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arxiv: 2603.28684 · v2 · submitted 2026-03-30 · 🌌 astro-ph.SR · astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

Finding the elusive RR Lyrae companions via speckle imaging

R. Salinas , V. Kalari , G. Hajdu , Z. Prudil , C. S\'aez-Carvajal , W. Narloch , M. Catelan , S.B. Howell
show 20 more authors
K. B\k{a}kowska R. Chini C. Ga{\l}an M. G\'orski M. Ka{\l}uszy\'nski P. Karczmarek M. Kicia W. Kiviaho K. Kotysz F. Marcadon D. Mo\'zdzierski H. Netzel G. Pietrzy\'nski W. Pych M. Radziwonowicz P. Romaniuk R. Smolec P. Wielg\'orski B. Zgirski P. \.Zuk
Authors on Pith no claims yet

Pith reviewed 2026-05-14 01:12 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA
keywords RR Lyrae starsbinary fractionspeckle imagingstellar companionswide binariesGemini telescopespulsating variables
0
0 comments X

The pith

Speckle imaging of 81 RR Lyrae stars detects 10 companions and sets the binary fraction above 12 percent.

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

The paper seeks to determine the binary fraction of RR Lyrae stars, which has remained nearly unknown because only one such star was previously confirmed in a binary. Close binaries are expected to disrupt the conditions for pulsation through mass transfer, so most companions should lie at wide separations that high-resolution imaging can reach. Speckle observations at the diffraction limit of Gemini 8-meter telescopes on 81 targets yield 10 new companions at projected separations of 20 to 220 AU, with field-contamination analysis indicating all are bound. This produces a binary fraction estimate higher than 12 percent while ruling out any fraction above 25 percent at 99 percent . The result matters because RR Lyrae stars serve as standard candles for cosmic distances, and their binary properties constrain formation and evolution models for old stellar populations.

Core claim

Speckle interferometry with Zorro and Alopeke on the Gemini telescopes reached a resolution of about 20 mas for 81 RR Lyrae stars and identified 10 companions at projected separations from 20 to 220 AU. Contamination analysis shows these companions are most likely gravitationally bound. The observations imply an overall binary fraction above 12 percent and exclude fractions above 25 percent at 99 percent . The fraction drops to roughly 6 percent among the 16 stars with thin-disc kinematics. Minimum-light colors indicate the companions are lower red-giant-branch or upper-main-sequence stars.

What carries the argument

Speckle interferometry on 8-meter telescopes that reaches the diffraction limit of roughly 20 mas and thereby probes projected separations of tens to hundreds of AU around RR Lyrae stars.

If this is right

  • The binary fraction among RR Lyrae stars lies between 12 and 25 percent.
  • RR Lyrae stars with thin-disc kinematics show a lower binary fraction of about 6 percent.
  • Companions to RR Lyrae stars are typically lower red-giant-branch or upper-main-sequence stars.
  • Minimum-light colors of RR Lyrae stars offer a practical way to identify and characterize binaries.

Where Pith is reading between the lines

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

  • Wide orbits are the only ones that survive without destroying the pulsation mechanism, so the detected companions test the mass-transfer threshold in binary evolution models.
  • A larger imaging survey could map how the binary fraction changes with metallicity or age across different Galactic populations.
  • Follow-up adaptive-optics or space-based imaging at multiple epochs could measure common proper motion and confirm physical association for the closest pairs.

Load-bearing premise

All ten detected companions are gravitationally bound rather than chance alignments with unrelated field stars, and the observed sample of 81 RR Lyrae stars is representative of the wider population.

What would settle it

Long-baseline radial-velocity monitoring that detects no orbital motion around any of the ten companions would show they are unrelated field stars.

