pith. sign in

arxiv: 2606.27586 · v1 · pith:SW57QMH4new · submitted 2026-06-25 · 🌌 astro-ph.SR

Detached Post-Algol Eclipsing Binaries Caught Between Case A and Case AB Mass Transfer

Megan G. Frank , Maxwell Moe , Nathan Smith This is my paper

Pith reviewed 2026-06-29 00:29 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords post-Algol binarieseclipsing binariesTAMS contractionmass transferRoche lobe fill factorLMCstellar evolutionAlgol systems
0
0 comments X

The pith

Detached post-Algol eclipsing binaries provide the first empirical evidence that intermediate-mass stars contract along the terminal-age main sequence.

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

The paper presents the discovery of detached eclipsing binary candidates in the Large Magellanic Cloud that are in a short-lived phase between two stages of mass transfer. These systems have a hot main-sequence primary and a cool subgiant secondary that has not yet refilled its Roche lobe after a previous mass transfer episode. The measured fill factors of 73 to 89 percent match predictions from binary evolution models for the contraction phase after the main-sequence hook. This finding supplies the first direct observational support for a sixty-year-old prediction in stellar evolution that intermediate-mass stars slightly contract as they exhaust core hydrogen.

Core claim

We report the discovery of detached post-Algol EB candidates in the LMC caught between Case A and Case AB mass transfer. Their OGLE light curves feature strong reflection effects as the hot primary irradiates the cool subgiant secondary. The primaries have mid-B MS atmospheres with masses 6-8 solar masses, and dynamical masses of the subgiant secondaries are 0.9-1.2 solar masses. Detailed fitting of the light curves reveals Roche lobe fill factors of 73-89 percent, consistent with binary evolution models. This provides the first empirical evidence that intermediate-mass stars contract along the TAMS.

What carries the argument

The Roche-lobe fill factors of the subgiant secondaries in post-Algol systems, measured from light curve fitting and compared to binary evolution tracks.

If this is right

  • The main-sequence hook feature on the Hertzsprung-Russell diagram for intermediate-mass stars is confirmed by observation.
  • Binary evolution models for the transition from Case A to Case AB mass transfer can be tested with these systems.
  • The duration of the detached post-Algol phase can be calibrated using the observed population.
  • Mass determinations from eclipsing binaries provide anchors for stellar models of subgiants.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • This identification may help refine the timescales in binary population synthesis models for Algol systems.
  • Similar systems could be searched for in other galaxies to test if the contraction phase is universal.
  • Future observations of the primaries' evolution could link to the formation of other exotic binaries.

Load-bearing premise

The 73-89% Roche-lobe fill factors place the secondaries in the brief post-Case-A contraction window on the TAMS rather than in some other detached evolutionary state.

What would settle it

Detailed comparison of the observed systems to binary evolution tracks showing that the fill factors and positions do not correspond to the predicted contraction phase after Case A mass transfer.

Figures

Figures reproduced from arXiv: 2606.27586 by Maxwell Moe, Megan G. Frank, Nathan Smith.

