Way, predicting ∼1800−3200 currently
existing BHBe binaries originating from the WRLOF channel. These systems are characterized
by high eccentricities and exceptionally wide orbits, with typical orbital periods
exceeding 1000 days and a peak distribution around ∼10,000 days. Due to their
long orbital separations, these BHBe binaries are promising targets for future
detection via astrometric and interferometric observations.
acknowledgement: We are deeply grateful to the anonymous referee for the insightful
comments, which have significantly improved the quality of this work. The authors
express their gratitude to Zhaoyu Zuo and I. El Mellah for sharing the grids of
wind accretion efficiencies. Z.L. thanks Matthias U. Kruckow for detailed discussions
about the BH formation. This work is supported by the Natural Science Foundation
of China (grant Nos. 12125303, 12525304, 12288102, 12090040/3, 12473034, 12503044,
12333008, 12433009, 12422305, 12273105, 12073070, 12173081), the Strategic Priority
Research Program of the Chinese Academy of Sciences (grant Nos. XDB1160303, XDB1160201,
XDB1160000), the National Key R&D Program of China (grant Nos. 2021YFA1600403 and
2021YFA1600400), the CAS “Light of West China,” the Yunnan Revitalization Talent
Support Program-Science & Technology Champion Project (No. 202305AB350003) and Young
Talent project, the International Centre of Supernovae (ICESUN), Yunnan Key Laboratory
of Supernova Research (Nos. 202302AN360001 and 202201BC070003), Yunnan Fundamental
Research Projects (No. 202401AT070139), and the Natural Science Foundation of Henan
Province (No. 242300420944). X.C. acknowledges the New Cornerstone Science Foundation
through the XPLORER PRIZE. The authors gratefully acknowledge the “PHOENIX Supercomputing
Platform” jointly operated by the Binary Population Synthesis Group and the Stellar
Astrophysics Group at Yunnan Observatories, Chinese Academy of Sciences.
article_number: L42
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Zhenwei
full_name: Li, Zhenwei
last_name: Li
- first_name: Shi
full_name: Jia, Shi
last_name: Jia
- first_name: Dandan
full_name: Wei, Dandan
id: 5dd129bd-0601-11ef-b325-833284687b76
last_name: Wei
- first_name: Hongwei
full_name: Ge, Hongwei
last_name: Ge
- first_name: Hailiang
full_name: Chen, Hailiang
last_name: Chen
- first_name: Yangyang
full_name: Zhang, Yangyang
last_name: Zhang
- first_name: Xuefei
full_name: Chen, Xuefei
last_name: Chen
- first_name: Zhanwen
full_name: Han, Zhanwen
last_name: Han
citation:
ama: 'Li Z, Jia S, Wei D, et al. Formation of Be stars via wind accretion: Case
study on Black Hole + Be star binaries. The Astrophysical Journal Letters.
2026;996(2). doi:10.3847/2041-8213/ae3008'
apa: 'Li, Z., Jia, S., Wei, D., Ge, H., Chen, H., Zhang, Y., … Han, Z. (2026). Formation
of Be stars via wind accretion: Case study on Black Hole + Be star binaries. The
Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae3008'
chicago: 'Li, Zhenwei, Shi Jia, Dandan Wei, Hongwei Ge, Hailiang Chen, Yangyang
Zhang, Xuefei Chen, and Zhanwen Han. “Formation of Be Stars via Wind Accretion:
Case Study on Black Hole + Be Star Binaries.” The Astrophysical Journal Letters.
IOP Publishing, 2026. https://doi.org/10.3847/2041-8213/ae3008.'
ieee: 'Z. Li et al., “Formation of Be stars via wind accretion: Case study
on Black Hole + Be star binaries,” The Astrophysical Journal Letters, vol.
996, no. 2. IOP Publishing, 2026.'
ista: 'Li Z, Jia S, Wei D, Ge H, Chen H, Zhang Y, Chen X, Han Z. 2026. Formation
of Be stars via wind accretion: Case study on Black Hole + Be star binaries. The
Astrophysical Journal Letters. 996(2), L42.'
mla: 'Li, Zhenwei, et al. “Formation of Be Stars via Wind Accretion: Case Study
on Black Hole + Be Star Binaries.” The Astrophysical Journal Letters, vol.
996, no. 2, L42, IOP Publishing, 2026, doi:10.3847/2041-8213/ae3008.'
short: Z. Li, S. Jia, D. Wei, H. Ge, H. Chen, Y. Zhang, X. Chen, Z. Han, The Astrophysical
Journal Letters 996 (2026).
date_created: 2026-04-12T22:01:50Z
date_published: 2026-01-10T00:00:00Z
date_updated: 2026-04-16T06:26:18Z
day: '10'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.3847/2041-8213/ae3008
external_id:
arxiv:
- '2512.18565'
file:
- access_level: open_access
checksum: 09200c1cf405101abdd298ce80c9a90d
content_type: application/pdf
creator: dernst
date_created: 2026-04-16T06:24:30Z
date_updated: 2026-04-16T06:24:30Z
file_id: '21741'
file_name: 2026_AstrophysicalJourLetters_Li.pdf
file_size: 5202345
relation: main_file
success: 1
file_date_updated: 2026-04-16T06:24:30Z
has_accepted_license: '1'
intvolume: ' 996'
issue: '2'
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Formation of Be stars via wind accretion: Case study on Black Hole + Be star
binaries'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 996
year: '2026'
...
---
OA_place: publisher
OA_type: diamond
_id: '19797'
abstract:
- lang: eng
text: Stars stripped of their hydrogen-rich envelopes through binary interaction
are thought to be responsible for both hydrogen-poor supernovae and the hard ionizing
radiation observed in low-Z galaxies. A population of these stars was recently
observed for the first time, but their prevalence remains unknown. In preparation
for such measurements, we estimate the mass distribution of hot, stripped stars
using a population synthesis code that interpolates over detailed single and binary
stellar evolution tracks. We predict that for a constant star formation rate of
1 M⊙/yr and regardless of metallicity, a scalable model population contains ∼30
000 stripped stars with mass Mstrip > 1 M⊙ and ∼4000 stripped stars that are sufficiently
massive to explode (Mstrip > 2.6 M⊙). Below Mstrip = 5 M⊙, the distribution is
metallicity-independent and can be described by a power law with the exponent
α ∼ −2. At higher masses and lower metallicity (Z ≲ 0.002), the mass distribution
exhibits a drop. This originates from the prediction, frequently seen in evolutionary
models, that massive low-metallicity stars do not expand substantially until central
helium burning or later and therefore cannot form long-lived stripped stars. With
weaker line-driven winds at low metallicity, this suggests that neither binary
interaction nor wind mass loss can efficiently strip massive stars at low metallicity.
As a result, a “helium-star desert” emerges around Mstrip = 15 M⊙ at Z = 0.002,
covering an increasingly large mass range with decreasing metallicity. We note
that these high-mass stars are those that potentially boost a galaxy’s He+-ionizing
radiation and that participate in the formation of merging black holes. This “helium-star
desert” therefore merits further study.
acknowledgement: We thank the anonymous referee for providing a constructive report.
We thank Tomer Shenar and Selma de Mink for the interesting discussions that helped
us improve the content of Sect. 4. Thank you to Jorick Vink and Andreas Sander for
helpful discussions about wind driving. BHA thanks the Caltech Summer Undergraduate
Research Fellowship (SURF) program and Peter Adams for supporting this project in
memory of Alain Porter and Arthur R. Adams. BHA thanks Gwen Rudie for organizing
the Carnegie Astrophysics Summer Student Internship (CASSI) program and all the
staff at Carnegie Observatories who help to support this program. BHA also thanks
Laura Jaliff, Sal Wanying Fu, Ivanna Escala, Johanna Teske, Tony Piro, Brian Lorenz,
and Peter Senchyna for their mentorship during this project. Computing resources
used for this work were made possible by a grant from the Ahmanson Foundation. We
thank the Observatories of the Carnegie Institution for Science for support, including
Chris Burns for help with computations. This work used computing resources provided
by Northwestern University and the Center for Interdisciplinary Exploration and
Research in Astrophysics (CIERA). This research was supported in part through the
computational resources and staff contributions provided for the Quest high performance
computing facility at Northwestern University which is jointly supported by the
Office of the Provost, the Office for Research, and Northwestern University Information
Technology. MRD acknowledges support from the NSERC through grant RGPIN-2019-06186,
the Canada Research Chairs Program, and the Dunlap Institute at the University of
Toronto. BHA is supported by the National Science Foundation Graduate Research Fellowship
under Grant No. DGE-2234667.
article_number: A239
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: B.
full_name: Hovis-Afflerbach, B.
last_name: Hovis-Afflerbach
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: J.
full_name: Klencki, J.
last_name: Klencki
- first_name: A. L.
full_name: Strom, A. L.
last_name: Strom
- first_name: B. A.
full_name: Ludwig, B. A.
last_name: Ludwig
- first_name: M. R.
full_name: Drout, M. R.
last_name: Drout
citation:
ama: 'Hovis-Afflerbach B, Götberg YLL, Schootemeijer A, et al. The mass distribution
of stars stripped in binaries: The effect of metallicity. Astronomy & Astrophysics.
2025;697. doi:10.1051/0004-6361/202453185'
apa: 'Hovis-Afflerbach, B., Götberg, Y. L. L., Schootemeijer, A., Klencki, J., Strom,
A. L., Ludwig, B. A., & Drout, M. R. (2025). The mass distribution of stars
stripped in binaries: The effect of metallicity. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202453185'
chicago: 'Hovis-Afflerbach, B., Ylva Louise Linsdotter Götberg, A. Schootemeijer,
J. Klencki, A. L. Strom, B. A. Ludwig, and M. R. Drout. “The Mass Distribution
of Stars Stripped in Binaries: The Effect of Metallicity.” Astronomy &
Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202453185.'
ieee: 'B. Hovis-Afflerbach et al., “The mass distribution of stars stripped
in binaries: The effect of metallicity,” Astronomy & Astrophysics,
vol. 697. EDP Sciences, 2025.'
ista: 'Hovis-Afflerbach B, Götberg YLL, Schootemeijer A, Klencki J, Strom AL, Ludwig
BA, Drout MR. 2025. The mass distribution of stars stripped in binaries: The effect
of metallicity. Astronomy & Astrophysics. 697, A239.'
mla: 'Hovis-Afflerbach, B., et al. “The Mass Distribution of Stars Stripped in Binaries:
The Effect of Metallicity.” Astronomy & Astrophysics, vol. 697, A239,
EDP Sciences, 2025, doi:10.1051/0004-6361/202453185.'
short: B. Hovis-Afflerbach, Y.L.L. Götberg, A. Schootemeijer, J. Klencki, A.L. Strom,
B.A. Ludwig, M.R. Drout, Astronomy & Astrophysics 697 (2025).
corr_author: '1'
date_created: 2025-06-08T22:01:22Z
date_published: 2025-05-01T00:00:00Z
date_updated: 2026-02-16T12:10:11Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202453185
external_id:
arxiv:
- '2412.05356'
isi:
- '001494033100007'
file:
- access_level: open_access
checksum: caa92beb22ab3146a75c5b03e926de1f
content_type: application/pdf
creator: dernst
date_created: 2025-06-10T07:00:38Z
date_updated: 2025-06-10T07:00:38Z
file_id: '19799'
file_name: 2025_AstronomyAstrophysics_HovisAfflerbach.pdf
file_size: 6378030
relation: main_file
success: 1
file_date_updated: 2025-06-10T07:00:38Z
has_accepted_license: '1'
intvolume: ' 697'
isi: 1
language:
- iso: eng
month: '05'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The mass distribution of stars stripped in binaries: The effect of metallicity'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 697
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19841'
abstract:
- lang: eng
text: "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.\r\nAims.
