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arxiv: 2606.26219 · v1 · pith:ZBNXF6DKnew · submitted 2026-06-24 · 🌌 astro-ph.SR · astro-ph.GA

Connecting Stellar Population Surveys to Stellar Evolution with Delay-time Distributions: Application to LMC Classical Cepheids

Sumit K. Sarbadhicary This is my paper

Pith reviewed 2026-06-26 01:25 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA
keywords delay-time distributionclassical CepheidsLMCstar formation historystellar evolutionprogenitor agesOGLE surveyperiod-age relations
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The pith

Delay-time distributions from LMC star-formation maps recover Cepheid progenitor ages at 20-200 Myr and align with non-canonical models.

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

This paper applies the delay-time distribution technique, normally used for transients, to classical Cepheids in the LMC whose ages can be checked independently through period relations. It combines the OGLE-IV Cepheid catalog with optical and near-infrared SFH maps to extract the age distribution of the progenitors. The resulting DTDs show clear signals at 20-200 Myr for fundamental-mode Cepheids and 125-200 Myr for first-overtone ones. These peaks match the ages inferred from period-age-color relations and sit closer to predictions from models that include convective overshooting and rotational mixing than to canonical models. The work positions DTDs as a bridge between resolved stellar population surveys and tests of stellar evolution physics.

Core claim

The measured DTDs from optical SFH maps show significant detections at ages of 20-200 Myr for FU Cepheids, and 125-200 Myr for FO Cepheids. These are consistent with independently measured ages from the period-age-color relations, with the DTD peak being more consistent with relations from non-canonical models that include effects of overshooting, rotational mixing etc. An outlier population of 0.5-0.8 Gyr of FU Cepheids is also detected in the DTD, though its veracity is debatable given the brightness and pulsation periods of FU Cepheids, and because the signal is not recovered with DTDs derived from near-infrared SFH.

What carries the argument

The delay-time distribution (DTD), which extracts the progenitor age distribution and production rates of a stellar phenomenon from galaxy star-formation history maps.

If this is right

  • DTDs of stars with well-constrained progenitors such as Cepheids and RR Lyrae can provide independent verification of the derived SFHs in upcoming surveys.
  • The technique offers a route to investigate progenitor scenarios for supernovae, evolved giants, planetary nebulae and AGB stars by confronting uncertainties in mass-loss, binary evolution, rotation, mixing and overshooting.
  • An outlier 0.5-0.8 Gyr signal for FU Cepheids appears in optical DTDs but is absent in near-infrared versions and conflicts with expected brightness and periods.

Where Pith is reading between the lines

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

  • If DTDs successfully recover known Cepheid ages, the same maps could be used to constrain binary channels for other transients whose progenitors lack direct age indicators.
  • Extending the method to additional galaxies at different metallicities would test whether the preference for non-canonical models holds across environments.
  • Cross-validation between DTD ages and period relations could flag systematic biases in SFH map construction for age ranges where Cepheids are abundant.

Load-bearing premise

The optical and near-infrared SFH maps accurately capture the LMC star-formation history in the relevant age bins without large systematic errors that would distort the recovered DTD.

What would settle it

If the DTD peaks derived from the same SFH maps fail to align with the independently measured ages from period-age-color relations in the same sample, the claimed consistency would not hold.

Figures

Figures reproduced from arXiv: 2606.26219 by Sumit K. Sarbadhicary.

