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Binarity at LOw Metallicity (BLOeM): Pipeline-Determined Physical Properties of OB Stars

T0 review · 3 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read This paper reports that among 778 OB stars in the Small Magellanic Cloud, stars classified as single from the first nine survey epochs rotate at a median 78 km/s, binaries at 200 km/s, and apparently single O stars show a bimodal rotation…

desk verdict A genuinely useful SMC OB catalog whose headline rotation dichotomy is still a pipeline-level trend—valuable, but the abstract overreaches. read the letter →

arxiv 2506.00117 v2 pith:BBD5OMOF submitted 2025-05-30 astro-ph.SR astro-ph.GA

J. M. Bestenlehner , Paul A. Crowther , V. A. Bronner , S. Simon-Diaz , D. J. Lennon , J. Bodensteiner , N. Langer , P. Marchant
show 3 more authors
H. Sana F. R. N. Schneider T. Shenar
This is my paper
classification astro-ph.SRastro-ph.GA
keywords OBstarsSmallMagellanicCloudstellarrotationspectroscopicbinariesmulti-epochspectroscopyFASTWINDatmospheremodelsmassivestarevolution
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper aims to convert the first nine epochs of the BLOeM multi-epoch survey of massive OB stars in the Small Magellanic Cloud into a homogeneous set of physical parameters using an automated spectral-fitting pipeline. It determines effective temperatures, surface gravities, luminosities, projected rotational velocities, masses, and ages for 778 stars, and finds that rotation is strongly tied to whether a star is classified as single or binary. The median projected rotation is 78 km/s for apparent singles and 200 km/s for binaries, and the single O stars appear to show a bimodal distribution. A sympathetic reading takes this as evidence that at roughly one-fifth solar metallicity, binarity is a decisive factor in how fast massive stars rotate, which matters because rotation changes a star's mixing, wind, and final fate.

What carries the argument

The load-bearing object is a dedicated spectroscopic pipeline that fits co-added FLAMES spectra in the 3950-4550 Angstrom range with a grid of FASTWIND synthetic spectra at SMC metallicity ($0.2\,Z_\odot$), minimising $\chi^2$ over effective temperature, surface gravity, wind strength, and helium abundance while treating rotation as additional line broadening beyond a fixed macro-turbulence. The pipeline includes a model-error term so that imperfections in the synthetic spectra are budgeted into the uncertainties, and it gives extra weight to the Si IV 4089 line to remove a temperature degeneracy near 25 kK. The single/binary classification that feeds the rotation comparison is based on peak-to-peak radial velocity variations of at least 20 km/s at $4\sigma$ significance across the first nine epochs.

What would settle it

Re-run the same rotation analysis on the full 25-epoch BLOeM dataset with orbit-based binary classifications: if the 78 versus 200 km/s median gap between securely single and securely binary OB stars collapses, or the single-O-star bimodality disappears, the central claim is refuted. A complementary check is high-resolution spectroscopy of a subset of these stars: if the contrast is mostly an artefact of the 48 km/s instrumental broadening and the assumed 20 km/s macroturbulence, the claim fails.

Watch

Extended reading notes

Core claim

On the paper's own terms, the discovery is that the $v_\mathrm{e}\sin i$ distributions of OB stars in the SMC are sharply separated by multiplicity: spectroscopic binaries peak near 200 km/s while stars labelled single cluster near 78 km/s. Among O-type stars judged single, the histogram shows a slow and a fast component, and the paper presents this as a low-metallicity analogue of the bimodal rotation distribution previously seen in single early B stars in the Tarantula region. The same analysis recovers the $8\,M_\odot$ lower mass cutoff built into the target selection, gives median evolutionary masses of $12.6\,M_\odot$ for B stars and $19.8\,M_\odot$ for O stars, and finds spectroscopic masses systematically above evolutionary masses, albeit with large surface-gravity uncertainties.

Load-bearing premise

The single/binary split rests on only the first nine epochs of radial-velocity monitoring, flagging binaries by peak-to-peak variations of at least 20 km/s at 4-sigma; the paper itself says the true multiplicity fraction is 'doubtless higher' and calls the single-star categorisation preliminary.

Editorial extensions

If this is right

  • If the rotation dichotomy is real, close binarity is a dominant determinant of rotation among metal-poor massive stars, so population models must treat single and binary channels separately instead of adopting one rotation distribution.
  • The apparent bimodality among single O stars suggests the birth spin distribution at low metallicity is bimodal; because stellar winds are weak at $0.2\,Z_\odot$, both modes survive without being spun down.
  • With half of the 159 BLOeM O stars newly classified as O type, the updated census changes population context: BLOeM covers roughly one-third of the known O-star systems in the SMC, and 17 of its stars supply over 40% of the sample's Lyman-continuum ionizing output.
  • The automated pipeline makes it practical to derive consistent parameters for more than 90% of a large multi-epoch survey, which is the basis for future mass and IMF studies once all epochs are complete.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Beyond the paper: the 'single' sample almost certainly contains undetected longer-period binaries because it uses only nine epochs; if those hidden binaries are mostly fast rotators the true single median could be even lower, strengthening the dichotomy, but if they are slow the gap could narrow.
  • Beyond the paper: the fixed macro-turbulent broadening of 20 km/s and the 48 km/s instrumental resolution likely inflate measured $v_\mathrm{e}\sin i$, so the absolute numbers may shift in a dedicated high-resolution rotation study, although the single-binary gap should persist.
  • Beyond the paper: if the fast mode among single O stars is real, it should leave observable traces such as nitrogen surface enrichment from rotational mixing, which can be tested with abundance maps of the sample.
  • Beyond the paper: the contrast with earlier LMC results, where binary primaries resembled single stars in rotation, predicts a metallicity sequence in which stronger winds at higher metallicity erase the slow/fast dichotomy; extending this pipeline to other metallicities would test that prediction.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. The manuscript applies a spectroscopic pipeline based on FASTWIND model grids to the co-added first nine epochs of the BLOeM VLT/FLAMES survey, deriving Teff, log g, log L/Lsun, helium abundances, projected rotational velocities, spectroscopic and evolutionary masses, and ages for 778 OB stars in the SMC. The headline results are (i) a claimed bimodality in v sin i for single O stars and a striking difference between single (median 78 km/s) and binary (median 200 km/s) OB stars, (ii) broad agreement of pipeline temperatures and rotational velocities with literature and with independent iacob tools, (iii) recovery of the survey-design lower mass cutoff near 8 Msun via Bayesian inference with SMC evolutionary models, and (iv) an updated catalogue of SMC O stars. The paper is candid about several systematics, but the central rotation claim is presented in the abstract more strongly than the acknowledged caveats support.

Significance. If the rotation dichotomy survives a more careful treatment of binarity and line broadening, it would be an important result for massive-star formation and evolution at low metallicity. The paper's strengths include a large and relatively homogeneous SMC sample, a reproducible pipeline (public code and online spectral fits), quantitative comparisons with iacob-broad and iacob-gbat, and a useful updated census of SMC O stars. However, the main abstract claim depends on exactly the quantities that the paper itself flags as preliminary or systematically biased: the single/binary classification from only nine epochs and the pipeline v sin i values obtained with a fixed macroturbulence. The value of the catalogue and the mass/age analysis is more secure than the rotation dichotomy, but the latter needs additional work before it can be stated as established.