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.\r\n\r\nMethods. 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.\r\n\r\nResults. 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."
acknowledgement: '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’s 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 für 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’s 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).'
article_number: A40
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: N.
full_name: Britavskiy, N.
last_name: Britavskiy
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- first_name: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: J. I.
full_name: Villaseñor, J. I.
last_name: Villaseñor
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: M.
full_name: Bernini-Peron, M.
last_name: Bernini-Peron
- first_name: S. R.
full_name: Berlanas, S. R.
last_name: Berlanas
- first_name: D. M.
full_name: Bowman, D. M.
last_name: Bowman
- first_name: P. A.
full_name: Crowther, P. A.
last_name: Crowther
- first_name: S. E.
full_name: De Mink, S. E.
last_name: De Mink
- first_name: C. J.
full_name: Evans, C. J.
last_name: Evans
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: G.
full_name: Holgado, G.
last_name: Holgado
- first_name: C.
full_name: Johnston, C.
last_name: Johnston
- first_name: Z.
full_name: Keszthelyi, Z.
last_name: Keszthelyi
- first_name: J.
full_name: Klencki, J.
last_name: Klencki
- first_name: N.
full_name: Langer, N.
last_name: Langer
- first_name: I.
full_name: Mandel, I.
last_name: Mandel
- first_name: A.
full_name: Menon, A.
last_name: Menon
- first_name: M.
full_name: Moe, M.
last_name: Moe
- first_name: L. M.
full_name: Oskinova, L. M.
last_name: Oskinova
- first_name: D.
full_name: Pauli, D.
last_name: Pauli
- first_name: M.
full_name: Pawlak, M.
last_name: Pawlak
- first_name: V.
full_name: Ramachandran, V.
last_name: Ramachandran
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: A. A.C.
full_name: Sander, A. A.C.
last_name: Sander
- first_name: F. R.N.
full_name: Schneider, F. R.N.
last_name: Schneider
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: K.
full_name: Sen, K.
last_name: Sen
- first_name: S.
full_name: Simón-Díaz, S.
last_name: Simón-Díaz
- first_name: J. T.
full_name: Van Loon, J. T.
last_name: Van Loon
- first_name: J. S.
full_name: Vink, J. S.
last_name: Vink
citation:
ama: 'Britavskiy N, Mahy L, Lennon DJ, et al. Binarity at LOw Metallicity (BLOeM):
Multiplicity of early B-type supergiants in the Small Magellanic Cloud. Astronomy
& Astrophysics. 2025;698. doi:10.1051/0004-6361/202452963'
apa: 'Britavskiy, N., Mahy, L., Lennon, D. J., Patrick, L. R., Sana, H., Villaseñor,
J. I., … Vink, J. S. (2025). Binarity at LOw Metallicity (BLOeM): Multiplicity
of early B-type supergiants in the Small Magellanic Cloud. Astronomy &
Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202452963'
chicago: 'Britavskiy, N., L. Mahy, D. J. Lennon, L. R. Patrick, H. Sana, J. I. Villaseñor,
T. Shenar, et al. “Binarity at LOw Metallicity (BLOeM): Multiplicity of Early
B-Type Supergiants in the Small Magellanic Cloud.” Astronomy & Astrophysics.
EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452963.'
ieee: 'N. Britavskiy et al., “Binarity at LOw Metallicity (BLOeM): Multiplicity
of early B-type supergiants in the Small Magellanic Cloud,” Astronomy &
Astrophysics, vol. 698. EDP Sciences, 2025.'
ista: 'Britavskiy N, Mahy L, Lennon DJ, Patrick LR, Sana H, Villaseñor JI, Shenar
T, Bodensteiner J, Bernini-Peron M, Berlanas SR, Bowman DM, Crowther PA, De Mink
SE, Evans CJ, Götberg YLL, Holgado G, Johnston C, Keszthelyi Z, Klencki J, Langer
N, Mandel I, Menon A, Moe M, Oskinova LM, Pauli D, Pawlak M, Ramachandran V, Renzo
M, Sander AAC, Schneider FRN, Schootemeijer A, Sen K, Simón-Díaz S, Van Loon JT,
Vink JS. 2025. Binarity at LOw Metallicity (BLOeM): Multiplicity of early B-type
supergiants in the Small Magellanic Cloud. Astronomy & Astrophysics. 698,
A40.'
mla: 'Britavskiy, N., et al. “Binarity at LOw Metallicity (BLOeM): Multiplicity
of Early B-Type Supergiants in the Small Magellanic Cloud.” Astronomy &
Astrophysics, vol. 698, A40, EDP Sciences, 2025, doi:10.1051/0004-6361/202452963.'
short: N. Britavskiy, L. Mahy, D.J. Lennon, L.R. Patrick, H. Sana, J.I. Villaseñor,
T. Shenar, J. Bodensteiner, M. Bernini-Peron, S.R. Berlanas, D.M. Bowman, P.A.
Crowther, S.E. De Mink, C.J. Evans, Y.L.L. Götberg, G. Holgado, C. Johnston, Z.
Keszthelyi, J. Klencki, N. Langer, I. Mandel, A. Menon, M. Moe, L.M. Oskinova,
D. Pauli, M. Pawlak, V. Ramachandran, M. Renzo, A.A.C. Sander, F.R.N. Schneider,
A. Schootemeijer, K. Sen, S. Simón-Díaz, J.T. Van Loon, J.S. Vink, Astronomy &
Astrophysics 698 (2025).
date_created: 2025-06-15T22:01:29Z
date_published: 2025-06-01T00:00:00Z
date_updated: 2026-02-16T12:09:34Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202452963
external_id:
arxiv:
- '2502.12239'
isi:
- '001497903100019'
file:
- access_level: open_access
checksum: 53a9f290cb1f468895e0d4446e0020f0
content_type: application/pdf
creator: dernst
date_created: 2025-06-25T08:38:02Z
date_updated: 2025-06-25T08:38:02Z
file_id: '19901'
file_name: 2025_AstronomyAstrophysics_Britavskiy.pdf
file_size: 7106568
relation: main_file
success: 1
file_date_updated: 2025-06-25T08:38:02Z
has_accepted_license: '1'
intvolume: ' 698'
isi: 1
language:
- iso: eng
month: '06'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Binarity at LOw Metallicity (BLOeM): Multiplicity of early B-type supergiants
in the Small Magellanic Cloud'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 698
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19842'
abstract:
- lang: eng
text: Given the uncertain evolutionary status of blue supergiant stars, their multiplicity
properties hold vital clues to better understand their origin and evolution. As
part of The Binarity at LOw Metallicity (BLOeM) campaign in the Small Magellanic
Cloud, we present a multi-epoch spectroscopic survey of 128 supergiant stars of
spectral type B5–F5, which roughly correspond to initial masses in the 6–30 M⊙
range. The observed binary fraction for the B5–9 supergiants is 25 ± 6% (10 ±
4%) and 5 ± 2% (0%) for the A–F stars, which were found using a radial-velocity
(RV) variability threshold of 5 km s−1 (10 km s−1) as a criterion for binarity.
Accounting for observational biases, we find an intrinsic multiplicity fraction
of less than 18% for the B5–9 stars and 8−7+9% for the AF stars, for the orbital
periods up to 103.5 days and mass ratios (q) in the 0.1 < q < 1 range. The large
stellar radii of these supergiant stars prevent short orbital periods, but we
demonstrate that this effect alone cannot explain our results. We assessed the
spectra and RV time series of the detected binary systems and find that only a
small fraction display convincing solutions. We conclude that the multiplicity
fractions are compromised by intrinsic stellar variability, such that the true
multiplicity fraction may be significantly smaller. Our main conclusions from
comparing the multiplicity properties of the B5–9- and AF-type supergiants to
that of their less evolved counterparts is that such stars cannot be explained
by a direct evolution from the main sequence. Furthermore, by comparing their
multiplicity properties to red supergiant stars, we conclude that the AF supergiant
stars are neither progenitors nor descendants of red supergiants.
acknowledgement: 'We thank Sipra Hota for kindly sharing the SMC UVIT catalogue prior
to publication. LRP, FN. and FT acknowledge support by grants PID2019-105552RB-C41
and PID2022-137779OB-C41 funded by MCIN/AEI/10.13039/501100011033 by “ERDF A way
of making Europe”. LRP acknowledges support from grant PID2022-140483NB-C22 funded
by MCIN/AEI/10.13039/501100011033. TS acknowledges support by the Israel Science
Foundation (ISF) under grant number 0603225041. The research leading to these results
has received funding from the European Research Council (ERC) under the European
Union’s Horizon 2020 research and innovation programme (grant agreement numbers
772225: MULTIPLES). DMB gratefully acknowledges support from UK Research and Innovation
(UKRI) in the form of a Frontier Research grant under the UK government’s ERC Horizon
Europe funding guarantee (SYMPHONY; grant number: EP/Y031059/1), and a Royal Society
University Research Fellowship (grant number: URF\R1\231631). GGT is supported by
the German Deutsche Forschungsgemeinschaft (DFG) under Project-ID 496854903 (SA4064/2-1,
PI Sander). AACS is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research
Foundation) in the form of an Emmy Noether Research Group – Project-ID 445674056
(SA4064/1-1, PI Sander). GGT and AACS further acknowledges support from the Federal
Ministry of Education and Research (BMBF) and the Baden-Württemberg Ministry of
Science as part of the Excellence Strategy of the German Federal and State Governments.
This paper benefited from discussions at the International Space Science Institute
(ISSI) in Bern through ISSI International Team project 512 (Multiwavelength View
on Massive Stars in the Era of Multimessenger Astronomy). DP acknowledges financial
support by the Deutsches Zentrum für Luft und Raumfahrt (DLR) grant FKZ 50OR2005.