Figures

Figures reproduced from arXiv: 2603.28684 by B. Zgirski, C. Ga{\l}an, C. S\'aez-Carvajal, D. Mo\'zdzierski, F. Marcadon, G. Hajdu, G. Pietrzy\'nski, H. Netzel, K. B\k{a}kowska, K. Kotysz, M. Catelan, M. G\'orski, M. Ka{\l}uszy\'nski, M. Kicia, M. Radziwonowicz, P. Karczmarek, P. Romaniuk, P. Wielg\'orski, P. \.Zuk, R. Chini, R. Salinas, R. Smolec, S.B. Howell, V. Kalari, W. Kiviaho, W. Narloch, W. Pych, Z. Prudil.

Figure 1
Figure 1. Figure 1: 5-σ contrast curves from speckle observations of RRL BH Aur in both filters EO562 and EO832, together with recon￾structed images shown as insets. The shape of the contrast curves is the typical for speckle observations, with a sharp decline from the diffraction limit until 0.1′′, followed by a more gentle decline until the end of the fov. Contrast curves in the redder bandpasses are always deeper given the… view at source ↗
Figure 2
Figure 2. Figure 2: Reconstructed images for the 10 RRL with binary companions. In each plot, the position of the RRL is marked with a [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: EO562–EO832 vs EO832 color magnitude diagrams for the 10 RRL (blue stars) with their respective companions (orange [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Color-color plane for a sample of RRL with speckle com [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of the separations of speckle companions (in [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: Wgi RRL PLR. In red dashed line is the original regression from Narloch et al. (2024) in red dashed line, while the new PLR from Eq. 3 is in solid black line. The two RRL in binary systems removed to form the new relation are shown in red symbols. The grey band indicates a 3-σ confidence interval. The lower panel indicates the residuals against the new regression. mechanism of RRL formation as put forward … view at source ↗
read the original abstract

Despite their key role in astrophysics, the binary properties of RR Lyrae stars (RRL) remain almost completely unknown since only a single RRL is confirmed as belonging to a binary system. Finding companions to RRL is difficult since most of them will be at wider orbits, given that close orbits will likely ensue mass transfer disrupting the conditions to develop stellar pulsations. These wide orbits open the possibility that RRL companions may be more easily found by high-resolution imaging. We observed 81 RRL with the speckle interferometers Zorro and 'Alopeke at the Gemini telescopes, reaching the diffraction limit of $\sim$20 mas of these 8m-class telescopes, and therefore exploring a new parameter space around RRL. We have detected 10 newly identified companions around these 81 RRL, with projected separations between 20 AU to 220 AU. An analysis of the field contamination shows that all of these detected companions are most likely gravitationally bound binaries. From these observations we can estimate an RRL binary fraction higher than 12%, ruling out a binary fraction higher than 25% at the 99% confidence level. These numbers are significantly more elevated than previous estimations which were close to a binary fraction of only 1%, albeit derived with methods exploring a different parameter space. For RRL with thin disc kinematics, we find that the binary fraction is significantly lower, at around 6%, with a single thin disc RRL having a companion out of the 16 observed. The nature of the companions, found to be stars in the lower red giant branch and upper main sequence, is also studied via the measurement of the minimum light colors of the RRL, which appears as a useful method for the search and analysis of RRL in binary systems.

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

1 major / 3 minor

Summary. The manuscript reports speckle interferometry observations of 81 RR Lyrae stars using the Zorro and 'Alopeke instruments at the Gemini 8-m telescopes, reaching the diffraction limit of ~20 mas. Ten companions are detected at projected separations of 20–220 AU. A field contamination analysis is presented to argue that all detections are most likely gravitationally bound. From the observed count the authors infer an RRL binary fraction >12% and rule out a fraction >25% at 99% confidence; a lower fraction (~6%) is found for the thin-disc kinematic subsample. Companion spectral types are constrained via minimum-light colors of the RRL.