major comments (3)
  1. [Section 2, Section 5.1, Fig. 10, Table 2] The central claim of a striking single-vs-binary rotation difference (78 versus 200 km/s) and of an O-star bimodality rests on multiplicity labels from the initial nine epochs and on pipeline v sin i values. The paper itself states that the true multiplicity fraction is 'doubtless higher' and that stars categorised as single are 'preliminary' (Section 2), and that the sample includes a subset of known SB2s 'likely to artificially boost inferred rotational velocities of binary systems' (Section 5.1). Undetected binaries in the single sample and line-doubling in the binary sample can both inflate the contrast and create or enhance the apparent bimodality. Please re-run the distributions excluding all known SB2/SB3 systems and, if possible, use the full 25-epoch classification, or at least quantify how the single and binary medians and the O-star bimodality change under these cuts.
  2. [Section 3, Section 5.2, Fig. 13] The pipeline v sin i values are not direct rotation measurements: the synthetic grid is convolved with a fixed v_mac = 20 km/s and all additional broadening is attributed to rotation. Section 5.2 admits that pipeline values typically exceed iacob-broad Fourier-transform measurements and that v_mac may be significantly larger than 20 km/s. For example, for BLOeM 1-020 the iacob-broad GOF solution with a non-zero v_mac gives 89 km/s versus the pipeline value of 113 +/- 19 km/s. Because the rotation dichotomy is the abstract's headline, this systematic offset is load-bearing. Please provide a quantitative comparison (bias, scatter, and outliers) against iacob-broad for the full subset, and test the sensitivity of the single/binary medians and the O-star histogram to the choice of v_mac.
  3. [Section 3, Fig. 2, Fig. 5, Section 4.1] The adopted extra weighting of Si IV 4089 changes the effective temperature of a representative B1II star from 23.6 kK to 29.9 kK, and the paper reports an 'unrealistic' spread near B1 and a gap at Teff ~ 25 kK. Since O II 4089 is missing from the FASTWIND line list, part of this weighting compensates for missing physics rather than being a parameter-free choice. This temperature sensitivity propagates into luminosities, radii, spectroscopic masses, and evolutionary masses/ages. Please report how many early B stars shift by more than ~2 kK between the unweighted and weighted solutions and quantify the impact on the derived mass and age distributions, or include O II 4089 in the models and re-fit.
minor comments (5)
  1. [Abstract and Section 2] The abstract should temper 'strikingly different' and 'bimodality' with the preliminary nature of the nine-epoch single-star classification and the acknowledged v sin i systematics; the text in Section 2 already contains the necessary caveats.
  2. [Table 2] The presentation of Table 2 is confusing: the single O-star median (153 km/s) differs substantially from the combined single OB median (78 km/s) quoted in the abstract, and the reader has to infer that the latter is B-star dominated. Please clarify in the text and table that the 78 km/s value is driven by the B-star subsample.
  3. [Section 5.2, Fig. 13] Figure 13 shows that pipeline v sin i values systematically exceed iacob-broad FT values, but no quantitative bias or scatter is reported. Please provide the mean offset, RMS, and number of outliers in the caption or text.
  4. [Table A1] In the row for BLOeM 2-042, the effective radius appears as '1111.5+6.3' with a leading '1' that looks like a typo; please check and correct.
  5. [Section 7.1] The phrase 'we recover the anticipated lower mass cutoff at 8 Msun' should be phrased as a consistency check with the survey selection and the adopted Salpeter IMF prior, rather than an independent recovery, since both the target selection and the prior already encode an 8 Msun threshold.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the 8 Msun cutoff is an acknowledged survey-design check, and the single/binary rotation contrast is an observational trend whose caveats are stated by the authors.

full rationale

The paper's derivations are not circular. Stellar parameters are obtained by fitting FASTWIND synthetic grids to the FLAMES spectra, with model-error treatment described in Bestenlehner et al. (2024); the pipeline does not feed the derived quantities back into the fitting in a way that forces the conclusions. The single/binary classification comes from independent multi-epoch radial-velocity variability (peak-to-peak >=20 km/s at 4 sigma), not from the projected rotational velocity, so the 78 versus 200 km/s median comparison is an observational contrast rather than a definitional identity. The authors explicitly caution that the multiplicity fraction is 'doubtless higher', that single-star classifications are preliminary, and that known SB2s can artificially boost inferred rotational velocities; these are correctness and systematics concerns, not circularity. The only element that superficially resembles a fitted input is the 'recovery' of the 8 Msun lower mass cutoff, but the abstract and Section 7 explicitly label it as 'anticipated' and 'from the survey design', and the paper defers a real IMF determination to future work, making it a consistency check rather than a prediction. Evolutionary masses rely on an in-prep tool by co-author V. Bronner, but the method is described as similar to the external bonnsai code and the paper compares against independent spectroscopic masses and literature; this is a documentation/transparency limitation, not a circular step. The paper is largely self-contained and benchmarked against iacob-gbat, iacob-broad, and prior literature, so no load-bearing claim reduces by construction to its own inputs.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The analysis introduces no new physical entities. The principal burdens are the adopted stellar atmosphere grid, the fixed broadening parameters (v_mac = 20 km/s, v_mic = 10 km/s), the hand-chosen Si IV 4089 weighting, and the evolutionary model priors used for masses. The unpublished Bayesian mass tool is an additional external dependency.

free parameters (4)
  • v_mac = 20 km/s (fixed macroturbulence) = 20 km/s
    Convolved into all synthetic spectra; all additional broadening is attributed to rotation. If true macroturbulence differs, pipeline v_e sin i is biased, acknowledged in Section 5.1.
  • Extra weighting for Si IV 4089 = not quantified (extra points at 4088.85 +/- 0.25 A)
    Adopted after observing an unphysical 25 kK gap in early B star solutions; changes BLOeM 1-005 Teff from 23.6 to 29.9 kK (Fig. 2), so the temperature scale depends on this hand-chosen adjustment.
  • Micro-turbulence v_mic = 10 km/s = 10 km/s
    Fixed in model grids; affects line widths and thus v_e sin i and gravity estimates.
  • Salpeter IMF prior for evolutionary masses = Salpeter slope, alpha = 2.35
    Bayesian mass inference uses a Salpeter IMF prior; the mass and age distributions depend on this prior choice.
assumptions (5)
  • domain assumption FASTWIND non-LTE model atmospheres with SMC metallicity accurately reproduce the BLOeM LR02 optical spectra, including Balmer lines, He I-II, and Si III-IV lines.
    Section 3: pipeline fits grids of FASTWIND spectra; missing O II 4089 is tested only at a few grid points, so broad applicability is assumed.
  • domain assumption Binarity classification from 9 epochs using peak-to-peak RV > 20 km/s at 4 sigma is sufficient to identify 'single' stars for rotation statistics.
    Section 2: authors note true multiplicity is 'doubtless higher' and single stars are 'preliminary'; the single versus binary rotation comparison depends on this classification.
  • domain assumption Initial mass function prior and Brott et al. (2011) rotating evolutionary tracks, together with the unpublished Bronner et al. Bayesian method, provide unbiased masses and ages.
    Section 7.1: evolutionary masses and ages are derived from these models with a Salpeter IMF prior; results depend on the model grid and prior.
  • domain assumption Adopted SMC distance modulus of 18.98 mag and the Maiz Apellaniz reddening law are correct for all targets.
    Section 3: individual luminosities and radii use this distance and reddening law.
  • ad hoc to paper The pipeline's de-idealized model-error covariance, averaged over the whole sample, adequately represents spectral model uncertainties.
    Section 3: 'model-error is averaged over the entire parameter space of our sample. This impacted overall performance'.

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Cite this review

Pith. "Pith review of Binarity at LOw Metallicity (BLOeM): Pipeline-Determined Physical Properties of OB Stars." pith.science (2026). https://pith.science/paper/BBD5OMOF

@misc{pith2026250600117,
  author       = {Pith},
  title        = {Pith review of: Binarity at LOw Metallicity (BLOeM): Pipeline-Determined Physical Properties of OB Stars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/BBD5OMOF}},
  note         = {Machine review of arXiv:2506.00117}
}
read the original abstract

We aim to determine the physical properties of OB stars from the multi-epoch VLT/FLAMES BLOeM spectroscopic survey of the Small Magellanic Cloud. We apply a pipeline designed to analyse large spectroscopic samples of OB stars to the co-added, initial 9 epochs of the BLOeM survey, utilising grids of synthetic model spectra computed with the stellar atmosphere code FASTWIND. 69 OB stars are excluded from the analysis owing to disk emission or significant contamination by secondaries in SB2 binaries. We determine physical properties of 778 OB stars, including Teff, log g, log L/Lsun and v_e sin i. There appears to be a bimodality in v_e sin i of single O stars, while v_e sin i distributions of OB stars are strikingly different for single (median 78 km/s) and binary (median 200 km/s) systems. Inferred temperatures are broadly in agreement with literature results for stars in common, plus results from a grid-based automization tool for a subset of O and early B stars, although uncertainties are larger for surface gravities. Rotational velocities are broadly in line with an independent tool applied to the same subset. We recover the anticipated lower mass cutoff at 8 Msun from the survey design using a Bayesian inference method coupled with SMC metallicity evolutionary models, with median masses of 12.6 Msun (19.8 Msun) for B-type (O-type) stars. Spectroscopic masses exceed evolutionary masses, albeit with large uncertainties in surface gravities. We also provide an updated catalogue of O stars in the SMC since half of the 159 BLOeM O stars are newly classified as O-type stars.

Figures

Figures reproduced from arXiv: 2506.00117 by the authors.