Figure 1
Figure 1. Figure 1: — Left: Spatial distribution of fundamental (FU, orange) and first overtone (FO, purple) Cepheids from Jacyszyn-Dobrzeniecka et al. (2016, J16), overlaid on the stellar age distribution (SFH) map from Harris & Zaritsky (2009, HZ09). Right: The measured DTD of the FU and FO Classical Cepheids from J16, given the SFH map from HZ09. Solid colors represent age bins where a statistically significant signal is d… view at source ↗
Figure 2
Figure 2. Figure 2: — Visual comparison of the stellar mass surface density formed at three different lookback times in the HZ09 SFH map, with the distribution of FU+FO Cepheids from J16, both shown in orange. We show the total mass formed in three representative lookback time ranges: 0-20 Myr (left), 20-200 Myr (middle) and 200 Myr-16 Gyr (right panel). Star-formation at 20-200 Myr appears best correlated with the Cepheid di… view at source ↗
Figure 3
Figure 3. Figure 3: — Comparison between the DTD and the independently measured ages of FU (left) and FO (right) Cepheids from the theoretical period-age (PA) and period-age color (PAC) relations of De Somma et al. (2021, DS21). The grey histograms show the DTD-based age distribution of Cepheids (grey), obtained from convolving the DTDs in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: — Mean reddening-corrected I vs V − I photometry of FU (brown) and FO (purple) Cepheids, and comparison with PARSEC v2.0 isochrones for different ages and two metallicities, [M/H]=[−0.5, −1.0], covering the lower range expected in the LMC. The comparison here broadly validates the ages being recov￾ered by the DTDs in Figures 1-3, though see discussion in Section 3. 1. We checked if this signal is a false p… view at source ↗
Figure 5
Figure 5. Figure 5: — Left: The J16 Classical Cepheid population in the LMC shown on the Mazzi et al. (2021, referred to as M21) SFH map, with spatial cells shown in grey. Right: The DTD for FU and FO Cepheids derived from the M21 SFH map (filled histogram + upper limits) and comparison with the HZ09-based DTDs from [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
read the original abstract

The progenitors of many stellar-origin phenomena such as supernovae, evolved giants and supergiants, planetary nebulae, AGB stars and other post-main-sequence exotica remain poorly understood due to stellar evolution uncertainties such as mass-loss, binary evolution, rotation, mixing, and overshooting. A promising technique for investigating stellar progenitor scenarios with resolved stellar population surveys of galaxies is the delay-time distribution (DTD). Given a survey of stellar phenomena of interest, the DTD extracts the progenitor age distribution and production rates of the phenomena from star-formation history (SFH) maps of galaxies. Here we test the potential of DTDs as a stellar evolution diagnostic by applying to stars with known ages -- Classical Cepheids in the LMC. We use the high-completeness OGLE-IV survey of Cepheids, and LMC SFH maps from optical and near-infrared surveys. The measured DTDs from optical SFH maps show significant detections at ages of 20-200 Myr for FU Cepheids, and 125-200 Myr for FO Cepheids. These are consistent with independently measured ages from the period-age-color relations, with the DTD peak being more consistent with relations from non-canonical models that include effects of overshooting, rotational mixing etc. An outlier population of 0.5-0.8 Gyr of FU Cepheids is also detected in the DTD, though its veracity is debatable given the brightness and pulsation periods of FU Cepheids, and because the signal is not recovered with DTDs derived from near-infrared SFH. For upcoming surveys (e.g. with Roman), DTDs of stars with well-constrained progenitors such as Cepheids and RR Lyrae can provide independent verification of the derived SFHs.

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

3 major / 2 minor

Summary. The paper applies the delay-time distribution (DTD) method to Classical Cepheids in the LMC, using the high-completeness OGLE-IV catalog together with optical and near-infrared SFH maps. It reports significant DTD signals for fundamental-mode Cepheids at 20-200 Myr and first-overtone Cepheids at 125-200 Myr, claims consistency between these DTD peaks and ages inferred from period-age-color relations, and states that the DTD peak aligns better with non-canonical stellar-evolution models that include overshooting and rotational mixing. An additional 0.5-0.8 Gyr feature appears only in the optical-derived DTD and is flagged as potentially spurious. The work positions DTDs of well-characterized tracers as an independent check on SFH maps for future surveys.

Significance. If the central result is robust, the manuscript demonstrates that DTD inversion on resolved populations can serve as an external consistency test for both SFH reconstructions and stellar-evolution prescriptions. This is a concrete, falsifiable link between population surveys and progenitor physics that could be applied to other tracers (RR Lyrae, planetary nebulae) once comparable completeness and age calibration are available. The approach is timely for Roman-era datasets.