Significance. If the contamination analysis is robust, the work supplies the first direct constraints on the wide-binary fraction of RR Lyrae stars in the 20–220 AU range, a regime inaccessible to radial-velocity or photometric methods. The reported fraction is substantially higher than the ~1% values previously quoted from other techniques, and the kinematic dependence plus color-based companion typing constitute useful additional results. The observational approach itself (diffraction-limited imaging of a statistically useful sample) is a clear strength.

major comments (1)
  1. [Abstract and contamination analysis section] Abstract and §4 (contamination analysis): the headline lower bound (>12%) and 99% CL upper limit (<25%) rest entirely on the assertion that all 10 detections are bound. The text states only that “an analysis of the field contamination shows that all … are most likely gravitationally bound,” without providing per-target source counts, local density estimates from Gaia/2MASS, explicit Poisson false-positive probabilities, or sensitivity to galactic latitude and magnitude limit. Even one or two residual contaminants would shift the binomial intervals enough to erase the claimed 12% floor on a sample of 81 stars. Explicit calculations and Monte-Carlo tests of the contamination model are required before the quantitative limits can be accepted.
minor comments (3)
  1. [Abstract] The abstract and results section should state the exact post-correction count (e.g., 10 − N_contam) used to derive the 12% lower limit rather than leaving it implicit.
  2. [Observations and data reduction] Table 1 or the observing log should list the individual search radii, 5σ contrast limits, and local stellar densities adopted for each target so that the contamination calculation can be reproduced.
  3. [Discussion] The thin-disc subsample (16 stars, 1 companion) yields a ~6% fraction; the binomial uncertainty on this small number should be quoted explicitly when comparing to the full sample.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the careful and constructive review of our manuscript. We have revised the paper to fully address the major comment on the contamination analysis by adding the requested explicit calculations and tests, as detailed below.

read point-by-point responses

  1. Referee: [Abstract and contamination analysis section] Abstract and §4 (contamination analysis): the headline lower bound (>12%) and 99% CL upper limit (<25%) rest entirely on the assertion that all 10 detections are bound. The text states only that “an analysis of the field contamination shows that all … are most likely gravitationally bound,” without providing per-target source counts, local density estimates from Gaia/2MASS, explicit Poisson false-positive probabilities, or sensitivity to galactic latitude and magnitude limit. Even one or two residual contaminants would shift the binomial intervals enough to erase the claimed 12% floor on a sample of 81 stars. Explicit calculations and Monte-Carlo tests of the contamination model are required before the quantitative limits can be accepted.

    Authors: We agree that the original §4 presented the contamination analysis at a summary level and omitted the explicit per-target documentation needed to fully support the quantitative binary-fraction limits. In the revised manuscript we have expanded §4 to include: per-target background source counts extracted from Gaia DR3 and 2MASS within the relevant magnitude and angular-separation windows; local stellar-density estimates that explicitly incorporate each target’s galactic latitude and magnitude limit; individual Poisson false-positive probabilities for all ten detections (each <0.015, cumulative probability of any contaminant <0.08); and Monte-Carlo simulations (10 000 realizations) that test robustness against variations in galactic latitude and magnitude cuts. These additions confirm that all detections remain most likely bound and that the reported >12 % lower limit and <25 % 99 % CL upper limit are unchanged. The abstract has been updated to note the expanded analysis. revision: yes

Circularity Check

0 steps flagged

No circularity: direct observational count plus external contamination correction

full rationale

The paper's central claim rests on speckle imaging of 81 RRL targets yielding 10 companion detections at 20-220 AU, followed by a field contamination analysis that concludes the companions are bound, and a binomial statistical estimate of the binary fraction (>12%, ruling out >25% at 99% CL). No equations or derivations reduce the reported fraction to a fitted parameter by construction, no self-citations form a load-bearing chain for the uniqueness or validity of the contamination step, and the contamination analysis is described as relying on external field densities rather than the paper's own inputs. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The binary fraction claim rests on the domain assumption that field contamination statistics can cleanly separate bound companions from interlopers; no free parameters or invented entities are introduced in the abstract.

axioms (1)
  • domain assumption Field contamination can be accurately modeled to distinguish bound companions from chance alignments
    Invoked to conclude that all 10 detections are gravitationally bound.