Figure 1
Figure 1. Radial velocities of single BLOeM OB stars – according to initial 9 epoch dataset – relative to 159 km s−1 average of sample, overlaid on a Herschel SPIRE 350𝜇m map of the SMC (Meixner et al. 2013). Higher radial velocities for OB stars in the wing (south east) has previously been reported by Evans & Howarth (2008). instrument (FLAMES) hindered sampling of crowded environments, such as the NGC 346 star-forming regio… view at source ↗
Figure 2
Figure 2. Comparison between the pipeline fits (red) obtained for BLOeM 1-005 (B1 II, blue) for the unweighted solution (upper panel, 𝑇eff = 23.6 +0.7 −0.8 kK, log 𝑔/(cm s−2 ) = 3.64+0.15 −0.16) versus the solution with additional weight given to Si iv 𝜆4089 (lower panel, 𝑇eff = 29.9 ± 1.2 kK, log 𝑔/(cm s−2 ) = 3.93+0.34 −0.17). It is apparent that both solutions reproduce H i and He i lines plus Si iii 𝜆4553, with the higher… view at source ↗
Figure 3
Figure 3. Comparison between the pipeline fits (red) obtained for visually faint OB stars, from top to bottom: BLOeM 3-004 (O9.7 IV:) for which 𝑇eff = 33.7 +1.5 −2.3 kK, log 𝑔/cm s−2 = 4.12+0.34 −0.43, BLOeM 2-041 (B2: II), for which 𝑇eff = 20.1 +4.7 −2.7 kK, log 𝑔/cm s−2 = 3.30+0.74 −0.40 and BLOeM 6-007 (B5 II), for which 𝑇eff = 15.9±0.8 kK, log 𝑔/cm s−2 = 3.07+0.17 −0.29. The grey shaded area is the square root of the diag… view at source ↗
Figures from the paper (17 more)
Figure 4
Figure 4. Figure 4: Pipeline effective temperatures, 𝑇eff for BLOeM OB stars using spectral types from Shenar et al. (2024). Single stars according to analysis of the initial 9 epochs of BLOeM (Sana et al. 2025; Villaseñor et al. 2025; Britavskiy et al. 2025; Bodensteiner et al. 2025; Pat…
Figure 5
Figure 5. Figure 5: Comparison between adopted 𝑇eff of BLOeM OB stars from SMC calibrations (Shenar et al. 2024) and pipeline-derived, 𝑇eff. Single stars ac￾cording to analysis of the initial 9 epochs of BLOeM (Sana et al. 2025; Vil￾laseñor et al. 2025; Britavskiy et al. 2025; Bodensteine…
Figure 6
Figure 6. Figure 6: Comparison between 𝑇eff for BLOeM OB stars from literature stud￾ies (circles: cmfgen, triangles: fastwind, squares: tlusty) and the current pipeline, colour coded by luminosity class. References are provided in the Appendix in Tables B1-B2. grid interpolation becomes c…
Figure 7
Figure 7. Figure 7: Hertzsprung-Russell diagram of the BLOeM OB sample (colour coded by luminosity class). Open symbols are single according to analysis of the initial 9 epochs of BLOeM (Sana et al. 2025; Villaseñor et al. 2025; Britavskiy et al. 2025; Bodensteiner et al. 2025; Patrick et…
Figure 8
Figure 8. Figure 8: Comparison between effective temperatures, 𝑇eff, and surface grav￾ities, log 𝑔, of BLOeM OB stars (Kiel diagram). Open symbols are single stars according to the initial 9 epochs of BLOeM (Sana et al. 2025; Villaseñor et al. 2025; Britavskiy et al. 2025; Bodensteiner et…
Figure 10
Figure 10. Figure 10: Histogram of projected rotational velocities 𝑣e sin 𝑖 (km s−1 ) of all O (blue) and B stars (green) in the top panel, sorted into 50 km s−1 bins (e.g. 50 km s−1 refers to 50±25 km s−1 ), aside from the 0 bin which refers to 0–25 km s−1 ; Central panel: As above for si…
Figure 11
Figure 11. Figure 11: Hertzsprung-Russell diagram of BLOeM sample (colour coded by 𝑣e sin 𝑖), together with evolutionary tracks for non-rotating SMC massive stars from Brott et al. (2011) [PITH_FULL_IMAGE:figures/full_fig_p010_11.png]
Figure 12
Figure 12. Figure 12: Histogram of projected rotational velocities 𝑣e sin 𝑖 (km s−1 ) of main sequence (dark green) and post-main sequence (pale green) OB stars, according to Brott et al. (2011) rotating models, sorted into 50 km s−1 bins aside for the 0 bin (e.g. 50 km s−1 refers to 50±25…
Figure 13
Figure 13. Figure 13: Comparison between 𝑣e sin 𝑖 for a subset of O (blue triangles) and B (green squares) BLOeM stars from iacob-broad (Simón-Díaz & Herrero 2014) and the spectroscopic pipeline [PITH_FULL_IMAGE:figures/full_fig_p011_13.png]
Figure 14
Figure 14. Figure 14: iacob-broad (Simón-Díaz & Herrero 2014) Fourier Transform (FT) and Goodness-of-Fit (GOF) results for Si iii 𝜆4553 in BLOeM 1-020 (B0 III). gravities and helium abundances (limits for BLOeM 3–090) to be determined in these cases [PITH_FULL_IMAGE:figures/full_fig_p011_…
Figure 15
Figure 15. Figure 15: iacob-gbat hydrogen and helium spectral line fits (black lines) to BLOeM 8–030 (O6.5 Vn), in which selected regions (excluded) are indicated in red (blue). Physical parameters are 𝑇eff = 38.2±0.8 kK, log 𝑔 = 3.82 ± 0.08 and 𝑦 = 0.130 ± 0.023, with 𝑣𝑒 sin 𝑖 = 290 km s−…
Figure 16
Figure 16. Figure 16: iacob-gbat hydrogen and helium spectral line fits (black lines) to BLOeM 3–090 (B0.2 Ia), in which selected regions (excluded) are indicated in red (blue). Physical parameters are 𝑇eff = 28.0±1.1 kK, log 𝑔 = 3.19 ± 0.21 and 𝑦 < 0.06+2.3 , with 𝑣𝑒 sin 𝑖 = 74 km s−1 (fr…
Figure 18
Figure 18. Figure 18: Histogram of (logarithmic) current masses (𝑀⊙) of BLOeM O (blue) and B (green) stars, with O stars dominant for log 𝑀evol/𝑀⊙ ≥ 1.35 ± 0.05 and B stars dominant for log 𝑀evol/𝑀⊙ ≤ 1.15 ± 0.05. Masses are based on Brott et al. (2011) rotating evolutionary models, plus H…
Figure 17
Figure 17. Figure 17: Comparison between iacob-gbat (Simón-Díaz et al. 2011) and pipeline effective temperatures for a subset of O (blue triangles) and B (green squares) BLOeM stars (top panel). Middle and lower panels: As above for log 𝑔 and helium mass fraction, 𝑌, respectively. 𝑌=0.25 i…
Figure 19
Figure 19. Figure 19: Comparison between (current) evolutionary masses and spectroscopic masses of BLOeM OB stars, based on Brott et al. (2011) rotating models, plus Hastings et al. (2021) evolutionary models for two luminous O supergiants above the upper mass limit of the Brott et al. (20…
Figure 20
Figure 20. Figure 20: Histogram of (logarithmic) ages (in Myr) of BLOeM O (blue) and B (green) stars, based on Brott et al. (2011) rotating evolutionary models, plus Hastings et al. (2021) evolutionary models for two luminous O supergiants. binary evolution can rejuvenate mass gainers, giv…
Figure 21
Figure 21. Figure 21: Ages of BLOeM OB stars, overlaid on a Herschel SPIRE 350𝜇m map of the SMC (Meixner et al. 2013). Field 8 (upper right) hosts OB stars with the highest median age (13.1 Myr) with the remainder in the range 7.7–11 Myr. O9.5 or B0, so the updated catalogue of SMC O stars…

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Works this paper leans on

144 extracted references · 36 canonical work pages

  1. [1]

    P., et al., 2016, @doi [Physical Review X] 10.1103/PhysRevX.6.041015 , https://ui.adsabs.harvard.edu/abs/2016PhRvX...6d1015A 6, 041015

    Abbott B. P., et al., 2016, @doi [Physical Review X] 10.1103/PhysRevX.6.041015 , https://ui.adsabs.harvard.edu/abs/2016PhRvX...6d1015A 6, 041015

    doi:10.1103/physrevx.6.041015 2016

  2. [2]

    Antoniou V., Hatzidimitriou D., Zezas A., Reig P., 2009, @doi [ ] 10.1088/0004-637X/707/2/1080 , https://ui.adsabs.harvard.edu/abs/2009ApJ...707.1080A 707, 1080

    doi:10.1088/0004-637x/707/2/1080 2009

  3. [3]

    Ardeberg A., Maurice E., 1977, , https://ui.adsabs.harvard.edu/abs/1977A&AS...30..261A 30, 261

    1977

  4. [4]

