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Hot and cool: Characterising the companions of red supergiant stars in binary systems

T0 review · 3 major / 6 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read The 88 ultraviolet-bright red supergiant binaries in the Small Magellanic Cloud show a flat mass-ratio distribution, though the photometric assumptions that produce it can underestimate companion masses.

desk verdict A genuinely useful compilation of the scarce RSG binary data, but the headline flat-q result is inherited from the authors' earlier photometric work and their own HST example shows why it should not be trusted yet. read the letter →

arxiv 2411.14540 v1 pith:XTXB2RPA submitted 2024-11-21 astro-ph.SR

L. R. Patrick , I. Negueruela This is my paper · ORCID
classification astro-ph.SR
keywords redsupergiantstarsbinarysystemsmass-ratiodistributionSmallMagellanicCloudultravioletphotometryhotcompanionsVVCepheimassivestarevolution
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 collects the small, well-observed population of red supergiant (RSG) stars that have hot companions, and uses it to interpret a much larger sample of 88 ultraviolet-bright RSG binaries recently found in the Small Magellanic Cloud. It argues that these extragalactic systems are genuine binaries whose hot companions are mostly main-sequence B-type stars, and that their mass ratios are distributed flatly over the range $0.3

What carries the argument

The load-bearing device is the mass ratio $q = M_2/M_{\rm RSG}$ obtained from ultraviolet photometry of the hot companion, under three simplifying assumptions: the companion is a normal main-sequence B-type star, it has the same age as the RSG, and it suffers the same extinction. These assumptions convert a UV excess into a companion mass, and the distribution of the resulting $q$ values over 88 systems is the evidence for the flat mass-ratio claim. The paper also relies on the compiled catalogue of well-characterised Galactic RSG binaries, with orbital periods and, where possible, component masses, as the reference point against which the SMC population is judged.

What would settle it

A decisive test is to obtain ultraviolet spectra with independent extinction determinations for a large fraction of the 88 SMC companions, not just 17 targets, and compare spectroscopically derived companion masses with the photometric ones. If the spectroscopically determined mass ratios are flat in $0.3<q<1$ as well, the claim holds; if they are systematically higher or cluster near $q>1$ as seen for PMMR 44, the flat distribution is an artefact of the photometric assumptions.

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Extended reading notes

Core claim

On the paper's own terms, the central discovery is that the 88 ultraviolet-bright RSG binaries in the Small Magellanic Cloud, identified from UVIT/Astrosat photometry and free of contamination from the red supergiant itself, display a flat mass-ratio distribution in the range $0.3<q<1$, in slight tension with the handful of Galactic systems whose mass ratios are known. The compiled Galactic systems, with current masses above roughly $8\,M_\odot$ and orbital periods from 3 to 75 years (with Antares at about 2000 years as a clear outlier), anchor this population: most companions are main-sequence B-type stars, and the SMC companions appear consistent with that picture. The paper cautions that the photometric mass ratios were derived assuming each hot companion is a normal main-sequence B star of the same age and extinction as the RSG, and presents an ultraviolet spectrum of one system (PMMR 44) in which the photometric effective temperature is significantly underestimated, which would raise its companion mass and push its mass ratio above $q=1$.

Load-bearing premise

The flat mass-ratio distribution stands or falls on the assumption that every hot companion in the SMC sample is a normal main-sequence B-type star of the same age and extinction as its red supergiant; the paper's own ultraviolet spectrum of PMMR 44 shows this assumption can fail, so a widespread failure would erase the flat distribution.