Figure 1
Figure 1. Figure 1: OGLE-III I-band light curve of our prototype post-Algol EB-5898. A schematic diagram of the positions of the B-type MS primary (blue) and irradiated subgiant (red) are displayed at the top as a function of orbital phase. 2. POST-ALGOLS We show the OGLE-III I-band light curve of EB-5898 in [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Evolutionary sequence of intermediate-mass bina￾ries, highlighting the post-Algol phase between Case A and AB mass transfer. and AB mass transfer are presented in [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Ellipsoidal amplitudes versus sum of eclipse widths for the 103 OGLE-III LMC EBs with OB primaries and reflection effect amplitudes ∆IRefl > 0.08 mag. We categorize 5 detached nascent EBs (dark purple diamonds), 3 semi-detached nascent EBs (light purple squares), 86 semi-detached Algols (light orange pluses), the 5 featured detached post-Algols (red crosses), and 4 ambiguous EBs (black asterisks). We displ… view at source ↗
Figure 4
Figure 4. Figure 4: Stacked spectrum of each EB (black) with corresponding best-fit TLUSTY model (red) across 3800 - 4300 ˚A [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: TLUSTY model atmospheres (purple) and smoothed, dust-reddened SED fits (green) to UV (crosses) and optical (pluses) broadband photometry. The near-IR photometry (grey) exhibits extreme variability due to the heated side of the subgiant secondary, which we exclude when fitting the SEDs of the B-dwarf primaries. velocities for each spectrum of each object using two dif￾ferent methods. As described in Section… view at source ↗
Figure 7
Figure 7. Figure 7: Locations of our B-dwarf primaries on HR diagrams in terms of luminosity (left) and absolute magnitude (right). We overlay MIST evolutionary tracks, plotting surface gravity tick marks in intervals of 0.25 dex (thick tick mark at log g = 4.0). curves and the adopted radial velocities. We report in [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: EB-1050 light curves and radial velocity fits. Panel a shows the light curve from OGLE-III (black) and the corresponding PHOEBE fit (blue). Panel b shows the residuals between the OGLE-III light curve and PHOEBE fit. Panels c and d show the same as Panels a and b but for the OGLE-IV light curve. Panel e shows the adopted radial velocities (black) and corresponding fit (blue) [PITH_FULL_IMAGE:figures/full_… view at source ↗
Figure 9
Figure 9. Figure 9: Same as [PITH_FULL_IMAGE:figures/full_fig_p016_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Same as [PITH_FULL_IMAGE:figures/full_fig_p017_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Same as [PITH_FULL_IMAGE:figures/full_fig_p017_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: HRD of the subgiant secondaries in our four EBs. We overlay MIST pre-MS evolutionary tracks and the zero-age MS. The dots along each track indicate 1 Myr of evolution. Three of our subgiants are measurably dis￾crepant with the corresponding pre-MS tracks given their measured dynamical masses, and therefore they are most likely post-Algols. but it may potentially be a runaway nascent EB that is only 1 Myr … view at source ↗
read the original abstract

For sixty years, stellar evolutionary models have predicted that intermediate-mass stars slightly contract on the terminal-age main-sequence (TAMS) as they exhaust hydrogen in their convective cores, producing the main-sequence (MS) hook on the Hertzsprung-Russell diagram. Contraction along the TAMS has not previously been observationally verified, but an evolved eclipsing binary (EB) with a component on the TAMS can test this prediction. In a very close binary with an orbital period of less than a week, the primary star initially fills its Roche lobe on the MS (Case A mass transfer), and the binary can invert mass ratios, producing a classical Algol. The subgiant donor then contracts on the TAMS and detaches slightly from its Roche lobe. The subgiant subsequently re-expands and refills its Roche lobe as it evolves toward the Hertzsprung Gap (Case AB mass transfer). We report the discovery of detached post-Algol EB candidates in the LMC caught between Case A and Case AB mass transfer. Their OGLE light curves feature strong reflection effects as the hot primary (former mass gainer) irradiates the cool subgiant secondary. We analyze multi-epoch echelle spectra of four post-Algol candidates taken with the MIKE spectrograph at the 6.5m Magellan-Clay telescope. The primaries have mid-B MS atmospheres (M1 = 6 - 8 Msun). We measure dynamical masses of the subgiant secondaries to be M2 = 0.9 - 1.2 Msun. Detailed fitting of the OGLE light curves with PHOEBE reveals that the subgiants have Roche lobe fill factors of RLF F2 = 73% - 89%, consistent with binary evolution models. Our discovery of detached post-Algol candidates provides the first empirical evidence that intermediate-mass stars contract along the TAMS.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The paper reports the discovery of four detached eclipsing binaries in the LMC interpreted as post-Algol systems in the brief window between Case A and Case AB mass transfer. Spectroscopic analysis yields dynamical masses M1 = 6–8 M⊙ (mid-B primaries) and M2 = 0.9–1.2 M⊙ (subgiant secondaries), while PHOEBE modeling of OGLE light curves gives secondary Roche-lobe fill factors of 73–89% together with strong reflection effects; the authors conclude these systems supply the first empirical evidence that intermediate-mass stars contract along the TAMS.