    Azzopardi M., Vigneau J., Macquet M., 1975, , https://ui.adsabs.harvard.edu/abs/1975A&AS...22..285A 22, 285

    1975

  5. [5]

    R., Butler K., 1988, , https://ui.adsabs.harvard.edu/abs/1988A&A...201..232B 201, 232

    Becker S. R., Butler K., 1988, , https://ui.adsabs.harvard.edu/abs/1988A&A...201..232B 201, 232

    1988

  6. [6]

    R., Butler K., 1990, , https://ui.adsabs.harvard.edu/abs/1990A&A...235..326B 235, 326

    Becker S. R., Butler K., 1990, , https://ui.adsabs.harvard.edu/abs/1990A&A...235..326B 235, 326

    1990

  7. [7]

    M., En lin T., Bergemann M., Crowther P

    Bestenlehner J. M., En lin T., Bergemann M., Crowther P. A., Greiner M., Selig M., 2024, @doi [ ] 10.1093/mnras/stae298 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.528.6735B 528, 6735

    work page doi:10.1093/mnras/stae298 2024

  8. [8]

    M., Crowther P

    Bestenlehner J. M., Crowther P. A., Hawcroft C., Sana H., Tramper F., Vink J. S., Brands S. A., Sander A. A. C., 2025, @doi [ ] 10.1051/0004-6361/202452491 , https://ui.adsabs.harvard.edu/abs/2025A&A...695A.198B 695, A198

    doi:10.1051/0004-6361/202452491 2025

Show all 144 references
  1. [9]

    et al., 2025, @doi [ ], https://ui.adsabs.harvard.edu/abs/2025arXiv250202641B 698, A38

    Bodensteiner J., Shenar T., Sana H. et al., 2025, @doi [ ], https://ui.adsabs.harvard.edu/abs/2025arXiv250202641B 698, A38

    2025

  2. [10]

    Z., et al., 2010, @doi [ ] 10.1088/0004-6256/140/2/416 , https://ui.adsabs.harvard.edu/abs/2010AJ....140..416B 140, 416

    Bonanos A. Z., et al., 2010, @doi [ ] 10.1088/0004-6256/140/2/416 , https://ui.adsabs.harvard.edu/abs/2010AJ....140..416B 140, 416

    2010 doi

  3. [11]

    C., Lanz T., Martins F., Marcolino W

    Bouret J. C., Lanz T., Martins F., Marcolino W. L. F., Hillier D. J., Depagne E., Hubeny I., 2013, @doi [ ] 10.1051/0004-6361/201220798 , https://ui.adsabs.harvard.edu/abs/2013A&A...555A...1B 555, A1

    2013 doi

  4. [12]

    C., Martins F., Hillier D

    Bouret J. C., Martins F., Hillier D. J., Marcolino W. L. F., Rocha-Pinto H. J., Georgy C., Lanz T., Hubeny I., 2021, @doi [ ] 10.1051/0004-6361/202039890 , https://ui.adsabs.harvard.edu/abs/2021A&A...647A.134B 647, A134

    2021 doi

  5. [13]

    A., et al., 2022, @doi [ ] 10.1051/0004-6361/202142742 , https://ui.adsabs.harvard.edu/abs/2022A&A...663A..36B 663, A36

    Brands S. A., et al., 2022, @doi [ ] 10.1051/0004-6361/202142742 , https://ui.adsabs.harvard.edu/abs/2022A&A...663A..36B 663, A36

    2022 doi

  6. [14]

    J., et al., 2025, @doi [ ], https://ui.adsabs.harvard.edu/abs/2025arXiv250212239B 698, A40

    Britavskiy N., Mahy L., Lennon D. J., et al., 2025, @doi [ ], https://ui.adsabs.harvard.edu/abs/2025arXiv250212239B 698, A40

    2025

  7. [15]

    Brott I., et al., 2011, @doi [ ] 10.1051/0004-6361/201016113 , https://ui.adsabs.harvard.edu/abs/2011A&A...530A.115B 530, A115

    2011 doi

  8. [16]

    Cantiello M., et al., 2009, @doi [ ] 10.1051/0004-6361/200911643 , https://ui.adsabs.harvard.edu/abs/2009A&A...499..279C 499, 279

    2009 doi

  9. [17]

    Castro N., Fossati L., Langer N., Sim \'o n-D \' az S., Schneider F. R. N., Izzard R. G., 2014, @doi [ ] 10.1051/0004-6361/201425028 , https://ui.adsabs.harvard.edu/abs/2014A&A...570L..13C 570, L13

    2014 doi

  10. [18]

    S., Fossati L., Langer N., 2018, @doi [ ] 10.3847/1538-4357/aae6d0 , https://ui.adsabs.harvard.edu/abs/2018ApJ...868...57C 868, 57

    Castro N., Oey M. S., Fossati L., Langer N., 2018, @doi [ ] 10.3847/1538-4357/aae6d0 , https://ui.adsabs.harvard.edu/abs/2018ApJ...868...57C 868, 57

    2018 doi

  11. [19]

    Cioni M. R. L., et al., 2011, @doi [ ] 10.1051/0004-6361/201016137 , https://ui.adsabs.harvard.edu/abs/2011A&A...527A.116C 527, A116

    2011 doi

  12. [20]

    Cioni M. R. L., et al., 2019, @doi [The Messenger] 10.18727/0722-6691/5128 , https://ui.adsabs.harvard.edu/abs/2019Msngr.175...54C 175, 54

    2019 doi

  13. [21]

    L., Polcaro V

    Covino S., Negueruela I., Campana S., Israel G. L., Polcaro V. F., Stella L., Verrecchia F., 2001, @doi [ ] 10.1051/0004-6361:20010773 , https://ui.adsabs.harvard.edu/abs/2001A&A...374.1009C 374, 1009

    2001 doi

  14. [22]

    Crampton D., Greasley J., 1982, @doi [ ] 10.1086/130936 , https://ui.adsabs.harvard.edu/abs/1982PASP...94...31C 94, 31

    1982 doi

  15. [23]

    A., et al., 2016, @doi [ ] 10.1093/mnras/stw273 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.458..624C 458, 624

    Crowther P. A., et al., 2016, @doi [ ] 10.1093/mnras/stw273 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.458..624C 458, 624

    2016 doi

  16. [24]

    A., Puls J., 2024, @doi [ ] 10.1051/0004-6361/202348808 , https://ui.adsabs.harvard.edu/abs/2024A&A...687A.228D 687, A228

    de Burgos A., Sim \'o n-D \' az S., Urbaneja M. A., Puls J., 2024, @doi [ ] 10.1051/0004-6361/202348808 , https://ui.adsabs.harvard.edu/abs/2024A&A...687A.228D 687, A228

    2024 doi

  17. [25]

    A., Holgado G., Ekstr \"o m S., Ram \' rez-Tannus M

    de Burgos A., Sim \'o n-D \' az S., Urbaneja M. A., Holgado G., Ekstr \"o m S., Ram \' rez-Tannus M. C., Zari E., 2025, @doi [ ] 10.1051/0004-6361/202453242 , https://ui.adsabs.harvard.edu/abs/2025A&A...695A..87D 695, A87

    2025 doi

  18. [26]

    E., Sana H., Langer N., Izzard R

    de Mink S. E., Sana H., Langer N., Izzard R. G., Schneider F. R. N., 2014, @doi [ ] 10.1088/0004-637X/782/1/7 , https://ui.adsabs.harvard.edu/abs/2014ApJ...782....7D 782, 7

    2014 doi

  19. [27]

    O., Moens N., Van der Sijpt C., Verhamme O., Poniatowski L

    Debnath D., Sundqvist J. O., Moens N., Van der Sijpt C., Verhamme O., Poniatowski L. G., 2024, @doi [ ] 10.1051/0004-6361/202348206 , https://ui.adsabs.harvard.edu/abs/2024A&A...684A.177D 684, A177

    2024 doi

  20. [28]

    I., et al., 2013, @doi [ ] 10.1051/0004-6361/201321824 , https://ui.adsabs.harvard.edu/abs/2013A&A...558A.134D 558, A134

    Doran E. I., et al., 2013, @doi [ ] 10.1051/0004-6361/201321824 , https://ui.adsabs.harvard.edu/abs/2013A&A...558A.134D 558, A134

    2013 doi

  21. [29]

    L., et al., 2013, @doi [ ] 10.1051/0004-6361/201220273 , https://ui.adsabs.harvard.edu/abs/2013A&A...550A.109D 550, A109

    Dufton P. L., et al., 2013, @doi [ ] 10.1051/0004-6361/201220273 , https://ui.adsabs.harvard.edu/abs/2013A&A...550A.109D 550, A109

    2013 doi

  22. [30]