JIV acknowledges support from the European Research Council for the ERC Advanced
Grant 101054731. PAC is supported by the Science and Technology Facilities Council
research grant ST/V000853/1 (PI. V. Dhillon). JSV is supported by Science and Technology
Facilities Council funding under grant number ST/V000233/1. DFR is thankful for
the support of the CAPES-Br and FAPERJ/DSC-10 (SEI-260003/001630/2023). This work
has received funding from the European Research Council (ERC) under the European
Union’s Horizon 2020 research and innovation programme (Grant agreement No. 945806)
and is supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)
under Germany’s Excellence Strategy EXC 2181/1-390900948 (the Heidelberg STRUCTURES
Excellence Cluster).'
article_number: A39
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- first_name: F.
full_name: Najarro, F.
last_name: Najarro
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: P. A.
full_name: Crowther, P. A.
last_name: Crowther
- first_name: N.
full_name: Britavskiy, N.
last_name: Britavskiy
- first_name: N.
full_name: Langer, N.
last_name: Langer
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: C. J.
full_name: Evans, C. J.
last_name: Evans
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: S. E.
full_name: De Mink, S. E.
last_name: De Mink
- first_name: F. R.N.
full_name: Schneider, F. R.N.
last_name: Schneider
- first_name: A. J.G.
full_name: O’Grady, A. J.G.
last_name: O’Grady
- first_name: J. I.
full_name: Villaseñor, J. I.
last_name: Villaseñor
- first_name: M.
full_name: Bernini-Peron, M.
last_name: Bernini-Peron
- first_name: D. M.
full_name: Bowman, D. M.
last_name: Bowman
- first_name: A.
full_name: De Koter, A.
last_name: De Koter
- first_name: K.
full_name: Deshmukh, K.
last_name: Deshmukh
- first_name: A.
full_name: Gilkis, A.
last_name: Gilkis
- first_name: G.
full_name: González-Torà, G.
last_name: González-Torà
- first_name: V. M.
full_name: Kalari, V. M.
last_name: Kalari
- first_name: Z.
full_name: K̃Eszthelyi, Z.
last_name: K̃Eszthelyi
- first_name: I.
full_name: Mandel, I.
last_name: Mandel
- first_name: A.
full_name: Menon, A.
last_name: Menon
- first_name: M.
full_name: Moe, M.
last_name: Moe
- first_name: L. M.
full_name: Oskinova, L. M.
last_name: Oskinova
- first_name: D.
full_name: Pauli, D.
last_name: Pauli
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: A. A.C.
full_name: Sander, A. A.C.
last_name: Sander
- first_name: K.
full_name: Sen, K.
last_name: Sen
- first_name: M.
full_name: Stoop, M.
last_name: Stoop
- first_name: J. T.
full_name: Van Loon, J. T.
last_name: Van Loon
- first_name: S.
full_name: Toonen, S.
last_name: Toonen
- first_name: F.
full_name: Tramper, F.
last_name: Tramper
- first_name: J. S.
full_name: Vink, J. S.
last_name: Vink
- first_name: C.
full_name: Wang, C.
last_name: Wang
citation:
ama: 'Patrick LR, Lennon DJ, Najarro F, et al. Binarity at LOw Metallicity (BLOeM):
The multiplicity properties and evolution of BAF-type supergiants. Astronomy
& Astrophysics. 2025;698. doi:10.1051/0004-6361/202452949'
apa: 'Patrick, L. R., Lennon, D. J., Najarro, F., Shenar, T., Bodensteiner, J.,
Sana, H., … Wang, C. (2025). Binarity at LOw Metallicity (BLOeM): The multiplicity
properties and evolution of BAF-type supergiants. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202452949'
chicago: 'Patrick, L. R., D. J. Lennon, F. Najarro, T. Shenar, J. Bodensteiner,
H. Sana, P. A. Crowther, et al. “Binarity at LOw Metallicity (BLOeM): The Multiplicity
Properties and Evolution of BAF-Type Supergiants.” Astronomy & Astrophysics.
EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452949.'
ieee: 'L. R. Patrick et al., “Binarity at LOw Metallicity (BLOeM): The multiplicity
properties and evolution of BAF-type supergiants,” Astronomy & Astrophysics,
vol. 698. EDP Sciences, 2025.'
ista: 'Patrick LR, Lennon DJ, Najarro F, Shenar T, Bodensteiner J, Sana H, Crowther
PA, Britavskiy N, Langer N, Schootemeijer A, Evans CJ, Mahy L, Götberg YLL, De
Mink SE, Schneider FRN, O’Grady AJG, Villaseñor JI, Bernini-Peron M, Bowman DM,
De Koter A, Deshmukh K, Gilkis A, González-Torà G, Kalari VM, K̃Eszthelyi Z, Mandel
I, Menon A, Moe M, Oskinova LM, Pauli D, Renzo M, Sander AAC, Sen K, Stoop M,
Van Loon JT, Toonen S, Tramper F, Vink JS, Wang C. 2025. Binarity at LOw Metallicity
(BLOeM): The multiplicity properties and evolution of BAF-type supergiants. Astronomy
& Astrophysics. 698, A39.'
mla: 'Patrick, L. R., et al. “Binarity at LOw Metallicity (BLOeM): The Multiplicity
Properties and Evolution of BAF-Type Supergiants.” Astronomy & Astrophysics,
vol. 698, A39, EDP Sciences, 2025, doi:10.1051/0004-6361/202452949.'
short: L.R. Patrick, D.J. Lennon, F. Najarro, T. Shenar, J. Bodensteiner, H. Sana,
P.A. Crowther, N. Britavskiy, N. Langer, A. Schootemeijer, C.J. Evans, L. Mahy,
Y.L.L. Götberg, S.E. De Mink, F.R.N. Schneider, A.J.G. O’Grady, J.I. Villaseñor,
M. Bernini-Peron, D.M. Bowman, A. De Koter, K. Deshmukh, A. Gilkis, G. González-Torà,
V.M. Kalari, Z. K̃Eszthelyi, I. Mandel, A. Menon, M. Moe, L.M. Oskinova, D. Pauli,
M. Renzo, A.A.C. Sander, K. Sen, M. Stoop, J.T. Van Loon, S. Toonen, F. Tramper,
J.S. Vink, C. Wang, Astronomy & Astrophysics 698 (2025).
date_created: 2025-06-15T22:01:29Z
date_published: 2025-06-01T00:00:00Z
date_updated: 2026-02-16T12:09:50Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202452949
external_id:
arxiv:
- '2502.02644'
isi:
- '001497903100028'
file:
- access_level: open_access
checksum: 93a907bf48da7e2ba7d75b53ea6011f5
content_type: application/pdf
creator: dernst
date_created: 2025-06-23T07:09:38Z
date_updated: 2025-06-23T07:09:38Z
file_id: '19863'
file_name: 2025_AstronomyAstrophysics_Patrick.pdf
file_size: 2130448
relation: main_file
success: 1
file_date_updated: 2025-06-23T07:09:38Z
has_accepted_license: '1'
intvolume: ' 698'
isi: 1
language:
- iso: eng
month: '06'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Binarity at LOw Metallicity (BLOeM): The multiplicity properties and evolution
of BAF-type supergiants'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 698
year: '2025'
...
---
OA_place: repository
OA_type: green
_id: '20352'
abstract:
- lang: eng
text: "At high metallicity, a majority of massive stars have at least one close
stellar companion. The evolution of such binaries is subject to strong interaction
processes, which heavily impact the characteristics of their life-ending supernova
and compact remnants. For the low-metallicity environments of high-redshift galaxies,
constraints on the multiplicity properties of massive stars over the separation
range leading to binary interaction are crucially missing. Here we show that the
presence of massive stars in close binaries is ubiquitous, even at low metallicity.
Using the Very Large Telescope, we obtained multi-epoch radial velocity measurements
of a representative sample of 139 massive O-type stars across the Small Magellanic
Cloud, which has a metal content of about one-fifth of the solar value. We find
that 45% of them show radial velocity variations that demonstrate that they are
members of close binary systems, and predominantly have orbital periods shorter
than 1 year. Correcting for observational biases indicates that at least 70+11−6
% of the O stars in our sample are in close binaries, and that at least 68+7\r\n−8%
of all O stars interact with a companion star during their lifetime. We found
no evidence supporting a statistically significant trend of the multiplicity properties
with metallicity. Our results indicate that multiplicity and binary interactions
govern the evolution of massive stars and determine their cosmic feedback and
explosive fates."
acknowledgement: 'Based on data collected at the European Southern Observatory (ESO)
under programme ID 112.25R7. The research leading to these results has received
funding from the European Research Council (ERC) under the European Union’s Horizon
2020 and Horizon Europe research and innovation programme (grant agreement numbers
772225: MULTIPLES, 772086: ASSESS and 945806: TEL-STARS, ADG101054731: Stellar-BHs-SDSS-V,
and 101164755: METAL). This research was supported by the Israel Science Foundation
(ISF) under grant number 0603225041. We acknowledge support from the Science and
Technology Facilities Council (research grant ST/V000853/1 and ST/V000233/1), UK
Research and Innovation (UKRI) and the UK government’s ERC Horizon Europe funding
guarantee (grant number EP/Y031059/1), a Royal Society University Research Fellowship
(grant number URF\R1\231631), a Royal Society–Science Foundation Ireland University
Research Fellowship, the German Deutsche Forschungsgemeinschaft (Project-ID 496854903,
445674056 and 443790621, Germany’s Excellence Strategy EXC 2181/1-390900948), the
Klaus Tschira Foundation, the JSPS Kakenhi Grant-in-Aid for Scientific Research
(23K19071) and international fellowships (at the Graduate school of Science, Tokyo
University), the Australian Research Council (ARC) Centre of Excellence for Gravitational
Wave Discovery (OzGrav; project number CE230100016), the Deutsches Zentrum für Luft
und Raumfahrt (DLR) grants FKZ 50OR2005 and 50OR2306, Agencia Española de Investigación
(AEI) of the Spanish Ministerio de Ciencia Innovación y Universidades (MICIU) and
the European Regional Development Fund, FEDER and Severo Ochoa Programme (grants
PID2021-122397NB-C21 and CEX2019-000920-S), the NextGeneration EU/PRTR and MIU (UNI/551/2021)
trough grant Margarita Salas-UL, the CAPES-Br and FAPERJ/DSC-10 (SEI-260003/001630/2023),
MCIN/AEI/10.13039/501100011033 by ‘ERDF A way of making Europe’ (grants PID2019-105552RB-C41
and PID2022-137779OB-C41, PID2021-125485NB-C22, CEX2019-000918-M) funded by MCIN/AEI/10.13039/501100011033
(State Agency for Research of the Spanish Ministry of Science and Innovation) and
SGR-2021-01069 (AGAUR), the Spanish Government Ministerio de Ciencia e Innovación
and Agencia Estatal de Investigación (10.13 039/501 100 011 033; grant PID2022-136
640 NB-C22), the Consejo Superior de Investigaciones Científicas (CSIC; grant 2022-AEP
005), the Polish National Agency for Academic Exchange (BEKKER fellowship BPN/BEK/2022/1/00106)
and National Science Center (NCN, Poland; grant number OPUS 2021/41/B/ST9/00757),
the ‘La Caixa’ Foundation (ID 100010434) under the fellowship code LCF/BQ/PI23/11970035,
the Research foundation Flanders (FWO) PhD fellowship under project 11E1721N and
senior postdoctoral fellowship under number 12ZY523N, and the Netherlands Research
Council NWO (VIDI 203.061 grant).'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: N.
full_name: Britavskiy, N.
last_name: Britavskiy
- first_name: N.
full_name: Langer, N.
last_name: Langer
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: I.
full_name: Mandel, I.
last_name: Mandel
- first_name: S. E.
full_name: De Mink, S. E.
last_name: De Mink
- first_name: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- first_name: J. I.
full_name: Villaseñor, J. I.
last_name: Villaseñor
- first_name: M.
full_name: Dirickx, M.
last_name: Dirickx
- first_name: M.
full_name: Abdul-Masih, M.
last_name: Abdul-Masih
- first_name: L. A.
full_name: Almeida, L. A.
last_name: Almeida
- first_name: F.
full_name: Backs, F.
last_name: Backs
- first_name: S. R.
full_name: Berlanas, S. R.
last_name: Berlanas
- first_name: M.
full_name: Bernini-Peron, M.