Significance. If the phase identification can be shown to be unique, the result would constitute the first direct observational test of the long-predicted TAMS hook for intermediate-mass stars. Dynamical masses and multi-epoch spectroscopy provide a solid foundation, but the absence of quantitative model comparisons limits the immediate impact.

major comments (2)
  1. [Abstract] Abstract: the assertion that RLF F2 = 73–89% is 'consistent with binary evolution models' is load-bearing for the central claim that the systems are observed precisely during the post-Case-A contraction phase. No specific evolutionary tracks, grid parameters, or quantitative overlap metrics are referenced, leaving open whether other detached channels (post-Case B, residual thermal adjustment, or certain pre-transfer states) can produce the same fill-factor range.
  2. [Abstract] Abstract: no uncertainties are reported on the dynamical masses or fill factors, and no goodness-of-fit statistics (e.g., χ² or residual rms) are given for the PHOEBE solutions. These omissions prevent assessment of whether the observed parameters robustly exclude alternative evolutionary states.
minor comments (1)
  1. [Abstract] The abstract states 'detailed fitting' but does not indicate whether the reflection-effect amplitudes or temperature ratios were fitted simultaneously with the fill factors.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive feedback. The comments highlight areas where additional quantitative detail will strengthen the manuscript. We agree that explicit model comparisons and error reporting are needed and will revise the paper accordingly to address both points.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the assertion that RLF F2 = 73–89% is 'consistent with binary evolution models' is load-bearing for the central claim that the systems are observed precisely during the post-Case-A contraction phase. No specific evolutionary tracks, grid parameters, or quantitative overlap metrics are referenced, leaving open whether other detached channels (post-Case B, residual thermal adjustment, or certain pre-transfer states) can produce the same fill-factor range.

    Authors: We agree that the abstract statement requires supporting detail to demonstrate uniqueness of the evolutionary phase. In the revised manuscript we will add explicit comparisons to published binary evolution grids (e.g., MESA-based Case A sequences for 6–8 M⊙ primaries) that predict Roche-lobe fill factors of 70–90 % during the brief TAMS contraction window, together with quantitative overlap metrics and a short discussion ruling out post-Case B and pre-transfer states at the observed mass ratio and period. revision: yes

  2. Referee: [Abstract] Abstract: no uncertainties are reported on the dynamical masses or fill factors, and no goodness-of-fit statistics (e.g., χ² or residual rms) are given for the PHOEBE solutions. These omissions prevent assessment of whether the observed parameters robustly exclude alternative evolutionary states.

    Authors: We concur that uncertainties and fit-quality metrics are essential. The revised version will report 1σ uncertainties on M1, M2, and RLF F2 derived from the MIKE radial-velocity orbits and PHOEBE light-curve solutions, and will include χ² per degree of freedom together with residual rms values for each system. These additions will allow readers to evaluate the robustness of the parameters relative to alternative channels. revision: yes

Circularity Check

0 steps flagged

No significant circularity; fill-factor measurements are independent of the cited models

full rationale

The paper measures dynamical masses from MIKE echelle spectra and Roche-lobe fill factors (RLF F2 = 73–89 %) from PHOEBE fitting of OGLE light curves; these quantities are extracted directly from observations and are not defined by or fitted to the binary evolution tracks. The tracks are invoked only for post-hoc consistency checks. No self-citation, self-definitional loop, or fitted-input-called-prediction appears in the derivation. The phase identification therefore rests on external comparison rather than internal reduction, satisfying the criteria for a self-contained, non-circular result.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the interpretation that the measured fill factors correspond to the TAMS contraction phase; this interpretation is not derived from first principles within the abstract but is asserted by comparison to unspecified binary evolution models.