    L., et al., 2018, @doi [ ] 10.1051/0004-6361/2001732440 , https://ui.adsabs.harvard.edu/abs/2018A&A...615A.101D 615, A101

    Dufton P. L., et al., 2018, @doi [ ] 10.1051/0004-6361/2001732440 , https://ui.adsabs.harvard.edu/abs/2018A&A...615A.101D 615, A101

    2018 doi

  23. [31]

    L., Evans C

    Dufton P. L., Evans C. J., Hunter I., Lennon D. J., Schneider F. R. N., 2019, @doi [ ] 10.1051/0004-6361/201935415 , https://ui.adsabs.harvard.edu/abs/2019A&A...626A..50D 626, A50

    2019 doi

  24. [33]

    J., Howarth I

    Evans C. J., Howarth I. D., Irwin M. J., Burnley A. W., Harries T. J., 2004a, @doi [ ] 10.1111/j.1365-2966.2004.08096.x , https://ui.adsabs.harvard.edu/abs/2004MNRAS.353..601E 353, 601

    2004

  25. [34]

    J., Crowther P

    Evans C. J., Crowther P. A., Fullerton A. W., Hillier D. J., 2004b, @doi [ ] 10.1086/421769 , https://ui.adsabs.harvard.edu/abs/2004ApJ...610.1021E 610, 1021

    doi

  26. [35]

    J., Lennon D

    Evans C. J., Lennon D. J., Smartt S. J., Trundle C., 2006, @doi [ ] 10.1051/0004-6361:20064988 , https://ui.adsabs.harvard.edu/abs/2006A&A...456..623E 456, 623

    2006 doi

  27. [36]

    J., et al., 2011, @doi [ ] 10.1051/0004-6361/201116782 , https://ui.adsabs.harvard.edu/abs/2011A&A...530A.108E 530, A108

    Evans C. J., et al., 2011, @doi [ ] 10.1051/0004-6361/201116782 , https://ui.adsabs.harvard.edu/abs/2011A&A...530A.108E 530, A108

    2011 doi

  28. [37]

    J., et al., 2012, @doi [ ] 10.1088/0004-637X/753/2/173 , https://ui.adsabs.harvard.edu/abs/2012ApJ...753..173E 753, 173

    Evans C. J., et al., 2012, @doi [ ] 10.1088/0004-637X/753/2/173 , https://ui.adsabs.harvard.edu/abs/2012ApJ...753..173E 753, 173

    2012 doi

  29. [39]

    Gaia Collaboration et al., 2021, @doi [ ] 10.1051/0004-6361/202039657 , https://ui.adsabs.harvard.edu/abs/2021A&A...649A...1G 649, A1

    2021 doi

  30. [40]

    D., Conti P

    Garmany C. D., Conti P. S., Massey P., 1987, @doi [ ] 10.1086/114391 , https://ui.adsabs.harvard.edu/abs/1987AJ.....93.1070G 93, 1070

    1987 doi

  31. [41]

    Geen S., et al., 2023, @doi [ ] 10.1088/1538-3873/acb6b5 , https://ui.adsabs.harvard.edu/abs/2023PASP..135b1001G 135, 021001

    2023 doi

  32. [42]

    B., 2009, @doi [ ] 10.1146/annurev.astro.46.060407.145147 , https://ui.adsabs.harvard.edu/abs/2009ARA&A..47..567G 47, 567

    Gehrels N., Ramirez-Ruiz E., Fox D. B., 2009, @doi [ ] 10.1146/annurev.astro.46.060407.145147 , https://ui.adsabs.harvard.edu/abs/2009ARA&A..47..567G 47, 567

    2009

  33. [43]

    D., et al., 2024, @doi [ ] 10.3847/1538-4357/ad4be1 , https://ui.adsabs.harvard.edu/abs/2024ApJ...970...51G 970, 51

    Gordon K. D., et al., 2024, @doi [ ] 10.3847/1538-4357/ad4be1 , https://ui.adsabs.harvard.edu/abs/2024ApJ...970...51G 970, 51

    2024 doi

  34. [44]

    Graczyk D., et al., 2020, @doi [ ] 10.3847/1538-4357/abbb2b , https://ui.adsabs.harvard.edu/abs/2020ApJ...904...13G 904, 13

    2020 doi

  35. [45]

    Hardorp J., Scholz M., 1970, , https://ui.adsabs.harvard.edu/abs/1970ApJS...19..193H 19, 193

    1970

  36. [46]

    P., 2021, @doi [ ] 10.1051/0004-6361/202141269 , https://ui.adsabs.harvard.edu/abs/2021A&A...653A.144H 653, A144

    Hastings B., Langer N., Wang C., Schootemeijer A., Milone A. P., 2021, @doi [ ] 10.1051/0004-6361/202141269 , https://ui.adsabs.harvard.edu/abs/2021A&A...653A.144H 653, A144

    2021 doi

  37. [47]

    P., Vilchez J

    Herrero A., Kudritzki R. P., Vilchez J. M., Kunze D., Butler K., Haser S., 1992, , https://ui.adsabs.harvard.edu/abs/1992A&A...261..209H 261, 209

    1992

  38. [48]

    Heydari-Malayeri M., Selier R., 2010, @doi [ ] 10.1051/0004-6361/201014230 , https://ui.adsabs.harvard.edu/abs/2010A&A...517A..39H 517, A39

    2010 doi

  39. [49]

    R., Zinnecker H., Deharveng L., Charmandaris V., 1999a, @doi [ ] 10.48550/arXiv.astro-ph/9901270 , https://ui.adsabs.harvard.edu/abs/1999A&A...344..848H 344, 848

    Heydari-Malayeri M., Rosa M. R., Zinnecker H., Deharveng L., Charmandaris V., 1999a, @doi [ ] 10.48550/arXiv.astro-ph/9901270 , https://ui.adsabs.harvard.edu/abs/1999A&A...344..848H 344, 848

    doi arXiv

  40. [50]

    R., Zinnecker H., 1999b, @doi [ ] 10.48550/arXiv.astro-ph/9904308 , https://ui.adsabs.harvard.edu/abs/1999A&A...347..841H 347, 841

    Heydari-Malayeri M., Charmandaris V., Deharveng L., Rosa M. R., Zinnecker H., 1999b, @doi [ ] 10.48550/arXiv.astro-ph/9904308 , https://ui.adsabs.harvard.edu/abs/1999A&A...347..841H 347, 841

    doi arXiv

  41. [51]

    W., Howarth I

    Hilditch R. W., Howarth I. D., Harries T. J., 2005, @doi [ ] 10.1111/j.1365-2966.2005.08653.x , https://ui.adsabs.harvard.edu/abs/2005MNRAS.357..304H 357, 304

    2005

  42. [52]

    J., Miller D

    Hillier D. J., Miller D. L., 1998, @doi [ ] 10.1086/305350 , https://ui.adsabs.harvard.edu/abs/1998ApJ...496..407H 496, 407

    1998 doi

  43. [53]

    J., Lanz T., Heap S

    Hillier D. J., Lanz T., Heap S. R., Hubeny I., Smith L. J., Evans C. J., Lennon D. J., Bouret J. C., 2003, @doi [ ] 10.1086/374329 , https://ui.adsabs.harvard.edu/abs/2003ApJ...588.1039H 588, 1039

    2003 doi

  44. [54]

    Holgado G., et al., 2018, @doi [ ] 10.1051/0004-6361/201731543 , https://ui.adsabs.harvard.edu/abs/2018A&A...613A..65H 613, A65

    2018 doi

  45. [55]

    Holgado G., et al., 2020, @doi [ ] 10.1051/0004-6361/202037699 , https://ui.adsabs.harvard.edu/abs/2020A&A...638A.157H 638, A157

    2020 doi

  46. [56]

    H., 2022, @doi [ ] 10.1051/0004-6361/202243851 , https://ui.adsabs.harvard.edu/abs/2022A&A...665A.150H 665, A150

    Holgado G., Sim \'o n-D \' az S., Herrero A., Barb \'a R. H., 2022, @doi [ ] 10.1051/0004-6361/202243851 , https://ui.adsabs.harvard.edu/abs/2022A&A...665A.150H 665, A150

    2022 doi

  47. [57]

    Hubeny I., Lanz T., 1995, @doi [ ] 10.1086/175226 , https://ui.adsabs.harvard.edu/abs/1995ApJ...439..875H 439, 875

    1995 doi

  48. [58]

    Hunter I., et al., 2007, @doi [ ] 10.1051/0004-6361:20066148 , https://ui.adsabs.harvard.edu/abs/2007A&A...466..277H 466, 277

    2007 doi

  49. [59]