Editorial extensions

If this is right

  • The 88 SMC systems form the only extragalactic RSG binary population whose hot companions can be directly studied, providing a statistical sample for binary-evolution models.
  • A flat mass-ratio distribution over $0.3<q<1$ implies that RSG binaries do not preferentially form with equal masses, and that the Galactic census, with only five measured mass ratios, cannot yet rule out the same flat shape.
  • Because the orbital-period distribution inferred from the SMC sample drops sharply after roughly $\log P \simeq 3.5$ days, most of these systems should have periods well under the 3–75 year range of the well-characterised Galactic binaries.
  • If the photometric assumptions underestimate companion masses, some SMC binaries may have $q>1$, meaning the companion is more massive than the visible red supergiant, and such systems would be misclassified by mass-ratio-based population comparisons.
  • The predominance of B-type main-sequence companions in both the compiled Galactic systems and the SMC candidates supports the theoretical expectation that most surviving RSG binaries avoided prior mass transfer and host unevolved hot stars.

Reading between the lines

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

  • If the underestimation seen in PMMR 44 is typical, the true SMC mass-ratio distribution may be rising toward $q>1$ rather than flat, which would change predictions for the supernova endpoints of these binaries (editorial inference, not stated by the paper).
  • The same photometric technique applied to yellow supergiant binaries and to the LMC RSG population could be tested against the SMC result; a similar flat distribution in another galaxy would strengthen the claim that low metallicity does not reshape RSG companion statistics.
  • The wide Galactic systems with periods of decades suggest that multi-epoch radial-velocity catalogues, such as those from long-baseline surveys, should reveal many more RSG binaries if the flat-q SMC distribution reflects a universal property, since only a fraction of such systems would show detectable UV excess.
  • A companion more massive than the RSG in a $q>1$ system would make the visible red supergiant the less massive component, implying that some systems classified as RSG binaries are actually post-mass-transfer binaries in which the mass ratio has reversed.
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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 / 6 minor

Summary. The paper reviews the observational and theoretical status of red supergiant (RSG) binaries, compiling nine Galactic systems with orbital-period constraints and five with mass-ratio estimates. It then turns to the newly discovered population of 88 ultraviolet-bright RSG binaries in the Small Magellanic Cloud (SMC), summarizes a Hubble Space Telescope (HST) STIS snapshot survey of 17 of these systems, and repeats the claim from prior work that these systems show a flat mass-ratio distribution in the range 0.3 < q < 1. The paper also discusses the theoretical expectations for RSG binaries and reports new characterization of the Galactic X-ray binary TYC 2673-2004-1.

Significance. If the flat-q claim for the SMC RSG binaries holds, it would be an important constraint on binary evolution and supernova progenitor channels, especially at low metallicity. The compilation of the best-studied Galactic RSG binaries is a useful reference, and the HST snapshot survey summary is a valuable preview of forthcoming results. The paper is transparent about the assumptions behind the photometric mass ratios and explicitly notes that the HST data indicate those assumptions are too simplistic. However, the headline quantitative claim is not newly established in this manuscript: it is inherited from Patrick et al. (2022), and the one fully worked HST example (PMMR 44) shows the companion is hotter and more massive than the photometric analysis inferred, potentially pushing q above unity. Because the full HST analysis is unpublished, the flat-q result remains conditional, and the paper should either include the HST-based mass ratios or clearly mark the claim as provisional.