axioms (1)
  • domain assumption Binary evolution models correctly predict the duration and fill-factor range of the post-Case-A detached phase for 6-8 solar-mass primaries.
    The abstract states consistency with models but does not derive the expected fill-factor window from first principles.

pith-pipeline@v0.9.1-grok · 5894 in / 1373 out tokens · 20556 ms · 2026-06-29T00:29:02.548686+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

49 extracted references · 48 canonical work pages · 6 internal anchors

  1. [1]

    A., Levato, H., & Grosso, M

    Abt, H. A., Levato, H., & Grosso, M. 2002, ApJ, 573, 359, doi: 10.1086/340590

    work page doi:10.1086/340590 2002

  2. [2]

    D., Pedretti, E., et al

    Baron, F., Monnier, J. D., Pedretti, E., et al. 2012, ApJ, 752, 20, doi: 10.1088/0004-637X/752/1/20

    work page doi:10.1088/0004-637x/752/1/20 2012

  3. [3]

    A., Gunnels, S

    Bernstein, R., Shectman, S. A., Gunnels, S. M., Mochnacki, S., & Athey, A. E. 2003, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 4841, Instrument Design and Performance for Optical/Infrared Ground-based Telescopes, ed. M. Iye & A. F. M. Moorwood, 1694–1704, doi: 10.1117/12.461502

    work page doi:10.1117/12.461502 2003

  4. [4]

    M., Sobral, D., Smail, I., et al

    Bressan, A., Marigo, P., Girardi, L., et al. 2012, MNRAS, 427, 127, doi: 10.1111/j.1365-2966.2012.21948.x

    work page doi:10.1111/j.1365-2966.2012.21948.x 2012

  5. [5]

    B., Nascimbeni, V., Borsato, L., et al

    Brown-Sevilla, S. B., Nascimbeni, V., Borsato, L., et al. 2021, MNRAS, 506, 2122, doi: 10.1093/mnras/stab1843

    work page doi:10.1093/mnras/stab1843 2021

  6. [6]

    Q., Guo, H

    Chen, B. Q., Guo, H. L., Gao, J., et al. 2022, MNRAS, 511, 1317, doi: 10.1093/mnras/stac072

    work page doi:10.1093/mnras/stac072 2022

  7. [7]

    2016, ApJ, 823, 102, doi: 10.3847/0004-637X/823/2/102

    Choi, J., Dotter, A., Conroy, C., et al. 2016, ApJ, 823, 102, doi: 10.3847/0004-637X/823/2/102 de Burgos, A., Sim´ on-D´ ıaz, S., Urbaneja, M. A., et al. 2025, A&A, 695, A87, doi: 10.1051/0004-6361/202453242 de Mink, S. E., Pols, O. R., & Hilditch, R. W. 2007, A&A, 467, 1181, doi: 10.1051/0004-6361:20067007

    work page internal anchor Pith review doi:10.3847/0004-637x/823/2/102 2016

  8. [8]

    J., & Jorissen, A

    Deschamps, R., Siess, L., Davis, P. J., & Jorissen, A. 2013, A&A, 557, A40, doi: 10.1051/0004-6361/201321509

    work page doi:10.1051/0004-6361/201321509 2013

  9. [9]

    2008, ApJS, 178, 89, doi: 10.1086/589654

    Dotter, A., Chaboyer, B., Jevremovi´ c, D., et al. 2008, ApJS, 178, 89, doi: 10.1086/589654

    work page doi:10.1086/589654 2008

  10. [10]

    Eggleton, P. P. 1983, ApJ, 268, 368, doi: 10.1086/160960

    work page doi:10.1086/160960 1983

  11. [11]

    Fitzpatrick, E. L. 1999, PASP, 111, 63, doi: 10.1086/316293 Post-Algols21

    work page doi:10.1086/316293 1999

  12. [12]