    Hunter I., et al., 2008, @doi [ ] 10.1051/0004-6361:20078511 , https://ui.adsabs.harvard.edu/abs/2008A&A...479..541H 479, 541

    2008 doi

  50. [60]

    B., Thompson I

    Hutchings J. B., Thompson I. B., 1988, @doi [ ] 10.1086/166553 , https://ui.adsabs.harvard.edu/abs/1988ApJ...331..294H 331, 294

    1988 doi

  51. [61]

    Kennicutt Jr. R. C., Lee J. C., Funes J. G., J. S., Sakai S., Akiyama S., 2008, @doi [ ] 10.1086/590058 , https://ui.adsabs.harvard.edu/abs/2008ApJS..178..247K 178, 247

    2008 doi

  52. [62]

    E., 1991, , https://ui.adsabs.harvard.edu/abs/1991A&AS...88..101K 88, 101

    Kilian J., Montenbruck O., Nissen P. E., 1991, , https://ui.adsabs.harvard.edu/abs/1991A&AS...88..101K 88, 101

    1991

  53. [63]

    B., Oey M

    Lamb J. B., Oey M. S., Segura-Cox D. M., Graus A. S., Kiminki D. C., Golden-Marx J. B., Parker J. W., 2016, @doi [ ] 10.3847/0004-637X/817/2/113 , https://ui.adsabs.harvard.edu/abs/2016ApJ...817..113L 817, 113

    2016 doi

  54. [64]

    M., 1961, @doi [ ] 10.1086/108396 , https://ui.adsabs.harvard.edu/abs/1961AJ.....66..169L 66, 169

    Lindsay E. M., 1961, @doi [ ] 10.1086/108396 , https://ui.adsabs.harvard.edu/abs/1961AJ.....66..169L 66, 169

    1961 doi

  55. [65]

    Mahy L., et al., 2020, @doi [ ] 10.1051/0004-6361/201936151 , https://ui.adsabs.harvard.edu/abs/2020A&A...634A.118M 634, A118

    2020 doi

  56. [66]

    Ma \' z Apell \'a niz J., et al., 2014, @doi [ ] 10.1051/0004-6361/201423439 , https://ui.adsabs.harvard.edu/abs/2014A&A...564A..63M 564, A63

    2014 doi

  57. [67]

    Marchant P., 2017, PhD thesis, Rheinische Friedrich Wilhelms University of Bonn, Germany, https://bonndoc.ulb.uni-bonn.de/xmlui/handle/20.500.11811/7507

    2017

  58. [68]

    M., Floquet M., Zorec J., Neiner C., 2007, @doi [ ] 10.1051/0004-6361:20065076 , https://ui.adsabs.harvard.edu/abs/2007A&A...462..683M 462, 683

    Martayan C., Fr \'e mat Y., Hubert A. M., Floquet M., Zorec J., Neiner C., 2007, @doi [ ] 10.1051/0004-6361:20065076 , https://ui.adsabs.harvard.edu/abs/2007A&A...462..683M 462, 683

    2007 doi

  59. [69]

    Mart \' nez-Sebasti \'a n C., Sim \'o n-D \' az S., Jin H., Keszthelyi Z., Holgado G., Langer N., Puls J., 2025, @doi [ ] 10.1051/0004-6361/202452622 , https://ui.adsabs.harvard.edu/abs/2025A&A...693L..10M 693, L10

    2025 doi

  60. [70]

    J., Heydari-Malayeri M., 2004, @doi [ ] 10.1051/0004-6361:20034509 , https://ui.adsabs.harvard.edu/abs/2004A&A...420.1087M 420, 1087

    Martins F., Schaerer D., Hillier D. J., Heydari-Malayeri M., 2004, @doi [ ] 10.1051/0004-6361:20034509 , https://ui.adsabs.harvard.edu/abs/2004A&A...420.1087M 420, 1087

    2004 doi

  61. [71]

    Martins F., et al., 2024, @doi [A&A] 10.1051/0004-6361/202449457 , 689, A31

    2024 doi

  62. [72]

    Massey P., 2002, @doi [ ] 10.1086/338286 , https://ui.adsabs.harvard.edu/abs/2002ApJS..141...81M 141, 81

    2002 doi

  63. [73]

    S., 2001, @doi [ ] 10.1086/319818 , https://ui.adsabs.harvard.edu/abs/2001ApJ...550..713M 550, 713

    Massey P., Duffy A. S., 2001, @doi [ ] 10.1086/319818 , https://ui.adsabs.harvard.edu/abs/2001ApJ...550..713M 550, 713

    2001 doi

  64. [74]

    W., Garmany C

    Massey P., Parker J. W., Garmany C. D., 1989, @doi [ ] 10.1086/115217 , https://ui.adsabs.harvard.edu/abs/1989AJ.....98.1305M 98, 1305

    1989 doi

  65. [75]

    Massey P., Waterhouse E., DeGioia-Eastwood K., 2000, @doi [ ] 10.1086/301345 , https://ui.adsabs.harvard.edu/abs/2000AJ....119.2214M 119, 2214

    2000 doi

  66. [76]

    P., Puls J., Pauldrach A

    Massey P., Bresolin F., Kudritzki R. P., Puls J., Pauldrach A. W. A., 2004, @doi [ ] 10.1086/420766 , https://ui.adsabs.harvard.edu/abs/2004ApJ...608.1001M 608, 1001

    2004 doi

  67. [77]

    Massey P., Puls J., Pauldrach A. W. A., Bresolin F., Kudritzki R. P., Simon T., 2005, @doi [ ] 10.1086/430417 , https://ui.adsabs.harvard.edu/abs/2005ApJ...627..477M 627, 477

    2005 doi

  68. [78]

    M., Morrell N

    Massey P., Zangari A. M., Morrell N. I., Puls J., DeGioia-Eastwood K., Bresolin F., Kudritzki R.-P., 2009, @doi [ ] 10.1088/0004-637X/692/1/618 , https://ui.adsabs.harvard.edu/abs/2009ApJ...692..618M 692, 618

    2009 doi

  69. [79]

    F., Morrell N., Hillier D

    Massey P., Neugent K. F., Morrell N., Hillier D. J., 2014, @doi [ ] 10.1088/0004-637X/788/1/83 , https://ui.adsabs.harvard.edu/abs/2014ApJ...788...83M 788, 83

    2014 doi

  70. [80]

    A., Coe M

    McBride V. A., Coe M. J., Negueruela I., Schurch M. P. E., McGowan K. E., 2008, @doi [ ] 10.1111/j.1365-2966.2008.13410.x , https://ui.adsabs.harvard.edu/abs/2008MNRAS.388.1198M 388, 1198

    2008

  71. [81]

    Meixner M., et al., 2013, @doi [ ] 10.1088/0004-6256/146/3/62 , https://ui.adsabs.harvard.edu/abs/2013AJ....146...62M 146, 62

    2013 doi

  72. [82]

    W., Massey P., Morrell N

    Melena N. W., Massey P., Morrell N. I., Zangari A. M., 2008, @doi [ ] 10.1088/0004-6256/135/3/878 , https://ui.adsabs.harvard.edu/abs/2008AJ....135..878M 135, 878

    2008 doi

  73. [83]

    Menon A., et al., 2024, @doi [ ] 10.3847/2041-8213/ad2074 , https://ui.adsabs.harvard.edu/abs/2024ApJ...963L..42M 963, L42

    2024 doi

  74. [84]

    Meyssonnier N., Azzopardi M., 1993, , https://ui.adsabs.harvard.edu/abs/1993A&AS..102..451M 102, 451

    1993

  75. [85]

    Moffat A. F. J., Breysacher J., Seggewiss W., 1985, @doi [ ] 10.1086/163184 , https://ui.adsabs.harvard.edu/abs/1985ApJ...292..511M 292, 511

    1985 doi

  76. [86]

    R., et al., 2006, @doi [ ] 10.1051/0004-6361:20064995 , https://ui.adsabs.harvard.edu/abs/2006A&A...456.1131M 456, 1131

    Mokiem M. R., et al., 2006, @doi [ ] 10.1051/0004-6361:20064995 , https://ui.adsabs.harvard.edu/abs/2006A&A...456.1131M 456, 1131

    2006 doi

  77. [87]

    Morrell N., Ostrov P., Massey P., Gamen R., 2003, @doi [ ] 10.1046/j.1365-8711.2003.06433.x , https://ui.adsabs.harvard.edu/abs/2003MNRAS.341..583M 341, 583

    2003

  78. [88]

    S., Bassino L

    Niemela V. S., Bassino L. P., 1994, @doi [ ] 10.1086/174999 , https://ui.adsabs.harvard.edu/abs/1994ApJ...437..332N 437, 332

    1994 doi

  79. [89]