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full_name: Bowman, D. M.
last_name: Bowman
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full_name: Crowther, P. A.
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full_name: Deshmukh, K.
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full_name: Gilkis, A.
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last_name: González-Torà
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full_name: Gräfener, G.
last_name: Gräfener
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
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- first_name: B.
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last_name: Kubátová
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full_name: Lefever, R. R.
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full_name: Renzo, M.
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last_name: Shahaf
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full_name: Simón-Díaz, S.
last_name: Simón-Díaz
- first_name: L. A.C.
full_name: Van Son, L. A.C.
last_name: Van Son
- first_name: M.
full_name: Stoop, M.
last_name: Stoop
- first_name: S.
full_name: Toonen, S.
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- first_name: F.
full_name: Tramper, F.
last_name: Tramper
- first_name: R.
full_name: Valli, R.
last_name: Valli
- first_name: A.
full_name: Vigna-Gómez, A.
last_name: Vigna-Gómez
- first_name: J. S.
full_name: Vink, J. S.
last_name: Vink
- first_name: C.
full_name: Wang, C.
last_name: Wang
- first_name: R.
full_name: Willcox, R.
last_name: Willcox
citation:
ama: Sana H, Shenar T, Bodensteiner J, et al. A high fraction of close massive binary
stars at low metallicity. Nature Astronomy. 2025;9:1337-1346. doi:10.1038/s41550-025-02610-x
apa: Sana, H., Shenar, T., Bodensteiner, J., Britavskiy, N., Langer, N., Lennon,
D. J., … Willcox, R. (2025). A high fraction of close massive binary stars at
low metallicity. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-025-02610-x
chicago: Sana, H., T. Shenar, J. Bodensteiner, N. Britavskiy, N. Langer, D. J. Lennon,
L. Mahy, et al. “A High Fraction of Close Massive Binary Stars at Low Metallicity.”
Nature Astronomy. Springer Nature, 2025. https://doi.org/10.1038/s41550-025-02610-x.
ieee: H. Sana et al., “A high fraction of close massive binary stars at low
metallicity,” Nature Astronomy, vol. 9. Springer Nature, pp. 1337–1346,
2025.
ista: Sana H, Shenar T, Bodensteiner J, Britavskiy N, Langer N, Lennon DJ, Mahy
L, Mandel I, De Mink SE, Patrick LR, Villaseñor JI, Dirickx M, Abdul-Masih M,
Almeida LA, Backs F, Berlanas SR, Bernini-Peron M, Bowman DM, Bronner VA, Crowther
PA, Deshmukh K, Evans CJ, Fabry M, Gieles M, Gilkis A, González-Torà G, Gräfener
G, Götberg YLL, Hawcroft C, Hénault-Brunet V, Herrero A, Holgado G, Izzard RG,
De Koter A, Janssens S, Johnston C, Josiek J, Justham S, Kalari VM, Klencki J,
Kubát J, Kubátová B, Lefever RR, Van Loon JT, Ludwig B, Mackey J, Maíz Apellániz
J, Maravelias G, Marchant P, Mazeh T, Menon A, Moe M, Najarro F, Oskinova LM,
Ovadia R, Pauli D, Pawlak M, Ramachandran V, Renzo M, Rocha DF, Sander AAC, Schneider
FRN, Schootemeijer A, Schösser EC, Schürmann C, Sen K, Shahaf S, Simón-Díaz S,
Van Son LAC, Stoop M, Toonen S, Tramper F, Valli R, Vigna-Gómez A, Vink JS, Wang
C, Willcox R. 2025. A high fraction of close massive binary stars at low metallicity.
Nature Astronomy. 9, 1337–1346.
mla: Sana, H., et al. “A High Fraction of Close Massive Binary Stars at Low Metallicity.”
Nature Astronomy, vol. 9, Springer Nature, 2025, pp. 1337–46, doi:10.1038/s41550-025-02610-x.
short: H. Sana, T. Shenar, J. Bodensteiner, N. Britavskiy, N. Langer, D.J. Lennon,
L. Mahy, I. Mandel, S.E. De Mink, L.R. Patrick, J.I. Villaseñor, M. Dirickx, M.
Abdul-Masih, L.A. Almeida, F. Backs, S.R. Berlanas, M. Bernini-Peron, D.M. Bowman,
V.A. Bronner, P.A. Crowther, K. Deshmukh, C.J. Evans, M. Fabry, M. Gieles, A.
Gilkis, G. González-Torà, G. Gräfener, Y.L.L. Götberg, C. Hawcroft, V. Hénault-Brunet,
A. Herrero, G. Holgado, R.G. Izzard, A. De Koter, S. Janssens, C. Johnston, J.
Josiek, S. Justham, V.M. Kalari, J. Klencki, J. Kubát, B. Kubátová, R.R. Lefever,
J.T. Van Loon, B. Ludwig, J. Mackey, J. Maíz Apellániz, G. Maravelias, P. Marchant,
T. Mazeh, A. Menon, M. Moe, F. Najarro, L.M. Oskinova, R. Ovadia, D. Pauli, M.
Pawlak, V. Ramachandran, M. Renzo, D.F. Rocha, A.A.C. Sander, F.R.N. Schneider,
A. Schootemeijer, E.C. Schösser, C. Schürmann, K. Sen, S. Shahaf, S. Simón-Díaz,
L.A.C. Van Son, M. Stoop, S. Toonen, F. Tramper, R. Valli, A. Vigna-Gómez, J.S.
Vink, C. Wang, R. Willcox, Nature Astronomy 9 (2025) 1337–1346.
date_created: 2025-09-14T22:01:32Z
date_published: 2025-09-02T00:00:00Z
date_updated: 2025-12-30T10:27:05Z
day: '02'
department:
- _id: YlGo
doi: 10.1038/s41550-025-02610-x
external_id:
arxiv:
- '2509.12488'
isi:
- '001568077900001'
intvolume: ' 9'
isi: 1
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.48550/arXiv.2509.12488
month: '09'
oa: 1
oa_version: Preprint
page: 1337-1346
publication: Nature Astronomy
publication_identifier:
eissn:
- 2397-3366
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
scopus_import: '1'
status: public
title: A high fraction of close massive binary stars at low metallicity
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 9
year: '2025'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '18984'
abstract:
- lang: eng
text: Although planets have been found orbiting binary systems, whether they can
survive binary interactions is debated. While the tightest-orbit binaries should
host the most dynamically stable and long-lived circumbinary planetary systems,
they are also the systems that are expected to experience mass transfer, common
envelope evolution, or stellar mergers. In this study, we explore the effect of
stable non-conservative mass transfer on the dynamical evolution of circumbinary
planets. We present a new script that seamlessly integrates binary evolution data
from the 1D binary stellar evolution code MESA into the N-body simulation code
REBOUND. This integration framework enables a comprehensive examination of the
dynamical evolution of circumbinary planets orbiting mass-transferring binaries,
while simultaneously accounting for the detailed stellar structure evolution.
In addition, we introduce a recalibration method to mitigate numerical errors
from updates of binary properties during the system's dynamical evolution. We
construct a reference binary model in which a 2.21M⊙ star loses its hydrogen-rich
envelope through non-conservative mass transfer to the 1.76M⊙ companion star,
creating a 0.38M⊙ subdwarf. We find the tightest stable orbital separation for
circumbinary planets to be ≃2.5 times the binary separation after mass transfer.
Accounting for tides by using the interior stellar structure, we find that tidal
effects become apparent after the rapid mass transfer phase and start to fade
away during the latter stage of the slow mass transfer phase. Our research provides
a new framework for exploring circumbinary planet dynamics in interacting binary
systems.
acknowledgement: We thank the participants of the 2023 Kavli Summer Program in Astrophysics,
hosted by the Max Planck Institute for Astrophysics and funded by the Kavli Foundation.
In particular, Holly Preece, Selma de Mink, and Stephen Justham for their feedback
and comments on our work. ZX acknowledges support from the China Scholarship Council
(CSC). ST acknowledges the funding from the European Union’s Horizon 2020 research
and innovation programme under the Marie Skłodowska-Curie grant agreement No. 101034413.
AAT acknowledges support from the Horizon Europe research and innovation programmes
under the Marie Skłodowska-Curie grant agreement no. 101103134.
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Zepei
full_name: Xing, Zepei
last_name: Xing
- first_name: Santiago
full_name: Torres Rodriguez, Santiago
id: a8df4360-4328-11ee-8f1a-e502d0c83fc2
last_name: Torres Rodriguez
orcid: 0000-0002-3150-8988
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: Alessandro A.
full_name: Trani, Alessandro A.
last_name: Trani
- first_name: Valeriya
full_name: Korol, Valeriya
last_name: Korol
- first_name: Jorge
full_name: Cuadra, Jorge
last_name: Cuadra
citation:
ama: 'Xing Z, Torres Rodriguez S, Götberg YLL, Trani AA, Korol V, Cuadra J. Combining
REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries.
Monthly Notices of the Royal Astronomical Society. 2025;537(1):285-292.
doi:10.1093/mnras/stae2820'
apa: 'Xing, Z., Torres Rodriguez, S., Götberg, Y. L. L., Trani, A. A., Korol, V.,
& Cuadra, J. (2025). Combining REBOUND and MESA: Dynamical evolution of planets
orbiting interacting binaries. Monthly Notices of the Royal Astronomical Society.