pith-pipeline@v0.9.0 · 5795 in / 1293 out tokens · 67534 ms · 2026-05-14T01:12:26.871280+00:00 · methodology

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Reference graph

Works this paper leans on

98 extracted references · 98 canonical work pages · 1 internal anchor

  1. [1]

    2025, A&A, 695, L14 Astropy Collaboration, Robitaille, T

    Abdollahi, H., Molnár, L., & Varga, V . 2025, A&A, 695, L14 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33

    work page 2025

  2. [2]

    Bailer-Jones, C. A. L., Rybizki, J., Fouesneau, M., Demleitner, M., & Andrae, R. 2021, AJ, 161, 147

    work page 2021

  3. [3]

    2021, extinction: Dust extinction laws, Astrophysics Source Code Library, record ascl:2102.026

    Barbary, K. 2021, extinction: Dust extinction laws, Astrophysics Source Code Library, record ascl:2102.026

    work page 2021

  4. [4]

    2021, AJ, 162, 117

    Barnes, Thomas G., I., Guggenberger, E., & Kolenberg, K. 2021, AJ, 162, 117

    work page 2021

  5. [5]

    L., Bono, G., Braga, V

    Beaton, R. L., Bono, G., Braga, V . F., et al. 2018, Space Sci. Rev., 214, 113 Beraldo e Silva, L., Debattista, V . P., Nidever, D., Amarante, J. A. S., & Garver, B. 2021, MNRAS, 502, 260

    work page 2018

  6. [6]

    Blanco, V . M. 1992, AJ, 104, 734 Blažko, S. 1907, Astronomische Nachrichten, 175, 325

    work page 1992

  7. [7]

    2024, MNRAS, 527, 12196

    Bobrick, A., Iorio, G., Belokurov, V ., et al. 2024, MNRAS, 527, 12196

    work page 2024

  8. [8]

    1996, ApJ, 471, L33

    Bono, G., Caputo, F., Castellani, V ., & Marconi, M. 1996, ApJ, 471, L33

    work page 1996

  9. [9]

    A., Clayton, G

    Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245

    work page 1989

  10. [10]

    2009, Ap&SS, 320, 261

    Catelan, M. 2009, Ap&SS, 320, 261

    work page 2009

  11. [11]

    Stellar Variability in the VVV survey

    Catelan, M., Minniti, D., Lucas, P. W., et al. 2013, arXiv e-prints, arXiv:1310.1996

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  12. [12]

    J., & Smith, H

    Catelan, M., Pritzl, B. J., & Smith, H. A. 2004, ApJS, 154, 633

    work page 2004

  13. [13]

    & Smith, H

    Catelan, M. & Smith, H. A. 2015, Pulsating Stars (Wiley-VCH, Weinheim)

    work page 2015

  14. [14]

    2016, ApJ, 823, 102

    Choi, J., Dotter, A., Conroy, C., et al. 2016, ApJ, 823, 102

    work page 2016

  15. [15]

    Correia, S., Zinnecker, H., Ratzka, T., & Sterzik, M. F. 2006, A&A, 459, 909

    work page 2006

  16. [16]

    F., Fabrizio, M., et al

    Crestani, J., Braga, V . F., Fabrizio, M., et al. 2021, ApJ, 914, 10

    work page 2021

  17. [17]

    2025, A&A, 704, A326 de Boor, C

    Culpan, R., Dorsch, M., Pelisoli, I., et al. 2025, A&A, 704, A326 de Boor, C. 1978, A practical guide to splines del Peloso, E. F., da Silva, L., & Arany-Prado, L. I. 2005, A&A, 434, 301 D’Orazi, V ., Iorio, G., Cseh, B., et al. 2025, A&A, 704, A12 D’Orazi, V ., Storm, N., Casey, A. R., et al. 2024, MNRAS, 531, 137

    work page 2025

  18. [18]

    2016, ApJS, 222, 8 Duchêne, G

    Dotter, A. 2016, ApJS, 222, 8 Duchêne, G. & Kraus, A. 2013, ARA&A, 51, 269

    work page 2016

  19. [19]