    Pasquini L., et al., 2002, The Messenger, https://ui.adsabs.harvard.edu/abs/2002Msngr.110....1P 110, 1

    2002

  80. [90]

    R., Lennon D

    Patrick L. R., Lennon D. J., Najarro , F. et al., 2025, @doi [ ], https://ui.adsabs.harvard.edu/abs/2025arXiv250202644P 698, A39

    2025

  81. [91]

    T., Subramaniam A., Mathew B., Mennickent R

    Paul K. T., Subramaniam A., Mathew B., Mennickent R. E., Sabogal B., 2012, @doi [ ] 10.1111/j.1365-2966.2012.20591.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.421.3622P 421, 3622

    2012

  82. [92]

    Pauli D., et al., 2022, @doi [ ] 10.1051/0004-6361/202141738 , https://ui.adsabs.harvard.edu/abs/2022A&A...659A...9P 659, A9

    2022 doi

  83. [93]

    Pauli D., et al., 2023, @doi [ ] 10.1051/0004-6361/202345881 , https://ui.adsabs.harvard.edu/abs/2023A&A...673A..40P 673, A40

    2023 doi

  84. [94]

    Paxton B., Bildsten L., Dotter A., Herwig F., Lesaffre P., Timmes F., 2011, @doi [ ] 10.1088/0067-0049/192/1/3 , https://ui.adsabs.harvard.edu/abs/2011ApJS..192....3P 192, 3

    2011 doi

  85. [95]

    Paxton B., et al., 2015, @doi [ ] 10.1088/0067-0049/220/1/15 , https://ui.adsabs.harvard.edu/abs/2015ApJS..220...15P 220, 15

    2015 doi

  86. [96]

    R., Gies D

    Penny L. R., Gies D. R., 2009, @doi [ ] 10.1088/0004-637X/700/1/844 , https://ui.adsabs.harvard.edu/abs/2009ApJ...700..844P 700, 844

    2009 doi

  87. [97]

    K., 1987, @doi [ ] 10.1093/mnras/228.1.173 , https://ui.adsabs.harvard.edu/abs/1987MNRAS.228..173P 228, 173

    Prinja R. K., 1987, @doi [ ] 10.1093/mnras/228.1.173 , https://ui.adsabs.harvard.edu/abs/1987MNRAS.228..173P 228, 173

    1987 doi

  88. [98]

    A., Venero R., Repolust T., Springmann U., Jokuthy A., Mokiem M

    Puls J., Urbaneja M. A., Venero R., Repolust T., Springmann U., Jokuthy A., Mokiem M. R., 2005, @doi [ ] 10.1051/0004-6361:20042365 , https://ui.adsabs.harvard.edu/abs/2005A&A...435..669P 435, 669

    2005 doi

  89. [99]

    R., Hainich R., Oskinova L

    Ramachandran V., Hamann W. R., Hainich R., Oskinova L. M., Shenar T., Sander A. A. C., Todt H., Gallagher J. S., 2018, @doi [ ] 10.1051/0004-6361/201832816 , https://ui.adsabs.harvard.edu/abs/2018A&A...615A..40R 615, A40

    2018 doi

  90. [100]

    Ramachandran V., et al., 2019, @doi [ ] 10.1051/0004-6361/201935365 , https://ui.adsabs.harvard.edu/abs/2019A&A...625A.104R 625, A104

    2019 doi

  91. [101]

    H., et al., 2015, @doi [ ] 10.1051/0004-6361/201425424 , https://ui.adsabs.harvard.edu/abs/2015A&A...580A..92R 580, A92

    Ram \' rez-Agudelo O. H., et al., 2015, @doi [ ] 10.1051/0004-6361/201425424 , https://ui.adsabs.harvard.edu/abs/2015A&A...580A..92R 580, A92

    2015 doi

  92. [102]

    H., et al., 2017, @doi [ ] 10.1051/0004-6361/201628914 , https://ui.adsabs.harvard.edu/abs/2017A&A...600A..81R 600, A81

    Ram \' rez-Agudelo O. H., et al., 2017, @doi [ ] 10.1051/0004-6361/201628914 , https://ui.adsabs.harvard.edu/abs/2017A&A...600A..81R 600, A81

    2017 doi

  93. [103]

    J., Pauli D., 2023, @doi [ ] 10.1051/0004-6361/202346055 , https://ui.adsabs.harvard.edu/abs/2023A&A...674A..56R 674, A56

    Rickard M. J., Pauli D., 2023, @doi [ ] 10.1051/0004-6361/202346055 , https://ui.adsabs.harvard.edu/abs/2023A&A...674A..56R 674, A56

    2023 doi

  94. [104]

    J., et al., 2022, @doi [ ] 10.1051/0004-6361/202243281 , https://ui.adsabs.harvard.edu/abs/2022A&A...666A.189R 666, A189

    Rickard M. J., et al., 2022, @doi [ ] 10.1051/0004-6361/202243281 , https://ui.adsabs.harvard.edu/abs/2022A&A...666A.189R 666, A189

    2022 doi

  95. [105]

    W., Stroud V

    Ritchie B. W., Stroud V. E., Evans C. J., Clark J. S., Hunter I., Lennon D. J., Langer N., Smartt S. J., 2012, @doi [ ] 10.1051/0004-6361/201117716 , https://ui.adsabs.harvard.edu/abs/2012A&A...537A..29R 537, A29

    2012 doi

  96. [106]

    G., Puls J., Najarro F., Brott I., 2012, @doi [ ] 10.1051/0004-6361/201117790 , https://ui.adsabs.harvard.edu/abs/2012A&A...537A..79R 537, A79

    Rivero Gonz \'a lez J. G., Puls J., Najarro F., Brott I., 2012, @doi [ ] 10.1051/0004-6361/201117790 , https://ui.adsabs.harvard.edu/abs/2012A&A...537A..79R 537, A79

    2012 doi

  97. [107]

    Roman-Duval J., et al., 2025, @doi [ ] 10.3847/1538-4357/adc45b , 985, 109

    2025 doi

  98. [108]

    C., Dopita M

    Russell S. C., Dopita M. A., 1990, @doi [ ] 10.1086/191494 , https://ui.adsabs.harvard.edu/abs/1990ApJS...74...93R 74, 93

    1990 doi

  99. [109]

    Sab \' n-Sanjuli \'a n C., et al., 2014, @doi [ ] 10.1051/0004-6361/201322798 , https://ui.adsabs.harvard.edu/abs/2014A&A...564A..39S 564, A39

    2014 doi

  100. [110]

    Sab \' n-Sanjuli \'a n C., et al., 2017, @doi [ ] 10.1051/0004-6361/201629210 , https://ui.adsabs.harvard.edu/abs/2017A&A...601A..79S 601, A79

    2017 doi

  101. [111]

    Sana H., et al., 2012, @doi [Science] 10.1126/science.1223344 , https://ui.adsabs.harvard.edu/abs/2012Sci...337..444S 337, 444

    2012 doi

  102. [112]

    Sana H., et al., 2013, @doi [ ] 10.1051/0004-6361/201219621 , https://ui.adsabs.harvard.edu/abs/2013A&A...550A.107S 550, A107

    2013 doi

  103. [113]

    Sana H., Shenar T., Bodensteiner J. et al. 2025, Nat. Astron., accepted

    2025

  104. [114]

    Sanduleak N., 1968, @doi [ ] 10.1086/110625 , https://ui.adsabs.harvard.edu/abs/1968AJ.....73..246S 73, 246

    1968 doi

  105. [115]

    Sanduleak N., 1969, @doi [ ] 10.1086/110875 , https://ui.adsabs.harvard.edu/abs/1969AJ.....74..877S 74, 877

    1969 doi

  106. [116]

    Schneider F. R. N., Langer N., de Koter A., Brott I., Izzard R. G., Lau H. H. B., 2014, @doi [ ] 10.1051/0004-6361/201424286 , https://ui.adsabs.harvard.edu/abs/2014A&A...570A..66S 570, A66

    2014 doi

  107. [117]

    Schneider F. R. N., et al., 2018, @doi [ ] 10.1051/0004-6361/201833433 , https://ui.adsabs.harvard.edu/abs/2018A&A...618A..73S 618, A73

    2018 doi

  108. [118]

    J., Wang C., 2019, @doi [ ] 10.1051/0004-6361/201935046 , https://ui.adsabs.harvard.edu/abs/2019A&A...625A.132S 625, A132

    Schootemeijer A., Langer N., Grin N. J., Wang C., 2019, @doi [ ] 10.1051/0004-6361/201935046 , https://ui.adsabs.harvard.edu/abs/2019A&A...625A.132S 625, A132

    2019 doi

  109. [119]