Oxford University Press. https://doi.org/10.1093/mnras/stae2820'
chicago: 'Xing, Zepei, Santiago Torres Rodriguez, Ylva Louise Linsdotter Götberg,
Alessandro A. Trani, Valeriya Korol, and Jorge Cuadra. “Combining REBOUND and
MESA: Dynamical Evolution of Planets Orbiting Interacting Binaries.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2025.
https://doi.org/10.1093/mnras/stae2820.'
ieee: 'Z. Xing, S. Torres Rodriguez, Y. L. L. Götberg, A. A. Trani, V. Korol, and
J. Cuadra, “Combining REBOUND and MESA: Dynamical evolution of planets orbiting
interacting binaries,” Monthly Notices of the Royal Astronomical Society,
vol. 537, no. 1. Oxford University Press, pp. 285–292, 2025.'
ista: 'Xing Z, Torres Rodriguez S, Götberg YLL, Trani AA, Korol V, Cuadra J. 2025.
Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting
binaries. Monthly Notices of the Royal Astronomical Society. 537(1), 285–292.'
mla: 'Xing, Zepei, et al. “Combining REBOUND and MESA: Dynamical Evolution of Planets
Orbiting Interacting Binaries.” Monthly Notices of the Royal Astronomical Society,
vol. 537, no. 1, Oxford University Press, 2025, pp. 285–92, doi:10.1093/mnras/stae2820.'
short: Z. Xing, S. Torres Rodriguez, Y.L.L. Götberg, A.A. Trani, V. Korol, J. Cuadra,
Monthly Notices of the Royal Astronomical Society 537 (2025) 285–292.
date_created: 2025-02-02T23:01:53Z
date_published: 2025-02-01T00:00:00Z
date_updated: 2025-12-30T07:25:37Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
- _id: LiBu
doi: 10.1093/mnras/stae2820
ec_funded: 1
external_id:
arxiv:
- '2410.19695'
isi:
- '001400731500001'
file:
- access_level: open_access
checksum: 49fb4fe69f487d36169ccea60acbeccc
content_type: application/pdf
creator: dernst
date_created: 2025-12-30T07:24:34Z
date_updated: 2025-12-30T07:24:34Z
file_id: '20881'
file_name: 2025_MonthlyNoticesRAS_Xing.pdf
file_size: 2974244
relation: main_file
success: 1
file_date_updated: 2025-12-30T07:24:34Z
has_accepted_license: '1'
intvolume: ' 537'
isi: 1
issue: '1'
language:
- iso: eng
month: '02'
oa: 1
oa_version: Published Version
page: 285-292
project:
- _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c
call_identifier: H2020
grant_number: '101034413'
name: 'IST-BRIDGE: International postdoctoral program'
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting
binaries'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 537
year: '2025'
...
---
OA_place: publisher
OA_type: diamond
_id: '19844'
abstract:
- lang: eng
text: "Context. Rapidly rotating classical OBe stars have been proposed as the products
of binary interactions, and the fraction of Be stars with compact companions implies
that at least some are. However, to constrain the interaction physics spinning
up the OBe stars, a large sample of homogeneously analyzed OBe stars with well-determined
binary characteristics and orbital parameters are required.\r\n\r\nAims. We investigated
the multiplicity properties of a sample of 18 Oe, 62 Be, and two Of?p stars observed
within the BLOeM survey in the Small Magellanic Cloud. We analyzed the first nine
epochs of spectroscopic observations obtained over approximately three months
in 2023.\r\n\r\nMethods. Radial velocities (RVs) of all stars were measured using
cross-correlation based on different sets of absorption and emission lines. Applying
commonly used binarity criteria, we classified objects as binaries, binary candidates,
and apparently single (RV stable) objects. We further inspected the spectra for
double-lined spectroscopic binaries and cross-matched with catalogs of X-ray sources
and photometric binaries.\r\n\r\nResults. We classify 14 OBe stars as binaries,
and an additional 11 as binary candidates. The two Of?p stars are apparently single.
We find two more objects that are most likely currently interacting binaries.
Without those, the observed binary fraction for the remaining OBe sample of 78
stars is fobs+candOBe = 0.18 ± 0.04 (fobs+candOBe = 0.32±0.05 including candidates).
This binary fraction is less than half of that measured for OB stars in BLOeM.
Combined with the lower fraction of SB2s, this suggests that OBe stars do indeed
have fundamentally different present-day binary properties than OB stars. We find
no evidence for OBe binaries with massive compact companions, in contrast to expectations
from binary population synthesis.\r\n\r\nConclusions. Our results support the
binary scenario as an important formation channel for OBe stars, as post-interaction
binaries may have been disrupted or the stripped companions of OBe stars are harder
to detect. Further observations are required to characterize the detected binaries,
their orbital parameters, and the nature of their companions."
acknowledgement: 'The research leading to these results has received funding from
the European Research Council (ERC) under the European Union’s Horizon 2020 and
Horizon Europe research and innovation programme (grant agreement numbers 772225:
MULTIPLES, and 945806) and is supported by the Deutsche Forschungsgemeinschaft (DFG,
German Research Foundation) under Germany’s Excellence Strategy EXC 2181/1-390900948
(the Heidelberg STRUCTURES Excellence Cluster). DMB gratefully acknowledges funding
from UK Research and Innovation (UKRI) in the form of a Frontier Research grant
under the UK government’s ERC Horizon Europe funding guarantee (SYMPHONY; grant
number: EP/Y031059/1), and a Royal Society University Research Fellowship (URF;
grant number: URF\R1\231631). RGI is funded by STFC grant ST/Y002350/1 as part of
the BRIDGCE UK network, and thanks IReNA colleagues for stimulating discussions.
Z.K. acknowledges support from JSPS Kakenhi Grant-in-Aid for Scientific Research
(23K19071). IM acknowledges support from the Australian Research Council (ARC) Centre
of Excellence for GravitationalWave Discovery (OzGrav), through project number CE230100016.
DP acknowledges financial support by the Deutsches Zentrum für Luft und Raumfahrt
(DLR) grant FKZ 50OR2005. DFR is thankful for the support of CAPES-Br and FAPERJ/DSC-10
(SEI-260003/001630/2023). AACS and VR are supported by the German Deutsche Forschungsgemeinschaft
(DFG) under Project-ID 445674056 (Emmy Noether Research Group SA4064/1-1, PI Sander).
AACS and VR are further supported by funding from the Federal Ministry of Education
and Research (BMBF) and the Baden-Württemberg Ministry of Science as part of the
Excellence Strategy of the German Federal and State Governments. JIV acknowledges
support from the European Research Council for the ERC Advanced Grant 101054731.
LRP acknowledges support from grant PID2022-140483NB-C22 funded by MCIN/AEI/10.13039/501100011033.
GH acknowledges support from grants PID2021-122397NB-C21/PID2022-136640NB-C22 funded
by MCIN/AEI/FEDER/10.13039/501100011033. J.K. thanks for the support of a grant
GA CR 22-34467S. This project has received funding from the European Research Council
(ERC) under the European Union’s Horizon 2020 research and innovation programme
(grant agreement 101164755/METAL) and was supported by the Israel Science Foundation
(ISF) under grant number 2434/24.'
article_number: A38
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: N.
full_name: Britavskiy, N.
last_name: Britavskiy
- first_name: P. A.
full_name: Crowther, P. A.
last_name: Crowther
- first_name: N.
full_name: Langer, N.
last_name: Langer
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- first_name: J. I.
full_name: Villaseñor, J. I.
last_name: Villaseñor
- first_name: M.
full_name: Abdul-Masih, M.
last_name: Abdul-Masih
- first_name: D. M.
full_name: Bowman, D. M.
last_name: Bowman
- first_name: A.
full_name: De Koter, A.
last_name: De Koter
- first_name: S. E.
full_name: De Mink, S. E.
last_name: De Mink
- first_name: K.
full_name: Deshmukh, K.
last_name: Deshmukh
- first_name: M.
full_name: Fabry, M.
last_name: Fabry
- first_name: A.
full_name: Gilkis, A.
last_name: Gilkis
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: G.
full_name: Holgado, G.
last_name: Holgado
- first_name: R. G.
full_name: Izzard, R. G.
last_name: Izzard
- first_name: S.
full_name: Janssens, S.
last_name: Janssens
- first_name: V. M.
full_name: Kalari, V. M.
last_name: Kalari
- first_name: Z.
full_name: Keszthelyi, Z.
last_name: Keszthelyi
- first_name: J.
full_name: Kubát, J.
last_name: Kubát
- first_name: I.
full_name: Mandel, I.
last_name: Mandel
- first_name: G.
full_name: Maravelias, G.
last_name: Maravelias
- first_name: L. M.
full_name: Oskinova, L. M.
last_name: Oskinova
- first_name: D.
full_name: Pauli, D.
last_name: Pauli
- first_name: V.
full_name: Ramachandran, V.
last_name: Ramachandran
- first_name: D. F.
full_name: Rocha, D. F.
last_name: Rocha
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: A. A.C.
full_name: Sander, A. A.C.
last_name: Sander
- first_name: F. R.N.
full_name: Schneider, F. R.N.
last_name: Schneider
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: K.
full_name: Sen, K.
last_name: Sen
- first_name: M.
full_name: Stoop, M.
last_name: Stoop
- first_name: S.
full_name: Toonen, S.
last_name: Toonen
- first_name: J. T.
full_name: Van Loon, J. T.
last_name: Van Loon
- first_name: R.
full_name: Valli, R.
last_name: Valli
- first_name: A.
full_name: Vigna-Gómez, A.
last_name: Vigna-Gómez
- first_name: J. S.
full_name: Vink, J. S.
last_name: Vink
- first_name: C.
full_name: Wang, C.
last_name: Wang
- first_name: X. T.
full_name: Xu, X. T.
last_name: Xu
citation:
ama: 'Bodensteiner J, Shenar T, Sana H, et al. Binarity at LOw Metallicity (BLOeM):
Multiplicity properties of Oe and Be stars. Astronomy & Astrophysics.
2025;698. doi:10.1051/0004-6361/202452623'
apa: 'Bodensteiner, J., Shenar, T., Sana, H., Britavskiy, N., Crowther, P. A., Langer,
N., … Xu, X. T. (2025). Binarity at LOw Metallicity (BLOeM): Multiplicity properties
of Oe and Be stars. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202452623'
chicago: 'Bodensteiner, J., T. Shenar, H. Sana, N. Britavskiy, P. A. Crowther, N.
Langer, D. J. Lennon, et al. “Binarity at LOw Metallicity (BLOeM): Multiplicity
Properties of Oe and Be Stars.” Astronomy & Astrophysics. EDP Sciences,
2025. https://doi.org/10.1051/0004-6361/202452623.'
ieee: 'J. Bodensteiner et al., “Binarity at LOw Metallicity (BLOeM): Multiplicity
properties of Oe and Be stars,” Astronomy & Astrophysics, vol. 698.