    S., & Portegies Zwart, S

    Fujii, M. S., & Portegies Zwart, S. 2011, Science, 334, 1380, doi: 10.1126/science.1211927

    work page doi:10.1126/science.1211927 2011

  13. [13]

    R., & Bolton, C

    Gies, D. R., & Bolton, C. T. 1986, ApJS, 61, 419, doi: 10.1086/191118 G lowacki, M., Soszy´ nski, I., Udalski, A., et al. 2024, AcA, 74, 241, doi: 10.32023/0001-5237/74.4.1

    work page doi:10.1086/191118 1986

  14. [14]

    The Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. XII. Eclipsing Binary Stars in the Large Magellanic Cloud

    Graczyk, D., Soszy´ nski, I., Poleski, R., et al. 2011, AcA, 61, 103, doi: 10.48550/arXiv.1108.0446

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1108.0446 2011

  15. [15]

    Hoogerwerf, R., de Bruijne, J. H. J., & de Zeeuw, P. T. 2001, A&A, 365, 49, doi: 10.1051/0004-6361:20000014

    work page doi:10.1051/0004-6361:20000014 2001

  16. [16]

    1967a, ARA&A, 5, 571, doi: 10.1146/annurev.aa.05.090167.003035

    Iben, Jr., I. 1967a, ARA&A, 5, 571, doi: 10.1146/annurev.aa.05.090167.003035

    work page doi:10.1146/annurev.aa.05.090167.003035

  17. [17]

    1967b, ApJ, 147, 650, doi: 10.1086/149041

    Iben, Jr., I. 1967b, ApJ, 147, 650, doi: 10.1086/149041

    work page doi:10.1086/149041

  18. [18]

    2021, MNRAS, 503, 5554, doi: 10.1093/mnras/stab846

    Jerzykiewicz, M., Pigulski, A., Michalska, G., et al. 2021, MNRAS, 503, 5554, doi: 10.1093/mnras/stab846

    work page doi:10.1093/mnras/stab846 2021

  19. [19]

    Kelson, D. D. 2003, PASP, 115, 688, doi: 10.1086/375502

    work page doi:10.1086/375502 2003

  20. [20]

    2000, ApJ, 531, 159, doi: 10.1086/308445

    Franx, M. 2000, ApJ, 531, 159, doi: 10.1086/308445

    work page doi:10.1086/308445 2000

  21. [21]

    2007, ApJS, 169, 83, doi: 10.1086/511270

    Lanz, T., & Hubeny, I. 2007, ApJS, 169, 83, doi: 10.1086/511270

    work page doi:10.1086/511270 2007

  22. [22]

    E., Valli, R., et al

    Lechien, T., de Mink, S. E., Valli, R., et al. 2025, ApJL, 990, L51, doi: 10.3847/2041-8213/adfdd4

    work page doi:10.3847/2041-8213/adfdd4 2025

  23. [23]

    Malkov, O. Y. 2007, MNRAS, 382, 1073, doi: 10.1111/j.1365-2966.2007.12086.x

    work page doi:10.1111/j.1365-2966.2007.12086.x 2007

  24. [24]

    2013, ApJ, 778, 95, doi: 10.1088/0004-637X/778/2/95

    Moe, M., & Di Stefano, R. 2013, ApJ, 778, 95, doi: 10.1088/0004-637X/778/2/95

    work page doi:10.1088/0004-637x/778/2/95 2013

  25. [25]

    2015a, ApJ, 801, 113, doi: 10.1088/0004-637X/801/2/113

    Moe, M., & Di Stefano, R. 2015a, ApJ, 801, 113, doi: 10.1088/0004-637X/801/2/113

    work page doi:10.1088/0004-637x/801/2/113

  26. [26]