major comments (3)
  1. [Abstract and §3] Abstract and §3 (results): the claim of consistency with period-age relations is presented without any quantitative metric (overlap integral, Kolmogorov-Smirnov statistic, or likelihood ratio) comparing the measured DTD to the canonical versus non-canonical model predictions; the statement that the DTD peak is “more consistent” with non-canonical models therefore cannot be evaluated from the supplied information.
  2. [Methods (SFH maps) and §4] Methods (SFH maps) and §4 (discussion): the DTD is obtained by matrix inversion of observed counts against the adopted SFH; the manuscript shows that the 0.5-0.8 Gyr feature disappears when NIR SFH maps are substituted, yet provides no propagated uncertainty budget or Monte-Carlo test of how plausible systematic shifts in the 20-200 Myr optical SFH bins (extinction, isochrone library, age resolution) would move the reported DTD peaks.
  3. [Abstract] Abstract: completeness corrections, photometric error budgets, and the precise handling of the 0.5-0.8 Gyr outlier are not quantified, leaving the statistical significance of the 20-200 Myr and 125-200 Myr detections unstated.
minor comments (2)
  1. The manuscript would benefit from an explicit table or figure panel showing the DTD values with 1σ uncertainties for each age bin so that readers can judge detection significance directly.
  2. Notation for the two SFH map sets (optical vs. NIR) should be standardized throughout the text and figures to avoid ambiguity when comparing results.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thoughtful and constructive report. The comments highlight areas where the manuscript can be strengthened with additional quantitative analysis and uncertainty quantification. We address each major comment below and indicate the revisions planned for the next version.

read point-by-point responses

  1. Referee: [Abstract and §3] Abstract and §3 (results): the claim of consistency with period-age relations is presented without any quantitative metric (overlap integral, Kolmogorov-Smirnov statistic, or likelihood ratio) comparing the measured DTD to the canonical versus non-canonical model predictions; the statement that the DTD peak is “more consistent” with non-canonical models therefore cannot be evaluated from the supplied information.

    Authors: We agree that the consistency claim would benefit from a quantitative metric. In the revised manuscript we will add a direct comparison (e.g., overlap integral or Kolmogorov-Smirnov statistic) between the measured DTD and the age distributions predicted by canonical versus non-canonical period-age relations, allowing readers to evaluate the degree of agreement. revision: yes

  2. Referee: [Methods (SFH maps) and §4] Methods (SFH maps) and §4 (discussion): the DTD is obtained by matrix inversion of observed counts against the adopted SFH; the manuscript shows that the 0.5-0.8 Gyr feature disappears when NIR SFH maps are substituted, yet provides no propagated uncertainty budget or Monte-Carlo test of how plausible systematic shifts in the 20-200 Myr optical SFH bins (extinction, isochrone library, age resolution) would move the reported DTD peaks.

    Authors: We acknowledge that a systematic uncertainty budget is needed. We will add Monte-Carlo realizations that perturb the optical SFH bins within ranges consistent with published uncertainties on extinction, isochrone libraries, and age binning, and will report the resulting spread on the DTD peak locations and amplitudes. revision: yes

  3. Referee: [Abstract] Abstract: completeness corrections, photometric error budgets, and the precise handling of the 0.5-0.8 Gyr outlier are not quantified, leaving the statistical significance of the 20-200 Myr and 125-200 Myr detections unstated.

    Authors: The manuscript references the high completeness of the OGLE-IV catalog but does not provide explicit error propagation or significance values. We will expand the abstract and methods to include (i) a quantitative statement of completeness and photometric error contributions, (ii) Poisson or bootstrap uncertainties on the DTD bins, and (iii) a clearer description of why the 0.5-0.8 Gyr feature is treated as potentially spurious. revision: yes

Circularity Check

0 steps flagged

No circularity: DTD recovered from independent SFH maps and Cepheid counts, then compared to external period-age relations

full rationale

The paper derives DTDs by inverting observed Cepheid counts against adopted optical/NIR SFH maps of the LMC, then reports age bins of significant detection (20-200 Myr for FU, 125-200 Myr for FO) and notes consistency with independently published period-age-color relations from stellar models. No step defines the DTD peak in terms of the same fitted quantities it claims to test, nor does any load-bearing premise reduce to a self-citation chain or ansatz smuggled from prior author work. The central comparison is to external model relations, and the method is self-contained against the provided SFH inputs and counts; map accuracy is an assumption but does not create definitional circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Based solely on abstract; no explicit free parameters, axioms, or invented entities are stated.

axioms (1)
  • domain assumption Delay-time distributions can be reliably extracted from a combination of observed stellar counts and independently derived star-formation history maps.
    This is the foundational premise of the entire method described in the abstract.