major comments (3)
  1. [Abstract; §4.1; §5] The central claim that the 88 SMC RSG binaries show a flat mass-ratio distribution in the range 0.3 < q < 1 is not supported by the evidence in this manuscript. The claim is quoted from Patrick et al. (2022), and the paper's own HST spectrum of PMMR 44 (Fig. 3) shows that the key photometric assumptions fail for this object: the effective temperature is significantly higher than the UVIT value, which would make the companion more massive and could give q > 1. Section 5 concedes that the simplifying assumptions used in the photometric analysis are 'indeed too simplistic.' Since the HST re-analysis for the full sample of 17 observed targets is only summarized as unpublished work (Patrick et al., in prep.), the flat-q result cannot be verified from the material in this paper. The abstract and Section 5 should either present the flat-q claim as provisional pending the HST analysis, or the paper should include the HST-based stellar parameters and mass ratios.
  2. [§4.1] The treatment of extinction in the HST analysis is not sufficiently clear. The text says Patrick et al. (in prep.) determined stellar parameters 'by assuming extinction properties based on the RSG component,' and the continuum fits for PMMR 44 shown in Fig. 3 are for a fixed A_V. This means the HST analysis does not independently test the third simplifying assumption (same extinction for both components). The PMMR 44 example therefore only demonstrates that the assumed main-sequence B-star temperature scale or the coeval age assumption can fail, not that the extinction assumption is too simplistic. The paper should clarify which of the three assumptions are actually tested by the HST data, and whether the quoted result that the assumptions are 'too simplistic' extends to the extinction treatment.
  3. [Table 1; §5] The comparison of the SMC flat-q distribution with the Galactic population rests on only five mass-ratio estimates in Table 1, several with large and asymmetric uncertainties. For V766 Cen, q = 0.16^{+0.4}_{-0.07} is consistent with q ≈ 0.5 at the upper end, and for WY Gem the quoted range 0.75–1 spans most of the claimed flat-q interval. With five systems, the statement in Section 5 that the Galactic sample is in 'slight tension' with the SMC flat-q distribution is not statistically meaningful. The paper should either quantify the tension (e.g., with a formal comparison of the two small samples) or soften the claim.
minor comments (6)
  1. [Figures] Two figures are both labeled 'Figure 2': the spectrum of TYC 2673-2004-1 and the HST spectrum of PMMR 44. The HST spectrum shown in Section 4.1 should be renumbered as Figure 3, and the in-text reference in §4.1 should be updated accordingly.
  2. [§4] The phrase 'Milky Clouds' in the opening sentence of Section 4 should be 'Magellanic Clouds.'
  3. [§3] In the paragraph on VV Cep, 'text bookGiants of the Eclipse' is missing a space and should read 'textbook Giants of the Eclipse.'
  4. [Abstract] The abstract states the orbital period of Antares is 'around 2000 a,' while Table 1 lists 2700 a. These values should be harmonized.
  5. [References] References [40] and [41] are duplicated entries for the same paper (Moe & Di Stefano 2017). One of them should be removed.
  6. [Front matter] The MSC codes (65F15, 65G50, 15-04, 15B99) are numerical linear algebra classifications and are unrelated to the astrophysical content of the paper. They should be replaced with appropriate astronomy/astrophysics codes or removed.

Circularity Check

0 steps flagged · score 2.0 of 10

No derivational circularity; the headline flat-q result is explicitly imported from the authors' own prior UVIT analysis and is undermined by the paper's own HST test, but it is transparently attributed and not reconstructed as a new derivation.

full rationale

The paper is a review and synthesis rather than a derivation. The headline claim that the 88 SMC RSG binaries show a flat-q distribution over 0.3<q<1 is not fitted in this manuscript; it is quoted from Patrick et al. [50] and [49], both first-authored by L. R. Patrick. The text says: 'This led Patrick et al. [50] to conclude that RSGs with hot UV companions in the SMC are best described with a flat-q distribution, which was further shown by [49].' Section 4.1 then lists the three simplifying assumptions on which [50]'s mass ratios rest (normal main-sequence B star, coeval companion, same extinction), and the paper's own HST STIS spectrum of PMMR 44 shows Teff = 20,000 K, significantly hotter than the [50] photometric value, which would make q>1 possible. Section 5 concedes that the simplifying assumptions are 'indeed too simplistic.' These statements are limitations and correctness risks, not circular constructions: no equation in this paper equals its own input by definition, the q range is not definitionally forced, and the Galactic compilation of nine well-characterised systems plus the theoretical period-q simulations in Section 2 provide independent content. The self-citations carry the flat-q result, but the result is externally falsifiable and is being explicitly tested by new HST data from the same group, so per the review rules this raises a self-citation burden rather than a circularity score above 2.