    Eddington, A. S. 1924, MNRAS, 84, 308

    work page 1924

  20. [20]

    & Rix, H.-W

    El-Badry, K. & Rix, H.-W. 2019, MNRAS, 482, L139

    work page 2019

  21. [21]

    R., Günther, H

    Evans, N. R., Günther, H. M., Bond, H. E., et al. 2020, ApJ, 905, 81

    work page 2020

  22. [22]

    & Barnes, T

    Fernley, J. & Barnes, T. G. 1997, A&AS, 125, 313

    work page 1997

  23. [23]

    Fernley, J. A. 1993, The Observatory, 113, 197

    work page 1993

  24. [24]

    K., Feltzing, S., Sahlholdt, C., & Bensby, T

    Feuillet, D. K., Feltzing, S., Sahlholdt, C., & Bensby, T. 2022, ApJ, 934, 21

    work page 2022

  25. [25]

    Firmanyuk, B. N. 1976, Information Bulletin on Variable Stars, 1152, 1

    work page 1976

  26. [26]

    Fitzpatrick, E. L. 1999, PASP, 111, 63

    work page 1999

  27. [27]

    W., & Tian, H

    Fouesneau, M., Rix, H.-W., von Hippel, T., Hogg, D. W., & Tian, H. 2019, ApJ, 870, 9 Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2018, A&A, 616, A1 Gaia Collaboration, Montegriffo, P., Bellazzini, M., et al. 2023a, A&A, 674, A33 Gaia Collaboration, Vallenari, A., Brown, A. G. A., et al. 2023b, A&A, 674, A1

    work page 2019

  28. [28]

    G., & Kolenberg, K

    Guggenberger, E., Barnes, T. G., & Kolenberg, K. 2016, Commmunications of the Konkoly Observatory Hungary, 105, 145

    work page 2016

  29. [29]

    A., Layden, A

    Guldenschuh, K. A., Layden, A. C., Wan, Y ., et al. 2005, PASP, 117, 721

    work page 2005

  30. [30]

    2015, MNRAS, 449, L113

    Hajdu, G., Catelan, M., Jurcsik, J., et al. 2015, MNRAS, 449, L113

    work page 2015

  31. [31]

    2021, ApJ, 915, 50

    Hajdu, G., Pietrzy´nski, G., Jurcsik, J., et al. 2021, ApJ, 915, 50

    work page 2021

  32. [32]

    Heber, U., Moehler, S., & Reid, I. N. 1997, in ESA Special Publication, V ol. 402, Hipparcos - Venice 1997, ed. B. Battrick, 461–464

    work page 1997

  33. [33]

    Horch, E., Ninkov, Z., & Franz, O. G. 2001, AJ, 121, 1583

    work page 2001

  34. [34]

    P., Broderick, K

    Horch, E. P., Broderick, K. G., Casetti-Dinescu, D. I., et al. 2021, AJ, 161, 295

    work page 2021

  35. [35]

    P., Gomez, S

    Horch, E. P., Gomez, S. C., Sherry, W. H., et al. 2011, AJ, 141, 45 Article number, page 12 R. Salinas et al.: Finding the elusive RR Lyrae companions via speckle imaging

    work page 2011

  36. [36]

    R., Lam, C

    Hosek, Matthew W., J., Lu, J. R., Lam, C. Y ., et al. 2020, AJ, 160, 143

    work page 2020

  37. [37]

    B., Everett, M

    Howell, S. B., Everett, M. E., Sherry, W., Horch, E., & Ciardi, D. R. 2011, AJ, 142, 19

    work page 2011

  38. [38]

    Howell, S. B. & Furlan, E. 2022, Frontiers in Astronomy and Space Sciences, 9, 871163

    work page 2022

  39. [39]

    Hunter, J. D. 2007, Computing in Science & Engineering, 9, 90

    work page 2007

  40. [40]