pith-pipeline@v0.9.1-grok · 5864 in / 1267 out tokens · 22220 ms · 2026-06-26T01:25:49.730854+00:00 · methodology

discussion (0)

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Works this paper leans on

70 extracted references · 68 canonical work pages · 8 internal anchors

  1. [1]

    S., Badenes, C., Chomiuk, L., et al

    Abelson, C. S., Badenes, C., Chomiuk, L., et al. 2025, ApJ, 984, 134, doi: 10.3847/1538-4357/adc68c

    work page doi:10.3847/1538-4357/adc68c 2025

  2. [2]

    I., Saio, H., Ekstr¨ om, S., Georgy, C., & Meynet, G

    Anderson, R. I., Saio, H., Ekstr¨ om, S., Georgy, C., & Meynet, G. 2016, A&A, 591, A8, doi: 10.1051/0004-6361/201528031

    work page doi:10.1051/0004-6361/201528031 2016

  3. [3]

    J., et al

    Antoniou, V., Zezas, A., Drake, J. J., et al. 2019, ApJ, 887, 20, doi: 10.3847/1538-4357/ab4a7a

    work page doi:10.3847/1538-4357/ab4a7a 2019

  4. [4]

    2015, ApJ, 804, L25, doi: 10.1088/2041-8205/804/1/L25

    Badenes, C., Maoz, D., & Ciardullo, R. 2015, ApJ, 804, L25, doi: 10.1088/2041-8205/804/1/L25

    work page doi:10.1088/2041-8205/804/1/l25 2015

  5. [5]

    Badenes, C., Maoz, D., & Draine, B. T. 2010, MNRAS, 407, 1301, doi: 10.1111/j.1365-2966.2010.17023.x B¨ ohm-Vitense, E., Evans, N. R., Carpenter, K., et al. 1998, ApJ, 505, 903, doi: 10.1086/306177

    work page doi:10.1111/j.1365-2966.2010.17023.x 2010

  6. [6]

    , keywords =

    Bono, G., Braga, V. F., & Pietrinferni, A. 2024, A&A Rev., 32, 4, doi: 10.1007/s00159-024-00153-0

    work page doi:10.1007/s00159-024-00153-0 2024

  7. [7]

    2005, ApJ, 621, 966, doi: 10.1086/427744

    Bono, G., Marconi, M., Cassisi, S., et al. 2005, ApJ, 621, 966, doi: 10.1086/427744

    work page doi:10.1086/427744 2005

  8. [8]

    L., Clementini, G., Girardi, L., et al

    Cioni, M.-R. L., Clementini, G., Girardi, L., et al. 2011, A&A, 527, A116, doi: 10.1051/0004-6361/201016137

    work page doi:10.1051/0004-6361/201016137 2011

  9. [9]

    E., McQuinn, K

    Cohen, R. E., McQuinn, K. B. W., Murray, C. E., et al. 2024, ApJ, 975, 42, doi: 10.3847/1538-4357/ad6cd5

    work page doi:10.3847/1538-4357/ad6cd5 2024

  10. [10]

    doi:10.1088/0004-637X/699/1/486 , eprint =

    Conroy, C., Gunn, J. E., & White, M. 2009, ApJ, 699, 486, doi: 10.1088/0004-637X/699/1/486

    work page internal anchor Pith review doi:10.1088/0004-637x/699/1/486 2009

  11. [11]

    2025, MNRAS, 541, 1434, doi: 10.1093/mnras/staf1095 De Somma, G., Marconi, M., Cassisi, S., et al

    Cuevas-Otahola, B., Mateu, C., Cabrera-Ziri, I., et al. 2025, MNRAS, 541, 1434, doi: 10.1093/mnras/staf1095 De Somma, G., Marconi, M., Cassisi, S., et al. 2021, MNRAS, 508, 1473, doi: 10.1093/mnras/stab2611 De Somma, G., Marconi, M., Ripepi, V., et al. 2025, ApJ, 984, L60, doi: 10.3847/2041-8213/adcf92

    work page doi:10.1093/mnras/staf1095 2025

  12. [12]