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

The paper is a review and thus relies on standard astrophysical assumptions and on previously published analyses. No new free parameters or invented entities are introduced. The main assumptions concern the interpretation of the compiled data and the photometric derivation of mass ratios.

assumptions (4)
  • domain assumption The current masses of the RSGs in the compiled sample reflect their initial masses, i.e., no significant mass transfer has occurred.
    Stated in Section 3: 'This choice assumes that the current mass reflects the initial mass of the star, which is, in effect, assuming that mass-transfer has not taken place.' The paper notes this is difficult to assess.
  • domain assumption The hot companions in the SMC sample are normal main-sequence B-type stars with the same age and extinction as the RSG.
    Section 4.1 lists these as the three key simplifying assumptions in Patrick et al. (2022) that underlie the flat-q distribution.
  • domain assumption The orbital period distribution of the compiled Galactic systems is representative of the total RSG binary population.
    The paper compares the SMC period distribution (sharp drop after log P ~ 3.5) with only 9-10 Galactic systems, a small and heterogeneous sample.
  • domain assumption The eccentricity distribution P(e) ~ e + 0.8 from Moe & Di Stefano (2017) is appropriate for long-period massive binaries.
    Used in the simulations in Section 2 to set minimum orbital periods.

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Cite this review

Pith. "Pith review of Hot and cool: Characterising the companions of red supergiant stars in binary systems." pith.science (2026). https://pith.science/paper/XTXB2RPA

@misc{pith2026241114540,
  author       = {Pith},
  title        = {Pith review of: Hot and cool: Characterising the companions of red supergiant stars in binary systems},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/XTXB2RPA}},
  note         = {Machine review of arXiv:2411.14540}
}
read the original abstract

In this article we study the nature of the recently identified populations of hot companions to red supergiant stars (RSGs). To this end, we compile the literature on the most well characterised systems with the aim of better understanding the hot companions identified with ultra-violet photometry and confirmed with Hubble Space Telescope spectra in the Local Group. We identify 9 systems with current masses greater than around 8 solar masses that have constraints on their orbital periods, which are in the range 3 to 75a. Antares (Alpha Sco) is the obvious outlier in this distribution, having an estimated orbital period of around 2000 a. Mass-ratio (q=M2/MRSG) estimates are available only for 5 of the compiled systems and range between 0.16 < q < 1. Ongoing efforts to identify and characterise hot companions to RSGs in the SMC have revealed 88 hot companions that have observational constraints free of contamination from the RSG component. We present a summary of a recently conducted HST UV spectroscopic survey that aims to characterise a subset of these companions. These companions show a flat-q distribution in the range 0.3 < q < 1.

Figures

Figures reproduced from arXiv: 2411.14540 by the authors.

Figure 1
Figure 1. Orbital period – mass-ratio (q = M2/M1) diagram for a set of simulated binary systems covering orbital periods in the range 3 to 105 d. The minimum allowed orbital period as a function of q for three RSG case studies at 8, 15 and 30 M⊙ with representative radii. Black solid lines show lines of constant semi-amplitude velocity for the simu￾lated systems on the 5, 10, 25 and 50 km s−1 levels. are excluded and the orbi… view at source ↗
Figure 2
Figure 2. A portion of the spectrum of TYC 2673-2004-1 (bottom) compared to the spectrum of HD 10465, an M2 Ib supergiant, from the ˙ spectral library of Carquillat et al. [9], after convolving to the same res￾olution. The strength of the Ca II triplet and the λ8468 blend, which are sensitive to luminosity, suggest the same luminosity class. The origi￾nal spectrum was taken with Mercator/HERMES and has a resolution R ≈ 85000 … view at source ↗
Figure 3
Figure 3. The full flux-calibrated HST STIS spectrum of PMMR 44 from Patrick et al. (in prep.). Coloured lines are effective temperature fits for a fixed AV . The features visible are dominated by interstellar contamination and are not appropriate for stellar parameter determina￾tion. The green solid star at 1750 Å shows the UVIT FUV photometry. The red solid line shows the best fit effective temperature to the contin￾uum for… view at source ↗

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Reviewed August 12, 2026 · model on record in the stance chip above.