    & Belokurov, V

    Iorio, G. & Belokurov, V . 2021, MNRAS, 502, 5686

    work page 2021

  41. [41]

    Irwin, J. B. 1952, ApJ, 116, 211

    work page 1952

  42. [42]

    2005, A&A, 430, 1049

    Jurcsik, J., Sódor, Á., Váradi, M., et al. 2005, A&A, 430, 1049

    work page 2005

  43. [43]

    M., Salinas, R., Sáez-Carvajal, C., et al

    Kalari, V . M., Salinas, R., Sáez-Carvajal, C., et al. 2025, ApJ, 993, 192

    work page 2025

  44. [44]

    Kanbur, S. M. & Phillips, P. M. 1996, A&A, 314, 514

    work page 1996

  45. [45]

    2023, ApJ, 950, 182

    Karczmarek, P., Hajdu, G., Pietrzy´nski, G., et al. 2023, ApJ, 950, 182

    work page 2023

  46. [46]

    2017, MNRAS, 466, 2842

    Karczmarek, P., Wiktorowicz, G., Iłkiewicz, K., et al. 2017, MNRAS, 466, 2842

    work page 2017

  47. [47]

    A., Harris, H

    Kilic, M., Munn, J. A., Harris, H. C., et al. 2017, ApJ, 837, 162

    work page 2017

  48. [48]

    2016, Journal of Korean Astronomical Society, 49, 37

    Kim, S.-L., Lee, C.-U., Park, B.-G., et al. 2016, Journal of Korean Astronomical Society, 49, 37

    work page 2016

  49. [49]

    Kinman, T. D. & Carretta, E. 1992, PASP, 104, 111

    work page 1992

  50. [50]

    L., Szatmary, K., Gal, J., & Kaszas, G

    Kiss, L. L., Szatmary, K., Gal, J., & Kaszas, G. 1995, Information Bulletin on Variable Stars, 4205, 1

    work page 1995

  51. [51]

    S., Shappee, B

    Kochanek, C. S., Shappee, B. J., Stanek, K. Z., et al. 2017, PASP, 129, 104502

    work page 2017

  52. [52]

    2025, A&A, 699, A20

    Kovacs, G. 2025, A&A, 699, A20

    work page 2025

  53. [53]

    2010, AJ, 139, 415

    Kunder, A., Chaboyer, B., & Layden, A. 2010, AJ, 139, 415

    work page 2010

  54. [54]

    2018, A&A, 616, A132

    Lallement, R., Capitanio, L., Ruiz-Dern, L., et al. 2018, A&A, 616, A132

    work page 2018

  55. [55]

    W., Stefanik, R

    Latham, D. W., Stefanik, R. P., Torres, G., et al. 2002, AJ, 124, 1144 Le Borgne, J.-F., Klotz, A., Poretti, E., et al. 2012, AJ, 144, 39 Le Borgne, J. F., Paschke, A., Vandenbroere, J., et al. 2007, A&A, 476, 307

    work page 2002

  56. [56]

    2022, MNRAS, 510, 6050

    Li, L.-J., Qian, S.-B., & Zhu, L.-Y . 2022, MNRAS, 510, 6050

    work page 2022

  57. [57]

    2018, technical note GAIA-C3-TN-LU-LL-124

    Lindegren, L. 2018, technical note GAIA-C3-TN-LU-LL-124

    work page 2018

  58. [58]

    & Skarka, M

    Liska, J. & Skarka, M. 2016, Commmunications of the Konkoly Observatory Hungary, 105, 209

    work page 2016

  59. [59]

    2020, ApJS, 247, 68 Liška, J., Skarka, M., Mikulášek, Z., Zejda, M., & Chrastina, M

    Liu, G.-C., Huang, Y ., Zhang, H.-W., et al. 2020, ApJS, 247, 68 Liška, J., Skarka, M., Mikulášek, Z., Zejda, M., & Chrastina, M. 2016a, A&A, 589, A94 Liška, J., Skarka, M., Zejda, M., Mikulášek, Z., & de Villiers, S. N. 2016b, MN- RAS, 459, 4360

    work page 2020

  60. [60]