    J., & Stanway, E

    Eldridge, J. J., & Stanway, E. R. 2022, ARA&A, 60, 455, doi: 10.1146/annurev-astro-052920-100646

    work page doi:10.1146/annurev-astro-052920-100646 2022

  13. [13]

    Binary Population and Spectral Synthesis Version 2.1: construction, observational verification and new results

    Eldridge, J. J., Stanway, E. R., Xiao, L., et al. 2017, PASA, 34, e058, doi: 10.1017/pasa.2017.51

    work page internal anchor Pith review doi:10.1017/pasa.2017.51 2017

  14. [14]

    W., & Walker, A

    Feast, M. W., & Walker, A. R. 1987, ARA&A, 25, 345, doi: 10.1146/annurev.aa.25.090187.002021

    work page doi:10.1146/annurev.aa.25.090187.002021 1987

  15. [15]

    L., Hughes, S

    Freedman, W. L., Hughes, S. M., Madore, B. F., et al. 1994, ApJ, 427, 628, doi: 10.1086/174172

    work page doi:10.1086/174172 1994

  16. [16]

    L., Madore, B

    Freedman, W. L., Madore, B. F., Gibson, B. K., et al. 2001, ApJ, 553, 47, doi: 10.1086/320638

    work page doi:10.1086/320638 2001

  17. [17]

    2021, MNRAS, 502, 5882, doi: 10.1093/mnras/stab493

    Freundlich, J., & Maoz, D. 2021, MNRAS, 502, 5882, doi: 10.1093/mnras/stab493

    work page doi:10.1093/mnras/stab493 2021

  18. [18]

    2018, MNRAS, 479, 3563, doi: 10.1093/mnras/sty1664

    Friedmann, M., & Maoz, D. 2018, MNRAS, 479, 3563, doi: 10.1093/mnras/sty1664

    work page doi:10.1093/mnras/sty1664 2018

  19. [19]

    2005, ARA&A, 43, 387, doi: 10.1146/annurev.astro.43.072103.150608

    Gallart, C., Zoccali, M., & Aparicio, A. 2005, ARA&A, 43, 387, doi: 10.1146/annurev.astro.43.072103.150608

    work page doi:10.1146/annurev.astro.43.072103.150608 2005

  20. [20]

    2011, MNRAS, 415, 2020, doi: 10.1111/j.1365-2966.2011.18607.x

    Graur, O., Poznanski, D., Maoz, D., et al. 2011, MNRAS, 417, 916, doi: 10.1111/j.1365-2966.2011.19287.x

    work page doi:10.1111/j.1365-2966.2011.19287.x 2011

  21. [21]

    A., Maoz, D., et al

    Graur, O., Rodney, S. A., Maoz, D., et al. 2014, ApJ, 783, 28, doi: 10.1088/0004-637X/783/1/28

    work page doi:10.1088/0004-637x/783/1/28 2014

  22. [22]

    2004, AJ, 127, 1531, doi: 10.1086/381953 —

    Harris, J., & Zaritsky, D. 2004, AJ, 127, 1531, doi: 10.1086/381953 —. 2009, AJ, 138, 1243, doi: 10.1088/0004-6256/138/5/1243

    work page doi:10.1086/381953 2004

  23. [23]

    Hubble, E. P. 1929, ApJ, 69, 103, doi: 10.1086/143167

    work page doi:10.1086/143167 1929

  24. [24]

    1993, PASP, 105, 1373, doi: 10.1086/133321

    Iben, Jr., I., & Livio, M. 1993, PASP, 105, 1373, doi: 10.1086/133321

    work page doi:10.1086/133321 1993

  25. [25]

    2021, MNRAS, 502, 5686, doi: 10.1093/mnras/stab005

    Iorio, G., & Belokurov, V. 2021, MNRAS, 502, 5686, doi: 10.1093/mnras/stab005

    work page doi:10.1093/mnras/stab005 2021

  26. [26]

    OGLE-ing the Magellanic System: Three-Dimensional Structure of the Clouds and the Bridge Using Classical Cepheids

    Jacyszyn-Dobrzeniecka, A. M., Skowron, D. M., Mr´ oz, P., et al. 2016, Acta Astron., 66, 149, doi: 10.48550/arXiv.1602.09141

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1602.09141 2016

  27. [27]