    Schootemeijer A., et al., 2021, @doi [ ] 10.1051/0004-6361/202038789 , https://ui.adsabs.harvard.edu/abs/2021A&A...646A.106S 646, A106

    2021 doi

  110. [120]

    A., Bolatto A

    Sheets H. A., Bolatto A. D., van Loon J. T., Sandstrom K., Simon J. D., Oliveira J. M., Barb \'a R. H., 2013, @doi [ ] 10.1088/0004-637X/771/2/111 , https://ui.adsabs.harvard.edu/abs/2013ApJ...771..111S 771, 111

    2013 doi

  111. [121]

    Shenar T., et al., 2018, @doi [ ] 10.1051/0004-6361/201833006 , https://ui.adsabs.harvard.edu/abs/2018A&A...616A.103S 616, A103

    2018 doi

  112. [122]

    Shenar T., et al., 2022, @doi [ ] 10.1051/0004-6361/202244245 , https://ui.adsabs.harvard.edu/abs/2022A&A...665A.148S 665, A148

    2022 doi

  113. [123]

    Shenar T., et al., 2024, @doi [ ] 10.1051/0004-6361/202451586 , https://ui.adsabs.harvard.edu/abs/2024A&A...690A.289S 690, A289

    2024 doi

  114. [124]

    Sim \'o n-D \' az S., Herrero A., 2014, @doi [ ] 10.1051/0004-6361/201322758 , https://ui.adsabs.harvard.edu/abs/2014A&A...562A.135S 562, A135

    2014 doi

  115. [125]

    Sim \'o n-D \' az S., Castro N., Herrero A., Puls J., Garcia M., Sab \' n-Sanjuli \'a n C., 2011, in Journal of Physics Conference Series. IOP, p. 012021 ( @eprint arXiv 1111.1341 ), @doi 10.1088/1742-6596/328/1/012021

    2011 arXiv

  116. [126]

    Sim \'o n-D \' az S., Godart M., Castro N., Herrero A., Aerts C., Puls J., Telting J., Grassitelli L., 2017, @doi [ ] 10.1051/0004-6361/201628541 , https://ui.adsabs.harvard.edu/abs/2017A&A...597A..22S 597, A22

    2017 doi

  117. [127]

    F., et al., 2006, @doi [ ] 10.1086/498708 , https://ui.adsabs.harvard.edu/abs/2006AJ....131.1163S 131, 1163

    Skrutskie M. F., et al., 2006, @doi [ ] 10.1086/498708 , https://ui.adsabs.harvard.edu/abs/2006AJ....131.1163S 131, 1163

    2006 doi

  118. [128]

    J., 2015, @doi [ ] 10.1017/pasa.2015.17 , https://ui.adsabs.harvard.edu/abs/2015PASA...32...16S 32, e016

    Smartt S. J., 2015, @doi [ ] 10.1017/pasa.2015.17 , https://ui.adsabs.harvard.edu/abs/2015PASA...32...16S 32, e016

    2015 doi

  119. [129]

    M., Bruhweiler F

    Smith Neubig M. M., Bruhweiler F. C., 1997, @doi [ ] 10.1086/118617 , https://ui.adsabs.harvard.edu/abs/1997AJ....114.1951S 114, 1951

    1997 doi

  120. [130]

    Testor G., 2001, @doi [ ] 10.1051/0004-6361:20010527 , https://ui.adsabs.harvard.edu/abs/2001A&A...372..667T 372, 667

    2001 doi

  121. [131]

    C., 1987, , https://ui.adsabs.harvard.edu/abs/1987A&A...178...25T 178, 25

    Testor G., Lortet M. C., 1987, , https://ui.adsabs.harvard.edu/abs/1987A&A...178...25T 178, 25

    1987

  122. [132]

    L., Heydari-Malayeri M., Kristensen L

    Testor G., Lemaire J. L., Heydari-Malayeri M., Kristensen L. E., Diana S., Field D., 2010, @doi [ ] 10.1051/0004-6361/200911786 , https://ui.adsabs.harvard.edu/abs/2010A&A...510A..95T 510, A95

    2010 doi

  123. [133]

    J., 2005, @doi [ ] 10.1051/0004-6361:20042061 , https://ui.adsabs.harvard.edu/abs/2005A&A...434..677T 434, 677

    Trundle C., Lennon D. J., 2005, @doi [ ] 10.1051/0004-6361:20042061 , https://ui.adsabs.harvard.edu/abs/2005A&A...434..677T 434, 677

    2005 doi

  124. [134]

    J., Puls J., Dufton P

    Trundle C., Lennon D. J., Puls J., Dufton P. L., 2004, @doi [ ] 10.1051/0004-6361:20034325 , https://ui.adsabs.harvard.edu/abs/2004A&A...417..217T 417, 217

    2004 doi

  125. [135]

    I., Sana H., Mahy L

    Villase\ n or J. I., Sana H., Mahy L. et al., 2025, @doi [ ], https://ui.adsabs.harvard.edu/abs/2025arXiv250321936V 698, A41

    2025

  126. [136]

    S., Brott I., Gr \"a fener G., Langer N., de Koter A., Lennon D

    Vink J. S., Brott I., Gr \"a fener G., Langer N., de Koter A., Lennon D. J., 2010, @doi [ ] 10.1051/0004-6361/201014205 , https://ui.adsabs.harvard.edu/abs/2010A&A...512L...7V 512, L7

    2010 doi

  127. [137]

    S., et al., 2023, @doi [ ] 10.1051/0004-6361/202245650 , https://ui.adsabs.harvard.edu/abs/2023A&A...675A.154V 675, A154

    Vink J. S., et al., 2023, @doi [ ] 10.1051/0004-6361/202245650 , https://ui.adsabs.harvard.edu/abs/2023A&A...675A.154V 675, A154

    2023 doi

  128. [138]

    R., 1983, @doi [ ] 10.1086/160716 , https://ui.adsabs.harvard.edu/abs/1983ApJ...265..716W 265, 716

    Walborn N. R., 1983, @doi [ ] 10.1086/160716 , https://ui.adsabs.harvard.edu/abs/1983ApJ...265..716W 265, 716

    1983 doi

  129. [139]

    R., Lennon D

    Walborn N. R., Lennon D. J., Haser S. M., Kudritzki R.-P., Voels S. A., 1995, @doi [ ] 10.1086/133524 , https://ui.adsabs.harvard.edu/abs/1995PASP..107..104W 107, 104

    1995 doi

  130. [140]

    R., Lennon D

    Walborn N. R., Lennon D. J., Heap S. R., Lindler D. J., Smith L. J., Evans C. J., Parker J. W., 2000, @doi [ ] 10.1086/316617 , https://ui.adsabs.harvard.edu/abs/2000PASP..112.1243W 112, 1243

    2000 doi

  131. [141]

    R., Fullerton A

    Walborn N. R., Fullerton A. W., Crowther P. A., Bianchi L., Hutchings J. B., Pellerin A., Sonneborn G., Willis A. J., 2002, @doi [ ] 10.1086/340571 , https://ui.adsabs.harvard.edu/abs/2002ApJS..141..443W 141, 443

    2002 doi

  132. [142]

    R., Morrell N

    Walborn N. R., Morrell N. I., Howarth I. D., Crowther P. A., Lennon D. J., Massey P., Arias J. I., 2004, @doi [ ] 10.1086/420761 , https://ui.adsabs.harvard.edu/abs/2004ApJ...608.1028W 608, 1028

    2004 doi

  133. [143]

    R., et al., 2010, @doi [ ] 10.1088/0004-6256/139/3/1283 , https://ui.adsabs.harvard.edu/abs/2010AJ....139.1283W 139, 1283

    Walborn N. R., et al., 2010, @doi [ ] 10.1088/0004-6256/139/3/1283 , https://ui.adsabs.harvard.edu/abs/2010AJ....139.1283W 139, 1283

    2010 doi

  134. [144]

    Wang B., Shi W., Miao Z., 2015, @doi [PLoS ONE] 10.1371/journal.pone.0118537 , https://ui.adsabs.harvard.edu/abs/2015PLoSO..1018537W 10, e0118537

    2015 doi

  135. [145]

    Wen ker I., 1990, @doi [ ] 10.1088/0031-8949/42/6/008 , https://ui.adsabs.harvard.edu/abs/1990PhyS...42..667W 42, 667

    1990 doi

  136. [146]

    M., 1994, @doi [ ] 10.1086/117189 , https://ui.adsabs.harvard.edu/abs/1994AJ....108.1674W 108, 1674

    Wilcots E. M., 1994, @doi [ ] 10.1086/117189 , https://ui.adsabs.harvard.edu/abs/1994AJ....108.1674W 108, 1674

    1994 doi

Pith tools

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