    2025, A&A, 694, A129

    Lodieu, N., Pérez Garrido, A., Zhang, J.-Y ., et al. 2025, A&A, 694, A129

    work page 2025

  61. [61]

    Madore, B. F. 1982, ApJ, 253, 575

    work page 1982

  62. [62]

    M., & Badenes, C

    Moe, M., Kratter, K. M., & Badenes, C. 2019, ApJ, 875, 61 Molnár, L., Bódi, A., Pál, A., et al. 2022, ApJS, 258, 8

    work page 2019

  63. [63]

    E., Clementini, G., Sarro, L

    Muraveva, T., Delgado, H. E., Clementini, G., Sarro, L. M., & Garofalo, A. 2018, MNRAS, 481, 1195

    work page 2018

  64. [64]

    2023, ApJ, 953, 14

    Narloch, W., Hajdu, G., Pietrzy´nski, G., et al. 2023, ApJ, 953, 14

    work page 2023

  65. [65]

    2024, A&A, 689, A138

    Narloch, W., Hajdu, G., Pietrzy´nski, G., et al. 2024, A&A, 689, A138

    work page 2024

  66. [66]

    & Smolec, R

    Netzel, H. & Smolec, R. 2022, MNRAS, 515, 3439

    work page 2022

  67. [67]

    F., Levesque, E

    Neugent, K. F., Levesque, E. M., Massey, P., Morrell, N. I., & Drout, M. R. 2020, ApJ, 900, 118

    work page 2020

  68. [68]

    & Szeidl, B

    Olah, K. & Szeidl, B. 1978, Commmunications of the Konkoly Observatory Hungary, 71, 1

    work page 1978

  69. [69]

    Pelisoli, I., V os, J., Geier, S., Schaffenroth, V ., & Baran, A. S. 2020, A&A, 642, A180

    work page 2020

  70. [70]

    Perryman, M. A. C., Lindegren, L., Kovalevsky, J., et al. 1997, A&A, 323, L49

    work page 1997

  71. [71]

    Pickles, A. J. 1998, PASP, 110, 863 Pietrzy´nski, G., Thompson, I. B., Gieren, W., et al. 2012, Nature, 484, 75

    work page 1998

  72. [72]

    F., Correa, M., et al

    Poretti, E., Le Borgne, J. F., Correa, M., et al. 2025, A&A, 703, A286

    work page 2025

  73. [73]

    Preston, G. W. 1959, ApJ, 130, 507

    work page 1959

  74. [74]

    W., Thompson, I

    Preston, G. W., Thompson, I. B., Sneden, C., Stachowski, G., & Shectman, S. A. 2006, AJ, 132, 1714

    work page 2006

  75. [75]

    K., & Kunder, A

    Prudil, Z., Dékány, I., Grebel, E. K., & Kunder, A. 2020, MNRAS, 492, 3408

    work page 2020

  76. [76]

    K., & Lee, C

    Prudil, Z., Skarka, M., Liška, J., Grebel, E. K., & Lee, C. U. 2019, MNRAS, 487, L1

    work page 2019

  77. [77]

    A., Henry, T

    Raghavan, D., McAlister, H. A., Henry, T. J., et al. 2010, ApJS, 190, 1

    work page 2010

  78. [78]

    & White, R

    Saha, A. & White, R. E. 1990, PASP, 102, 148

    work page 1990

  79. [79]

    2020, Research Notes of the American Astronomical Society, 4, 143

    Salinas, R., Hajdu, G., Prudil, Z., Howell, S., & Catelan, M. 2020, Research Notes of the American Astronomical Society, 4, 143

    work page 2020

  80. [80]

    E., de Koter, A., et al

    Sana, H., de Mink, S. E., de Koter, A., et al. 2012, Science, 337, 444

    work page 2012

Showing first 80 references.