    2022, ApJ, 930, 65, doi: 10.3847/1538-4357/ac6354

    Karczmarek, P., Smolec, R., Hajdu, G., et al. 2022, ApJ, 930, 65, doi: 10.3847/1538-4357/ac6354

    work page doi:10.3847/1538-4357/ac6354 2022

  28. [28]

    R., et al

    Kervella, P., Gallenne, A., Evans, N. R., et al. 2019, A&A, 623, A117, doi: 10.1051/0004-6361/201834211

    work page doi:10.1051/0004-6361/201834211 2019

  29. [29]

    2012, ARA&A, 50, 107, doi: 10.1146/annurev-astro-081811-125534 9

    Langer, N. 2012, ARA&A, 50, 107, doi: 10.1146/annurev-astro-081811-125534 9

    work page doi:10.1146/annurev-astro-081811-125534 2012

  30. [30]

    F., Durbin, M

    Lazzarini, M., Williams, B. F., Durbin, M. J., et al. 2022, ApJ, 934, 76, doi: 10.3847/1538-4357/ac7568

    work page doi:10.3847/1538-4357/ac7568 2022

  31. [31]

    Leavitt, H. S. 1907, Annals of Harvard College Observatory, 60, 87

    1907

  32. [32]

    S., & Pickering, E

    Leavitt, H. S., & Pickering, E. C. 1912, Harvard College Observatory Circular, 173, 1

    1912

  33. [33]

    R., Dolphin, A

    Lewis, A. R., Dolphin, A. E., Dalcanton, J. J., et al. 2015, ApJ, 805, 183, doi: 10.1088/0004-637X/805/2/183

    work page doi:10.1088/0004-637x/805/2/183 2015

  34. [34]

    , keywords =

    Madore, B. F., & Freedman, W. L. 1991, PASP, 103, 933, doi: 10.1086/132911

    work page doi:10.1086/132911 1991

  35. [35]

    2000, ARA&A, 38, 143, doi: 10.1146/annurev.astro.38.1.143

    Maeder, A., & Meynet, G. 2000, ARA&A, 38, 143, doi: 10.1146/annurev.astro.38.1.143

    work page doi:10.1146/annurev.astro.38.1.143 2000

  36. [36]

    Lewin, W. H. G. 1997, A&AS, 126, 401, doi: 10.1051/aas:1997394

    work page doi:10.1051/aas:1997394 1997

  37. [37]

    , keywords =

    Maoz, D., & Badenes, C. 2010, MNRAS, 407, 1314, doi: 10.1111/j.1365-2966.2010.16988.x

    work page doi:10.1111/j.1365-2966.2010.16988.x 2010

  38. [38]

    2012, PASA, 29, 447, doi: 10.1071/AS11052

    Maoz, D., & Mannucci, F. 2012, PASA, 29, 447, doi: 10.1071/AS11052

    work page doi:10.1071/as11052 2012

  39. [39]

    Maoz, D., Mannucci, F., & Brandt, T. D. 2012, MNRAS, 426, 3282, doi: 10.1111/j.1365-2966.2012.21871.x

    work page doi:10.1111/j.1365-2966.2012.21871.x 2012

  40. [40]

    , keywords =

    Maoz, D., Mannucci, F., Li, W., et al. 2011, MNRAS, 412, 1508, doi: 10.1111/j.1365-2966.2010.16808.x

    work page doi:10.1111/j.1365-2966.2010.16808.x 2011

  41. [41]

    2014, ARA&A, 52, 107, doi: 10.1146/annurev-astro-082812-141031

    Maoz, D., Mannucci, F., & Nelemans, G. 2014, ARA&A, 52, 107, doi: 10.1146/annurev-astro-082812-141031

    work page doi:10.1146/annurev-astro-082812-141031 2014

  42. [42]

    2010, ApJ, 722, 1879, doi: 10.1088/0004-637X/722/2/1879

    Maoz, D., Sharon, K., & Gal-Yam, A. 2010, ApJ, 722, 1879, doi: 10.1088/0004-637X/722/2/1879

    work page doi:10.1088/0004-637x/722/2/1879 2010

  43. [43]