EDP Sciences, 2025.'
ista: 'Bodensteiner J, Shenar T, Sana H, Britavskiy N, Crowther PA, Langer N, Lennon
DJ, Mahy L, Patrick LR, Villaseñor JI, Abdul-Masih M, Bowman DM, De Koter A, De
Mink SE, Deshmukh K, Fabry M, Gilkis A, Götberg YLL, Holgado G, Izzard RG, Janssens
S, Kalari VM, Keszthelyi Z, Kubát J, Mandel I, Maravelias G, Oskinova LM, Pauli
D, Ramachandran V, Rocha DF, Renzo M, Sander AAC, Schneider FRN, Schootemeijer
A, Sen K, Stoop M, Toonen S, Van Loon JT, Valli R, Vigna-Gómez A, Vink JS, Wang
C, Xu XT. 2025. Binarity at LOw Metallicity (BLOeM): Multiplicity properties of
Oe and Be stars. Astronomy & Astrophysics. 698, A38.'
mla: 'Bodensteiner, J., et al. “Binarity at LOw Metallicity (BLOeM): Multiplicity
Properties of Oe and Be Stars.” Astronomy & Astrophysics, vol. 698,
A38, EDP Sciences, 2025, doi:10.1051/0004-6361/202452623.'
short: J. Bodensteiner, T. Shenar, H. Sana, N. Britavskiy, P.A. Crowther, N. Langer,
D.J. Lennon, L. Mahy, L.R. Patrick, J.I. Villaseñor, M. Abdul-Masih, D.M. Bowman,
A. De Koter, S.E. De Mink, K. Deshmukh, M. Fabry, A. Gilkis, Y.L.L. Götberg, G.
Holgado, R.G. Izzard, S. Janssens, V.M. Kalari, Z. Keszthelyi, J. Kubát, I. Mandel,
G. Maravelias, L.M. Oskinova, D. Pauli, V. Ramachandran, D.F. Rocha, M. Renzo,
A.A.C. Sander, F.R.N. Schneider, A. Schootemeijer, K. Sen, M. Stoop, S. Toonen,
J.T. Van Loon, R. Valli, A. Vigna-Gómez, J.S. Vink, C. Wang, X.T. Xu, Astronomy
& Astrophysics 698 (2025).
date_created: 2025-06-15T22:01:30Z
date_published: 2025-06-01T00:00:00Z
date_updated: 2026-04-16T08:17:17Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202452623
external_id:
arxiv:
- '2502.02641'
isi:
- '001497903100011'
file:
- access_level: open_access
checksum: 51d79c82f6030180fb7c5d7ba01b2da8
content_type: application/pdf
creator: dernst
date_created: 2025-06-23T07:54:57Z
date_updated: 2025-06-23T07:54:57Z
file_id: '19866'
file_name: 2025_AstronomyAstrophysics_Bodensteiner.pdf
file_size: 2404827
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file_date_updated: 2025-06-23T07:54:57Z
has_accepted_license: '1'
intvolume: ' 698'
isi: 1
language:
- iso: eng
month: '06'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Binarity at LOw Metallicity (BLOeM): Multiplicity properties of Oe and Be
stars'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: ba8df636-2132-11f1-aed0-ed93e2281fdd
volume: 698
year: '2025'
...
---
DOAJ_listed: '1'
_id: '18111'
abstract:
- lang: eng
text: Observations of tidal disruption events (TDEs) show signs of nitrogen enrichment
reminiscent of other astrophysical sources such as active galactic nuclei and
star-forming galaxies. Given that TDEs probe the gas from a single star, it is
possible to test whether the observed enrichment is consistent with expectations
from the CNO cycle by looking at the observed nitrogen/carbon (N/C) abundance
ratios. Given that ≈20% of solar-mass stars (and an even larger fraction of more
massive stars) live in close binaries, it is worthwhile to also consider what
TDEs from stars influenced by binary evolution would look like. We show here that
TDEs from stars stripped of their hydrogen-rich (and nitrogen-poor) envelopes
through previous binary-induced mass loss can produce much higher observable N/C
enhancements than even TDEs from massive stars. Additionally, we predict that
the time dependence of the N/C abundance ratio in the mass fallback rate of stripped
stars will follow the inverse behavior of main-sequence stars, enabling a more
accurate characterization of the disrupted star.
acknowledgement: "This work was performed in part at Aspen Center for Physics, which
is supported by National Science Foundation grant PHY-2210452. We thank the participants
and organizers of the summer Aspen 2023 workshop on “Stellar Interactions and the
Transients They Cause” for fruitful discussions. B.M. is grateful for support from
the Carnegie Theoretical Astrophysics\r\nCenter. M.G.-G. is grateful for the support
from Northwestern University’s Presidential Fellowship. E.R.-R. thanks the Heising-Simons
Foundation, NSF (AST-2150255 and AST2307710), Swift (80NSSC21K1409, 80NSSC19K1391),
and Chandra (22-0142) for support. "
article_number: L9
article_processing_charge: Yes
article_type: original
author:
- first_name: Brenna
full_name: Mockler, Brenna
last_name: Mockler
- first_name: Monica
full_name: Gallegos-Garcia, Monica
last_name: Gallegos-Garcia
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: Jon M.
full_name: Miller, Jon M.
last_name: Miller
- first_name: Enrico
full_name: Ramirez-Ruiz, Enrico
last_name: Ramirez-Ruiz
citation:
ama: Mockler B, Gallegos-Garcia M, Götberg YLL, Miller JM, Ramirez-Ruiz E. Tidal
disruption events from stripped stars. Astrophysical Journal Letters. 2024;973(1).
doi:10.3847/2041-8213/ad6c34
apa: Mockler, B., Gallegos-Garcia, M., Götberg, Y. L. L., Miller, J. M., & Ramirez-Ruiz,
E. (2024). Tidal disruption events from stripped stars. Astrophysical Journal
Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ad6c34
chicago: Mockler, Brenna, Monica Gallegos-Garcia, Ylva Louise Linsdotter Götberg,
Jon M. Miller, and Enrico Ramirez-Ruiz. “Tidal Disruption Events from Stripped
Stars.” Astrophysical Journal Letters. IOP Publishing, 2024. https://doi.org/10.3847/2041-8213/ad6c34.
ieee: B. Mockler, M. Gallegos-Garcia, Y. L. L. Götberg, J. M. Miller, and E. Ramirez-Ruiz,
“Tidal disruption events from stripped stars,” Astrophysical Journal Letters,
vol. 973, no. 1. IOP Publishing, 2024.
ista: Mockler B, Gallegos-Garcia M, Götberg YLL, Miller JM, Ramirez-Ruiz E. 2024.
Tidal disruption events from stripped stars. Astrophysical Journal Letters. 973(1),
L9.
mla: Mockler, Brenna, et al. “Tidal Disruption Events from Stripped Stars.” Astrophysical
Journal Letters, vol. 973, no. 1, L9, IOP Publishing, 2024, doi:10.3847/2041-8213/ad6c34.
short: B. Mockler, M. Gallegos-Garcia, Y.L.L. Götberg, J.M. Miller, E. Ramirez-Ruiz,
Astrophysical Journal Letters 973 (2024).
date_created: 2024-09-22T22:01:42Z
date_published: 2024-09-12T00:00:00Z
date_updated: 2025-09-08T09:48:50Z
day: '12'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.3847/2041-8213/ad6c34
external_id:
isi:
- '001310592900001'
file:
- access_level: open_access
checksum: 050ddf873244839825714cca42b5d857
content_type: application/pdf
creator: dernst
date_created: 2024-09-30T08:54:26Z
date_updated: 2024-09-30T08:54:26Z
file_id: '18161'
file_name: 2024_AstrophysicalJourn_Mockler.pdf
file_size: 844227
relation: main_file
success: 1
file_date_updated: 2024-09-30T08:54:26Z
has_accepted_license: '1'
intvolume: ' 973'
isi: 1
issue: '1'
language:
- iso: eng
month: '09'
oa: 1
oa_version: Published Version
publication: Astrophysical Journal Letters
publication_identifier:
eissn:
- 2041-8213
issn:
- 2041-8205
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Tidal disruption events from stripped stars
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 973
year: '2024'
...
---
OA_place: publisher
OA_type: hybrid
_id: '18492'
abstract:
- lang: eng
text: 'Surveys in the Milky Way and Large Magellanic Cloud have revealed that the
majority of massive stars will interact with companions during their lives. However,
knowledge of the binary properties of massive stars at low metallicity, and therefore
in conditions approaching those of the Early Universe, remain sparse. We present
the Binarity at LOw Metallicity (BLOeM) campaign, an ESO large programme designed
to obtain 25 epochs of spectroscopy for 929 massive stars in the Small Magellanic
Cloud, allowing us to probe multiplicity in the lowest-metallicity conditions
to date (Z = 0.2 Z⊙). BLOeM will provide (i) the binary fraction, (ii) the orbital
configurations of systems with periods of P ≲ 3 yr, (iii) dormant black-hole binary
candidates (OB+BH), and (iv) a legacy database of physical parameters of massive
stars at low metallicity. Main sequence (OB-type) and evolved (OBAF-type) massive
stars are observed with the LR02 setup of the GIRAFFE instrument of the Very Large
Telescope (3960–4570 Å resolving power R = 6200; typical signal-to-noise ratio(S/N)
≈70–100). This paper utilises the first nine epochs obtained over a three-month
time period. We describe the survey and data reduction, perform a spectral classification
of the stacked spectra, and construct a Hertzsprung-Russell diagram of the sample
via spectral-type and photometric calibrations. Our detailed classification reveals
that the sample covers spectral types from O4 to F5, spanning the effective temperature
and luminosity ranges 6.5 ≲ Teff/kK ≲ 45 and 3.7 < log L/L⊙ < 6.1 and initial
masses of 8 ≲ Mini ≲ 80 M⊙. The sample comprises 159 O-type stars, 331 early B-type
(B0–3) dwarfs and giants (luminosity classes V–III), 303 early B-type supergiants
(II–I), and 136 late-type BAF supergiants. At least 82 stars are OBe stars: 20
O-type and 62 B-type (13% and 11% of the respective samples). In addition, the
sample includes 4 high-mass X-ray binaries, 3 stars resembling luminous blue variables,
2 bloated stripped-star candidates, 2 candidate magnetic stars, and 74 eclipsing
binaries.'
acknowledgement: 'The research leading to these results has received funding from
the European Research Council (ERC) under the European Union’s Horizon 2020 research
and innovation programme (grant agreement numbers 772225: MULTIPLES). PAC and JMB
are supported by the Science and Technology Facilities Council research grant ST/V000853/1
(PI. V. Dhillon). DMB gratefully acknowledges support from UK Research and Innovation
(UKRI) in the form of a Frontier Research grant under the UK government’s 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).
ZK acknowledges support from JSPS Kakenhi Grant-in-Aid for Scientific Research (23K19071).