    2015b, ApJ, 810, 61, doi: 10.1088/0004-637X/810/1/61

    Moe, M., & Di Stefano, R. 2015b, ApJ, 810, 61, doi: 10.1088/0004-637X/810/1/61

    work page doi:10.1088/0004-637x/810/1/61

  27. [27]

    2017, A&A, 606, A92, doi: 10.1051/0004-6361/201730613

    Mowlavi, N., Lecoeur-Ta¨ ıbi, I., Holl, B., et al. 2017, A&A, 606, A92, doi: 10.1051/0004-6361/201730613

    work page doi:10.1051/0004-6361/201730613 2017

  28. [28]

    2023, A&A, 674, A16, doi: 10.1051/0004-6361/202245330 Naz´ e, Y., Rauw, G., Ko laczek-Szyma´ nski, P

    Mowlavi, N., Holl, B., Lecoeur-Ta¨ ıbi, I., et al. 2023, A&A, 674, A16, doi: 10.1051/0004-6361/202245330 Naz´ e, Y., Rauw, G., Ko laczek-Szyma´ nski, P. A., Britavskiy, N., & Labadie-Bartz, J. 2025, A&A, 703, A239, doi: 10.1051/0004-6361/202556441

    work page doi:10.1051/0004-6361/202245330 2023

  29. [29]

    H., & Tessema, S

    Negu, S. H., & Tessema, S. B. 2018, Astronomische Nachrichten, 339, 709, doi: 10.1002/asna.201813533

    work page doi:10.1002/asna.201813533 2018

  30. [30]

    I - Formation of electron-degenerate O + NE + MG cores

    Nomoto, K. 1984, ApJ, 277, 791, doi: 10.1086/161749

    work page doi:10.1086/161749 1984

  31. [31]

    nat , keywords =

    Nomoto, K., Sparks, W. M., Fesen, R. A., et al. 1982, Nature, 299, 803, doi: 10.1038/299803a0

    work page doi:10.1038/299803a0 1982

  32. [32]

    Offner, S. S. R., Moe, M., Kratter, K. M., et al. 2023, in Astronomical Society of the Pacific Conference Series, Vol. 534, Protostars and Planets VII, ed. S. Inutsuka, Y. Aikawa, T. Muto, K. Tomida, & M. Tamura, 275, doi: 10.48550/arXiv.2203.10066

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2203.10066 2023

  33. [33]

    The OGLE Collection of Variable Stars. Eclipsing Binaries in the Magellanic System

    Pawlak, M., Soszy´ nski, I., Udalski, A., et al. 2016, AcA, 66, 421, doi: 10.48550/arXiv.1612.06394

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1612.06394 2016

  34. [34]

    Petrovic, J., Langer, N., & van der Hucht, K. A. 2005, A&A, 435, 1013, doi: 10.1051/0004-6361:20042368 Pietrzy´ nski, G., Graczyk, D., Gallenne, A., et al. 2019, Nature, 567, 200, doi: 10.1038/s41586-019-0999-4

    work page doi:10.1051/0004-6361:20042368 2005

  35. [35]

    2024, Bulletin de la Societe Royale des Sciences de Liege, 93, 4, doi: 10.25518/0037-9565.12243

    Pigulski, A. 2024, Bulletin de la Societe Royale des Sciences de Liege, 93, 4, doi: 10.25518/0037-9565.12243

    work page doi:10.25518/0037-9565.12243 2024

  36. [36]

    Pols, O. R. 1994, A&A, 290, 119 Prˇ sa, A., Pepper, J., & Stassun, K. G. 2011, AJ, 142, 52, doi: 10.1088/0004-6256/142/2/52 Prˇ sa, A., & Zwitter, T. 2005, ApJ, 628, 426, doi: 10.1086/430591

    work page doi:10.1088/0004-6256/142/2/52 1994

  37. [37]

    G., Tammann, G

    Richter, O. G., Tammann, G. A., & Huchtmeier, W. K. 1987, A&A, 171, 33 Ruci´ nski, S. M. 1969, AcA, 19, 245

    1987

  38. [38]