    2024, ARA&A, 62, 21, doi: 10.1146/annurev-astro-052722-105936

    Marchant, P., & Bodensteiner, J. 2024, ARA&A, 62, 21, doi: 10.1146/annurev-astro-052722-105936

    work page doi:10.1146/annurev-astro-052722-105936 2024

  44. [44]

    2013, MNRAS, 428, 2185, doi: 10.1093/mnras/sts197

    Marconi, M., Molinaro, R., Ripepi, V., Musella, I., & Brocato, E. 2013, MNRAS, 428, 2185, doi: 10.1093/mnras/sts197

    work page doi:10.1093/mnras/sts197 2013

  45. [45]

    Massana, P., Ruiz-Lara, T., No¨ el, N. E. D., et al. 2022, MNRAS, 513, L40, doi: 10.1093/mnrasl/slac030

    work page doi:10.1093/mnrasl/slac030 2022

  46. [46]

    First direct detection of an RR Lyrae star conclusively associated with an intermediate-age cluster

    Mateu, C., Cuevas-Otahola, B., & Jos´ e Downes, J. 2025, arXiv e-prints, arXiv:2509.22336, doi: 10.48550/arXiv.2509.22336

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2509.22336 2025

  47. [47]

    D., & Pols, O

    Mathieu, R. D., & Pols, O. R. 2025, ARA&A, 63, 467, doi: 10.1146/annurev-astro-071221-054402

    work page doi:10.1146/annurev-astro-071221-054402 2025

  48. [48]

    2021, MNRAS, 508, 245, doi: 10.1093/mnras/stab2399

    Mazzi, A., Girardi, L., Zaggia, S., et al. 2021, MNRAS, 508, 245, doi: 10.1093/mnras/stab2399

    work page doi:10.1093/mnras/stab2399 2021

  49. [49]

    McQuinn, K. B. W., Newman, M. J. B., Skillman, E. D., et al. 2024, ApJ, 976, 60, doi: 10.3847/1538-4357/ad8158

    work page doi:10.3847/1538-4357/ad8158 2024

  50. [50]

    R., Schneider, F

    Neilson, H. R., Schneider, F. R. N., Izzard, R. G., Evans, N. R., & Langer, N. 2015, A&A, 574, A2, doi: 10.1051/0004-6361/201424408 Pietrzy´ nski, G., Thompson, I. B., Gieren, W., et al. 2010, Nature, 468, 542, doi: 10.1038/nature09598

    work page doi:10.1051/0004-6361/201424408 2015

  51. [51]

    , keywords =

    Pilecki, B., Thompson, I. B., Espinoza-Arancibia, F., et al. 2022, ApJ, 940, L48, doi: 10.3847/2041-8213/ac9fcc Prada Moroni, P. G., Gennaro, M., Bono, G., et al. 2012, ApJ, 749, 108, doi: 10.1088/0004-637X/749/2/108

    work page doi:10.3847/2041-8213/ac9fcc 2022

  52. [52]

    2019, MNRAS, 490, 4975, doi: 10.1093/mnras/stz2881

    Ragosta, F., Marconi, M., Molinaro, R., et al. 2019, MNRAS, 490, 4975, doi: 10.1093/mnras/stz2881

    work page doi:10.1093/mnras/stz2881 2019

  53. [53]

    Large Magellanic Cloud Cepheid Standards Provide a 1% Foundation for the Determination of the Hubble Constant and Stronger Evidence for Physics Beyond LambdaCDM

    Riess, A. G., Casertano, S., Yuan, W., Macri, L. M., & Scolnic, D. 2019, ApJ, 876, 85, doi: 10.3847/1538-4357/ab1422

    work page internal anchor Pith review doi:10.3847/1538-4357/ab1422 2019

  54. [54]

    G., et al

    Riess, A. G., Yuan, W., Macri, L. M., et al. 2022, ApJ, 934, L7, doi: 10.3847/2041-8213/ac5c5b

    work page doi:10.3847/2041-8213/ac5c5b 2022

  55. [55]

    L., Moretti, M

    Ripepi, V., Cioni, M.-R. L., Moretti, M. I., et al. 2017, MNRAS, 472, 808, doi: 10.1093/mnras/stx2096

    work page doi:10.1093/mnras/stx2096 2017

  56. [56]