IM acknowledges support from the Australian Research Council (ARC) Centre of Excellence
for Gravitational Wave Discovery (OzGrav), through project number CE230100016. AACS,
VR, RRL, and MBP are funded by the Deutsche Forschungsgemeinschaft (DFG, German
Research Foundation) in the form of an Emmy Noether Research Group – Project-ID
445674056 (SA4064/1-1, PI Sander). GGT and JJ are supported by the German Deutsche
Forschungsgemeinschaft (DFG) under Project-ID 496854903 (SA4064/2-1, PI Sander)
VR, GGT, and AACS further acknowledge support from the Federal Ministry of Education
and Research (BMBF) and the Baden-Württemberg Ministry of Science as part of the
Excellence Strategy of the German Federal and State Governments. ECS acknowledges
financial support by the Federal Ministry for Economic Affairs and Climate Action
(BMWK) via the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt,
DLR) grant 50 OR 2306 (PI: Ramachandran/Sander). This work has received funding
from the European Research Council (ERC) under the European Union’s Horizon 2020
research and innovation programme (Grant agreement No. 945806) and is supported
by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s
Excellence Strategy EXC 2181/1-390900948 (the Heidelberg STRUCTURES Excellence Cluster).
LMO is thankful for the funding provided by the DFG grant 443790621. This paper
benefited from discussions at the International Space Science Institute (ISSI) in
Bern through ISSI International Team project 512 (Multiwavelength View on Massive
Stars in the Era of Multimessenger Astronomy). DP acknowledges financial support
by the Deutsches Zentrum für Luft und Raumfahrt (DLR) grant FKZ 50OR2005. JIV acknowledges
the European Research Council for support from the ERC Advanced grant ERC-2021-ADG101054731.
JSV is supported by STFC (Science and Technology Facilities Council) funding under
grant number ST/V000233/1. GH, SS-D, SRB and AH acknowledge support from the State
Research Agency (AEI) of the Spanish Ministry of Science and Innovation (MICIN)
and the European Regional Development Fund, FEDER under grants PID2021-122397NB-C21
and CEX2019-000920-S. SRB also acknowledges financial support by NextGeneration
EU/PRTR and MIU (UNI/551/2021) through grant Margarita Salas-ULL. DFR is thankful
for the support of the CAPES-Br and FAPERJ/DSC-10 (SEI-260003/001630/2023). F.N.,
and L.R.P. acknowledge support by grants PID2019-105552RB-C41 and PID2022-137779OB-C41
funded by MCIN/AEI/10.13039/501100011033 by “ERDF A way of making Europe”. MG acknowledges
financial support from the grants PID2021-125485NB-C22, CEX2019-000918-M funded
by MCIN/AEI/10.13039/501100011033 (State Agency for Research of the Spanish Ministry
of Science and Innovation) and SGR-2021-01069 (AGAUR). GM acknowledges funding support
from the European Research Council (ERC) under the European Union’s Horizon 2020
research and innovation programme (Grant agreement No. 772086). JMA acknowledges
support from the Spanish Government Ministerio de Ciencia e Innovación and Agencia
Estatal de Investigación (10.13 039/501 100 011 033) through grant PID2022-136640
NB-C22 and from the Consejo Superior de Investigaciones Científicas (CSIC) through
grant 2022-AEP 005. MP is supported by the BEKKER fellowship BPN/BEK/2022/1/00106
from the Polish National Agency for Academic Exchange. KS is funded by the National
Science Center (NCN), Poland, under grant number OPUS 2021/41/B/ST9/00757. JM acknowledges
support from a Royal Society-Science Foundation Ireland University Research Fellowship.
SJ acknowledges support from the FWO PhD fellowship under project 11E1721N. FB acknowledges
the support of the European Research Council (ERC) Horizon Europe under grant agreement
number 101044048.'
article_number: A289
article_processing_charge: Yes (in subscription journal)
article_type: original
arxiv: 1
author:
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: J.
full_name: Bodensteiner, J.
last_name: Bodensteiner
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: P. A.
full_name: Crowther, P. A.
last_name: Crowther
- first_name: D. J.
full_name: Lennon, D. J.
last_name: Lennon
- first_name: M.
full_name: Abdul-Masih, M.
last_name: Abdul-Masih
- first_name: L. A.
full_name: Almeida, L. A.
last_name: Almeida
- first_name: F.
full_name: Backs, F.
last_name: Backs
- first_name: S. R.
full_name: Berlanas, S. R.
last_name: Berlanas
- first_name: M.
full_name: Bernini-Peron, M.
last_name: Bernini-Peron
- first_name: J. M.
full_name: Bestenlehner, J. M.
last_name: Bestenlehner
- first_name: D. M.
full_name: Bowman, D. M.
last_name: Bowman
- first_name: V. A.
full_name: Bronner, V. A.
last_name: Bronner
- first_name: N.
full_name: Britavskiy, N.
last_name: Britavskiy
- first_name: A.
full_name: De Koter, A.
last_name: De Koter
- first_name: S. E.
full_name: De Mink, S. E.
last_name: De Mink
- first_name: K.
full_name: Deshmukh, K.
last_name: Deshmukh
- first_name: C. J.
full_name: Evans, C. J.
last_name: Evans
- first_name: M.
full_name: Fabry, M.
last_name: Fabry
- first_name: M.
full_name: Gieles, M.
last_name: Gieles
- first_name: A.
full_name: Gilkis, A.
last_name: Gilkis
- first_name: G.
full_name: González-Torà, G.
last_name: González-Torà
- first_name: G.
full_name: Gräfener, G.
last_name: Gräfener
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: C.
full_name: Hawcroft, C.
last_name: Hawcroft
- first_name: V.
full_name: Hénault-Brunet, V.
last_name: Hénault-Brunet
- first_name: A.
full_name: Herrero, A.
last_name: Herrero
- first_name: G.
full_name: Holgado, G.
last_name: Holgado
- first_name: S.
full_name: Janssens, S.
last_name: Janssens
- first_name: C.
full_name: Johnston, C.
last_name: Johnston
- first_name: J.
full_name: Josiek, J.
last_name: Josiek
- first_name: S.
full_name: Justham, S.
last_name: Justham
- first_name: V. M.
full_name: Kalari, V. M.
last_name: Kalari
- first_name: Z. Z.
full_name: Katabi, Z. Z.
last_name: Katabi
- first_name: Z.
full_name: Keszthelyi, Z.
last_name: Keszthelyi
- first_name: J.
full_name: Klencki, J.
last_name: Klencki
- first_name: J.
full_name: Kubát, J.
last_name: Kubát
- first_name: B.
full_name: Kubátová, B.
last_name: Kubátová
- first_name: N.
full_name: Langer, N.
last_name: Langer
- first_name: R. R.
full_name: Lefever, R. R.
last_name: Lefever
- first_name: B.
full_name: Ludwig, B.
last_name: Ludwig
- first_name: J.
full_name: Mackey, J.
last_name: Mackey
- first_name: L.
full_name: Mahy, L.
last_name: Mahy
- first_name: J.
full_name: Maíz Apellániz, J.
last_name: Maíz Apellániz
- first_name: I.
full_name: Mandel, I.
last_name: Mandel
- first_name: G.
full_name: Maravelias, G.
last_name: Maravelias
- first_name: P.
full_name: Marchant, P.
last_name: Marchant
- first_name: A.
full_name: Menon, A.
last_name: Menon
- first_name: F.
full_name: Najarro, F.
last_name: Najarro
- first_name: L. M.
full_name: Oskinova, L. M.
last_name: Oskinova
- first_name: A. J.G.
full_name: O'Grady, A. J.G.
last_name: O'Grady
- first_name: R.
full_name: Ovadia, R.
last_name: Ovadia
- first_name: L. R.
full_name: Patrick, L. R.
last_name: Patrick
- first_name: D.
full_name: Pauli, D.
last_name: Pauli
- first_name: M.
full_name: Pawlak, M.
last_name: Pawlak
- first_name: V.
full_name: Ramachandran, V.
last_name: Ramachandran
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: D. F.
full_name: Rocha, D. F.
last_name: Rocha
- first_name: A. A.C.
full_name: Sander, A. A.C.
last_name: Sander
- first_name: T.
full_name: Sayada, T.
last_name: Sayada
- first_name: F. R.N.
full_name: Schneider, F. R.N.
last_name: Schneider
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: E. C.
full_name: Schösser, E. C.
last_name: Schösser
- first_name: C.
full_name: Schürmann, C.
last_name: Schürmann
- first_name: K.
full_name: Sen, K.
last_name: Sen
- first_name: S.
full_name: Shahaf, S.
last_name: Shahaf
- first_name: S.
full_name: Simón-Díaz, S.
last_name: Simón-Díaz
- first_name: M.
full_name: Stoop, M.
last_name: Stoop
- first_name: S.
full_name: Toonen, S.
last_name: Toonen
- first_name: F.
full_name: Tramper, F.
last_name: Tramper
- first_name: J. Th
full_name: Van Loon, J. Th
last_name: Van Loon
- first_name: R.
full_name: Valli, R.
last_name: Valli
- first_name: L. A.C.
full_name: Van Son, L. A.C.
last_name: Van Son
- first_name: A.
full_name: Vigna-Gómez, A.
last_name: Vigna-Gómez
- first_name: J. I.
full_name: Villaseñor, J. I.
last_name: Villaseñor
- first_name: J. S.
full_name: Vink, J. S.
last_name: Vink
- first_name: C.
full_name: Wang, C.
last_name: Wang
- first_name: R.
full_name: Willcox, R.
last_name: Willcox
citation:
ama: 'Shenar T, Bodensteiner J, Sana H, et al. Binarity at LOw Metallicity (BLOeM):
A spectroscopic VLT monitoring survey of massive stars in the SMC. Astronomy
and Astrophysics. 2024;690. doi:10.1051/0004-6361/202451586'
apa: 'Shenar, T., Bodensteiner, J., Sana, H., Crowther, P. A., Lennon, D. J., Abdul-Masih,
M., … Willcox, R. (2024). Binarity at LOw Metallicity (BLOeM): A spectroscopic
VLT monitoring survey of massive stars in the SMC. Astronomy and Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/202451586'
chicago: 'Shenar, T., J. Bodensteiner, H. Sana, P. A. Crowther, D. J. Lennon, M.
Abdul-Masih, L. A. Almeida, et al. “Binarity at LOw Metallicity (BLOeM): A Spectroscopic
VLT Monitoring Survey of Massive Stars in the SMC.” Astronomy and Astrophysics.