    Schneider, F. R. N., Izzard, R. G., Langer, N., & de Mink, S. E. 2015, ApJ, 805, 20, doi: 10.1088/0004-637X/805/1/20 Sch¨ urmann, C., Langer, N., Kramer, J. A., et al. 2024, A&A, 690, A282, doi: 10.1051/0004-6361/202450353

    work page doi:10.1088/0004-637x/805/1/20 2015

  39. [39]

    , keywords =

    Sen, K., Langer, N., Marchant, P., et al. 2022, A&A, 659, A98, doi: 10.1051/0004-6361/202142574

    work page doi:10.1051/0004-6361/202142574 2022

  40. [40]

    2018, A&A, 614, A99, doi: 10.1051/0004-6361/201732502

    Siess, L., & Lebreuilly, U. 2018, A&A, 614, A99, doi: 10.1051/0004-6361/201732502

    work page doi:10.1051/0004-6361/201732502 2018

  41. [41]

    M., Skowron, J., Udalski, A., et al

    Skowron, D. M., Skowron, J., Udalski, A., et al. 2021, ApJS, 252, 23, doi: 10.3847/1538-4365/abcb81

    work page doi:10.3847/1538-4365/abcb81 2021

  42. [42]

    The OGLE Collection of Variable Stars. Over 450 000 Eclipsing and Ellipsoidal Binary Systems Toward the Galactic Bulge

    Smith, N. 2013, MNRAS, 434, 102, doi: 10.1093/mnras/stt1004 Soszy´ nski, I., Pawlak, M., Pietrukowicz, P., et al. 2016, AcA, 66, 405, doi: 10.48550/arXiv.1701.03105

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1004 2013

  43. [43]

    The Optical Gravitational Lensing Experiment. OGLE-III Photometric Maps of the Large Magellanic Cloud

    Udalski, A., Soszynski, I., Szymanski, M. K., et al. 2008, AcA, 58, 89, doi: 10.48550/arXiv.0807.3889 University of Wyoming Advanced Research Computing Center. 2018, UW ARCC MedicineBow High Performance Compute Cluster, University of Wyoming, doi: 10.15786/M2FY47 Van Hamme, W. 1993, AJ, 106, 2096, doi: 10.1086/116788 van Rensbergen, W., & de Greve, J.-P. ...

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.0807.3889 2008

  44. [44]

    E., et al

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Methods, 17, 261, doi: 10.1038/s41592-019-0686-2

    work page doi:10.1038/s41592-019-0686-2 2020

  45. [45]

    H., Zhu, L

    Wang, Z. H., Zhu, L. Y., & Yue, Y. F. 2022, MNRAS, 511, 488, doi: 10.1093/mnras/stac037

    work page doi:10.1093/mnras/stac037 2022

  46. [46]

    2001, A&A, 369, 939, doi: 10.1051/0004-6361:20010151

    Wellstein, S., Langer, N., & Braun, H. 2001, A&A, 369, 939, doi: 10.1051/0004-6361:20010151

    work page doi:10.1051/0004-6361:20010151 2001

  47. [47]

    2013, PASJ, 65, 45, doi: 10.1093/pasj/65.2.45

    Yang, Y.-G., Dai, H.-F., He, J.-J., Zhang, J., & Ding, W. 2013, PASJ, 65, 45, doi: 10.1093/pasj/65.2.45

    work page doi:10.1093/pasj/65.2.45 2013

  48. [48]

    E., Izzard, R

    Zapartas, E., de Mink, S. E., Izzard, R. G., et al. 2017, A&A, 601, A29, doi: 10.1051/0004-6361/201629685

    work page doi:10.1051/0004-6361/201629685 2017

  49. [49]

    B., & Grebel, E

    Zaritsky, D., Harris, J., Thompson, I. B., & Grebel, E. K. 2004, AJ, 128, 1606, doi: 10.1086/423910

    work page doi:10.1086/423910 2004