    2018, MNRAS, 478, 5017, doi: 10.1093/mnras/sty1279

    Rubele, S., Pastorelli, G., Girardi, L., et al. 2018, MNRAS, 478, 5017, doi: 10.1093/mnras/sty1279

    work page doi:10.1093/mnras/sty1279 2018

  57. [57]

    2011, MNRAS, 415, 2020, doi: 10.1111/j.1365-2966.2011.18607.x

    Ruiter, A. J., Belczynski, K., Sim, S. A., et al. 2011, MNRAS, 417, 408, doi: 10.1111/j.1365-2966.2011.19276.x

    work page doi:10.1111/j.1365-2966.2011.19276.x 2011

  58. [58]

    K., Heiger, M., Badenes, C., et al

    Sarbadhicary, S. K., Heiger, M., Badenes, C., et al. 2021, ApJ, 912, 140, doi: 10.3847/1538-4357/abca86

    work page doi:10.3847/1538-4357/abca86 2021

  59. [59]

    , keywords =

    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

  60. [60]

    The OGLE Collection of Variable Stars. Classical Cepheids in the Magellanic System

    Smith, N. 2014, ARA&A, 52, 487, doi: 10.1146/annurev-astro-081913-040025 Soszy´ nski, I., Udalski, A., Szyma´ nski, M. K., et al. 2015a, Acta Astron., 65, 297, doi: 10.48550/arXiv.1601.01318 —. 2015b, Acta Astron., 65, 329, doi: 10.48550/arXiv.1601.02020

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081913-040025 2014

  61. [61]

    2020, ApJ, 890, 140, doi: 10.3847/1538-4357/ab6a97

    Graur, O. 2020, ApJ, 890, 140, doi: 10.3847/1538-4357/ab6a97

    work page doi:10.3847/1538-4357/ab6a97 2020

  62. [62]

    and Nelemans, G

    Toonen, S., Nelemans, G., & Portegies Zwart, S. 2012, A&A, 546, A70, doi: 10.1051/0004-6361/201218966

    work page doi:10.1051/0004-6361/201218966 2012

  63. [63]

    OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment

    Udalski, A., Szyma´ nski, M. K., & Szyma´ nski, G. 2015a, Acta Astron., 65, 1, doi: 10.48550/arXiv.1504.05966

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1504.05966

  64. [64]

    Eclipsing Binaries with Classical Cepheid Component in the Magellanic System

    Udalski, A., Soszy´ nski, I., Szyma´ nski, M. K., et al. 2015b, Acta Astron., 65, 341, doi: 10.48550/arXiv.1601.01683

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1601.01683

  65. [65]

    R., Dolphin, A

    Weisz, D. R., Dolphin, A. E., Skillman, E. D., et al. 2013, MNRAS, 431, 364, doi: 10.1093/mnras/stt165 —. 2014, ApJ, 789, 147, doi: 10.1088/0004-637X/789/2/147

    work page doi:10.1093/mnras/stt165 2013

  66. [66]

    F., Dolphin, A

    Williams, B. F., Dolphin, A. E., Dalcanton, J. J., et al. 2017, ApJ, 846, 145, doi: 10.3847/1538-4357/aa862a

    work page doi:10.3847/1538-4357/aa862a 2017

  67. [67]

    2021, MNRAS, 506, 3330, doi: 10.1093/mnras/stab1943

    Wiseman, P., Sullivan, M., Smith, M., et al. 2021, MNRAS, 506, 3330, doi: 10.1093/mnras/stab1943

    work page doi:10.1093/mnras/stab1943 2021

  68. [68]

    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

  69. [69]

    1997, AJ, 114, 1002, doi: 10.1086/118531

    Zaritsky, D., Harris, J., & Thompson, I. 1997, AJ, 114, 1002, doi: 10.1086/118531

    work page doi:10.1086/118531 1997

  70. [70]

    B., & Grebel, E

    Zaritsky, D., Harris, J., Thompson, I. B., & Grebel, E. K. 2004, AJ, 128, 1606, doi: 10.1086/423910 This paper was built using the Open Journal of As- trophysics LATEX template. The OJA is a journal which provides fast and easy peer review for new papers in the astro-phsection of the arXiv, making the reviewing pro- cess simpler for authors and referees a...

    work page doi:10.1086/423910 2004