EDP Sciences, 2024. https://doi.org/10.1051/0004-6361/202451586.'
ieee: 'T. Shenar et al., “Binarity at LOw Metallicity (BLOeM): A spectroscopic
VLT monitoring survey of massive stars in the SMC,” Astronomy and Astrophysics,
vol. 690. EDP Sciences, 2024.'
ista: 'Shenar T, Bodensteiner J, Sana H, Crowther PA, Lennon DJ, Abdul-Masih M,
Almeida LA, Backs F, Berlanas SR, Bernini-Peron M, Bestenlehner JM, Bowman DM,
Bronner VA, Britavskiy N, De Koter A, De Mink SE, Deshmukh K, Evans CJ, Fabry
M, Gieles M, Gilkis A, González-Torà G, Gräfener G, Götberg YLL, Hawcroft C, Hénault-Brunet
V, Herrero A, Holgado G, Janssens S, Johnston C, Josiek J, Justham S, Kalari VM,
Katabi ZZ, Keszthelyi Z, Klencki J, Kubát J, Kubátová B, Langer N, Lefever RR,
Ludwig B, Mackey J, Mahy L, Maíz Apellániz J, Mandel I, Maravelias G, Marchant
P, Menon A, Najarro F, Oskinova LM, O’Grady AJG, Ovadia R, Patrick LR, Pauli D,
Pawlak M, Ramachandran V, Renzo M, Rocha DF, Sander AAC, Sayada T, Schneider FRN,
Schootemeijer A, Schösser EC, Schürmann C, Sen K, Shahaf S, Simón-Díaz S, Stoop
M, Toonen S, Tramper F, Van Loon JT, Valli R, Van Son LAC, Vigna-Gómez A, Villaseñor
JI, Vink JS, Wang C, Willcox R. 2024. Binarity at LOw Metallicity (BLOeM): A spectroscopic
VLT monitoring survey of massive stars in the SMC. Astronomy and Astrophysics.
690, A289.'
mla: 'Shenar, T., et al. “Binarity at LOw Metallicity (BLOeM): A Spectroscopic VLT
Monitoring Survey of Massive Stars in the SMC.” Astronomy and Astrophysics,
vol. 690, A289, EDP Sciences, 2024, doi:10.1051/0004-6361/202451586.'
short: T. Shenar, J. Bodensteiner, H. Sana, P.A. Crowther, D.J. Lennon, M. Abdul-Masih,
L.A. Almeida, F. Backs, S.R. Berlanas, M. Bernini-Peron, J.M. Bestenlehner, D.M.
Bowman, V.A. Bronner, N. Britavskiy, A. De Koter, S.E. De Mink, K. Deshmukh, C.J.
Evans, M. Fabry, M. Gieles, A. Gilkis, G. González-Torà, G. Gräfener, Y.L.L. Götberg,
C. Hawcroft, V. Hénault-Brunet, A. Herrero, G. Holgado, S. Janssens, C. Johnston,
J. Josiek, S. Justham, V.M. Kalari, Z.Z. Katabi, Z. Keszthelyi, J. Klencki, J.
Kubát, B. Kubátová, N. Langer, R.R. Lefever, B. Ludwig, J. Mackey, L. Mahy, J.
Maíz Apellániz, I. Mandel, G. Maravelias, P. Marchant, A. Menon, F. Najarro, L.M.
Oskinova, A.J.G. O’Grady, R. Ovadia, L.R. Patrick, D. Pauli, M. Pawlak, V. Ramachandran,
M. Renzo, D.F. Rocha, A.A.C. Sander, T. Sayada, F.R.N. Schneider, A. Schootemeijer,
E.C. Schösser, C. Schürmann, K. Sen, S. Shahaf, S. Simón-Díaz, M. Stoop, S. Toonen,
F. Tramper, J.T. Van Loon, R. Valli, L.A.C. Van Son, A. Vigna-Gómez, J.I. Villaseñor,
J.S. Vink, C. Wang, R. Willcox, Astronomy and Astrophysics 690 (2024).
date_created: 2024-11-03T23:01:44Z
date_published: 2024-10-01T00:00:00Z
date_updated: 2025-09-08T14:31:11Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.1051/0004-6361/202451586
external_id:
arxiv:
- '2407.14593'
isi:
- '001336770600014'
file:
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checksum: b378b36726591f3479a927d924ab8e77
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intvolume: ' 690'
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language:
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month: '10'
oa: 1
oa_version: Published Version
publication: Astronomy and Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Binarity at LOw Metallicity (BLOeM): A spectroscopic VLT monitoring survey
of massive stars in the SMC'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 690
year: '2024'
...
---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
_id: '18524'
abstract:
- lang: eng
text: Recent works have constrained the binary fraction of evolved populations of
massive stars in local galaxies such as red supergiants and Wolf–Rayet stars,
but the binary fraction of yellow supergiants (YSGs) in the Hertzsprung gap remains
unconstrained. Binary evolution theory predicts that the Hertzsprung gap is home
to multiple populations of binary systems with varied evolutionary histories.
In this paper, we develop a method to distinguish single YSGs from YSG plus O-
or B-type main-sequence binaries using optical and ultraviolet photometry, and
then apply this method to identify candidate YSG binaries in the Magellanic Clouds.
After constructing a set of combined stellar atmosphere models, we find that optical
photometry is, given typical measurement and reddening uncertainties, sufficient
to discern single YSGs from YSG+OB binaries if the OB-star is at least ∼5M⊙ for
Teff,YSG ∼ 4000 K, but requires a ∼20M⊙ OB star for YSGs up to Teff,YSG ∼ 9000
K. For these hotter YSG temperatures, ultraviolet photometry allows binaries with
OB companions as small as ∼7M⊙ to be identified. We use color–color spaces developed
from these models to search for evidence of excess blue or ultraviolet light in
a set of ∼1000 YSG candidates in the Magellanic Clouds. We identify hundreds of
candidate YSG binary systems and report a preliminary fraction of YSGs that show
a blue/UV color excess of 20%–60%. Spectroscopic follow-up is now required to
confirm the true nature of this population.
acknowledgement: "The authors thank Aaron Tohuvavohu, Katie Breivik, Marten van Kerkwijk,
Jakub Klencki, Eva Laplace, and Dae-Sik Moon for helpful discussions, and Adiv Paradise
for helpful edits. The authors also thank the anonymous reviewer for a helpful and
constructive referee report.\r\nThe authors at the University of Toronto acknowledge
that the land on which the University of Toronto operates is the traditional territory
of the Huron–Wendat, the Seneca, and the Mississaugas of the Credit River. They
are grateful to have the opportunity to work on this land.\r\nThe Dunlap Institute
is funded through an endowment established by the David Dunlap family and the University
of Toronto.\r\nA.J.G.O. is supported by a McWilliams Fellowship at Carnegie Mellon
University. M.R.D. acknowledges support from the NSERC through grant RGPIN-2019-06186,
the Canada Research Chairs Program, and the Dunlap Institute at the University of
Toronto. B.M.G. acknowledges the support of the Natural Sciences and Engineering
Research Council of Canada (NSERC) through grant RGPIN-2022-03163, and of the Canada
Research Chairs program. Support for this work was provided by NASA through the
NASA Hubble Fellowship Program grant Nos. HST-HF2-51457.001-A and HST-HF2-51516
awarded by the Space Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555.\r\nThis
research has made use of the SIMBAD database (M. Wenger et al. 2000), operated at
CDS, Strasbourg, France, and the SVO Filter Profile Service 13 supported by the
Spanish MINECO through grant AYA2017-84089 (C. Rodrigo et al. 2012, 2020).\r\nThis
research has made use of the following software: astropy (Astropy Collaboration
et al. 2013, 2018, 2022), IRAF (D. Tody 1986, 1993), and TOPCAT (M. B. Taylor 2005)."
article_number: '29'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Anna J.G.
full_name: O’Grady, Anna J.G.
last_name: O’Grady
- first_name: Maria R.
full_name: Drout, Maria R.
last_name: Drout
- first_name: Kathryn F.
full_name: Neugent, Kathryn F.
last_name: Neugent
- first_name: Bethany
full_name: Ludwig, Bethany
last_name: Ludwig
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: B. M.
full_name: Gaensler, B. M.
last_name: Gaensler
citation:
ama: O’Grady AJG, Drout MR, Neugent KF, Ludwig B, Götberg YLL, Gaensler BM. Binary
yellow supergiants in the Magellanic Clouds. I. Photometric candidate identification.
Astrophysical Journal. 2024;975. doi:10.3847/1538-4357/ad778a
apa: O’Grady, A. J. G., Drout, M. R., Neugent, K. F., Ludwig, B., Götberg, Y. L.
L., & Gaensler, B. M. (2024). Binary yellow supergiants in the Magellanic
Clouds. I. Photometric candidate identification. Astrophysical Journal.
IOP Publishing. https://doi.org/10.3847/1538-4357/ad778a
chicago: O’Grady, Anna J.G., Maria R. Drout, Kathryn F. Neugent, Bethany Ludwig,
Ylva Louise Linsdotter Götberg, and B. M. Gaensler. “Binary Yellow Supergiants
in the Magellanic Clouds. I. Photometric Candidate Identification.” Astrophysical
Journal. IOP Publishing, 2024. https://doi.org/10.3847/1538-4357/ad778a.
ieee: A. J. G. O’Grady, M. R. Drout, K. F. Neugent, B. Ludwig, Y. L. L. Götberg,
and B. M. Gaensler, “Binary yellow supergiants in the Magellanic Clouds. I. Photometric
candidate identification,” Astrophysical Journal, vol. 975. IOP Publishing,
2024.
ista: O’Grady AJG, Drout MR, Neugent KF, Ludwig B, Götberg YLL, Gaensler BM. 2024.
Binary yellow supergiants in the Magellanic Clouds. I. Photometric candidate identification.
Astrophysical Journal. 975, 29.
mla: O’Grady, Anna J. G., et al. “Binary Yellow Supergiants in the Magellanic Clouds.
I. Photometric Candidate Identification.” Astrophysical Journal, vol. 975,
29, IOP Publishing, 2024, doi:10.3847/1538-4357/ad778a.
short: A.J.G. O’Grady, M.R. Drout, K.F. Neugent, B. Ludwig, Y.L.L. Götberg, B.M.
Gaensler, Astrophysical Journal 975 (2024).
date_created: 2024-11-10T23:01:59Z
date_published: 2024-11-01T00:00:00Z
date_updated: 2025-09-08T14:37:18Z
day: '01'
ddc:
- '520'
department:
- _id: YlGo
doi: 10.3847/1538-4357/ad778a
external_id:
arxiv:
- '2406.17177'
isi:
- '001339486900001'
file:
- access_level: open_access
checksum: 0e9bb88b5048ecc782ac27953c84b8ce
content_type: application/pdf
creator: dernst
date_created: 2024-11-11T09:20:45Z
date_updated: 2024-11-11T09:20:45Z
file_id: '18535'
file_name: 2024_AstrophysicalJour_Grady.pdf
file_size: 34634395
relation: main_file
success: 1
file_date_updated: 2024-11-11T09:20:45Z
has_accepted_license: '1'
intvolume: ' 975'
isi: 1
language:
- iso: eng
month: '11'
oa: 1
oa_version: Published Version
publication: Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Binary yellow supergiants in the Magellanic Clouds. I. Photometric candidate
identification
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 975
year: '2024'
...