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The DESI Y1 RR Lyrae catalog II: The metallicity dependency of pulsational properties, the shape of the RR Lyrae instability strip, and metal rich RR Lyrae

T0 review · 3 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read This paper claims that the RR Lyrae instability strip shifts to cooler temperatures as metallicity drops, while its width stays roughly constant, based on the first large spectroscopic sample with phase-corrected temperatures.

desk verdict Largest homogeneous sample yet for RRL instability-strip metallicity trends, with a genuinely new blue-edge result that is plausible but not yet safe from Teff/[Fe/H] calibration systematics; deserves a real referee. read the letter →

arxiv 2505.10614 v2 pith:75BESMC4 submitted 2025-05-15 astro-ph.GA astro-ph.SR

Gustavo E. Medina , Ting S. Li , C. Allende Prieto , L. Beraldo e Silva , A. Bystrom , R. G. Carlberg , S. E. Koposov , M. Lambert
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J. R. Najita C. M. Rockosi N. Kizhuprakkat A. Riley J. Aguilar S. Ahlen D. Bianchi D. Brooks T. Claybaugh A. P. Cooper A. de la Macorra A. Dey P. Doel J. Forero-Romero E. Gaztañaga S. Gontcho A Gontcho G. Gutierrez M. Ishak R. Kehoe T. Kisner M. Landriau L. Le Guillou A. Meisner R. Miquel F. Prada I. Perez-Rafols G. Rossi E. Sanchez D. J. Schlegel J. H. Silber D. Sprayberry G. Tarle B. A. Weaver R. Zhou
This is my paper · ORCID
classification astro-ph.GAastro-ph.SR
keywords RRLyraevariablestarsInstabilitystripOosterhoffdichotomyStellarkinematicsMilkyWayhaloGlobularstarclustersDwarfgalaxiesSpectroscopy
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 uses 6,240 RR Lyrae stars from the first year of the DESI survey, with homogeneous spectroscopic iron abundances and pulsation-corrected effective temperatures, to ask how metal content shapes where and how these stars pulsate. Its central empirical result is that the RR Lyrae instability strip moves toward cooler effective temperatures as $[\mathrm{Fe/H}]$ declines, while its width stays roughly constant at about 1300–1400 K, consistent with stellar-evolution models. If this is right, it is the first large spectroscopic map of the range of temperatures over which RR Lyrae pulsation is possible as a function of metallicity, and it gives a quantitative explanation for the long-standing Oosterhoff dichotomy as a consequence of the scarcity of intermediate-metallicity globular clusters with sizable RR Lyrae populations.

What carries the argument

The load-bearing object is the DESI Year 1 RR Lyrae catalog of 6,240 stars, with one crucial refinement: the effective temperatures are phase-corrected, meaning each star's single-epoch spectrum is modeled against its pulsation cycle so the reported $T_{\rm eff}$ represents the mean over the cycle rather than a random phase. The instability strip edges are defined operationally as percentile limits of the temperature distributions of RRab stars (cooler, fundamental-mode) and RRc stars (hotter, first-overtone) in equal-number metallicity bins; linear fits to the running 16th/84th and 5th/95th percentiles give the empirical red and blue edges. The same catalog's RVS-derived $[\mathrm{Fe/H}]$ values and Gaia DR3 periods and subtype classifications carry the Bailey diagram, Petersen diagram, and metal-rich candidate analyses.

What would settle it

Measure $T_{\rm eff}$ for the same stars with a method independent of the spectral fitting, such as multiband photometric temperatures or asteroseismic constraints, and check whether the blue-edge slope of roughly $+83$ K per dex in $[\mathrm{Fe/H}]$ survives; if stars below $[\mathrm{Fe/H}]\approx-2.5$ are assigned temperatures that are systematically too cool, the strip shift disappears. A complete, selection-bias-free sample of low-metallicity RRc stars from deep wide-field photometry with follow-up spectra would also settle whether the blue edge truly moves to cooler temperatures.

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Extended reading notes

Core claim

The central claim is that the blue and red edges of the RR Lyrae instability strip shift toward cooler temperatures with declining $[\mathrm{Fe/H}]$, with the strip's width staying roughly constant. For the 2-$\sigma$ edges over $[\mathrm{Fe/H}]$ from roughly -2.8 to -1.2 dex, the paper reports $T_{\rm eff}^{\rm RE}=6020(\pm47)+40(\pm27)[\mathrm{Fe/H}]$ K and $T_{\rm eff}^{\rm BE}=7473(\pm37)+83(\pm20)[\mathrm{Fe/H}]$ K, so the blue edge moves about 83 K per dex while the red edge moves much less. Alongside this, the paper reports that high-amplitude short-period and small-amplitude short-period RR Lyrae stars are comparatively metal-rich, with mean $[\mathrm{Fe/H}]$ of $-1.39\pm0.27$ and $-1.30\pm0.28$; that double-mode RRd stars show metallicity declining smoothly with increasing fundamental-mode period; and that eight metal-rich candidates with $[\mathrm{Fe/H}]>-0.5$ dex split roughly evenly between disk-like and halo-like orbits.

Load-bearing premise

The load-bearing premise is that the DESI Year 1 RR Lyrae sample and its phase-corrected effective temperatures faithfully trace the true blue and red edges of the instability strip at every metallicity, with no metallicity-dependent bias in $T_{\rm eff}$ or in which stars were selected for spectroscopy.

Editorial extensions

If this is right

  • The smooth anti-correlation between logarithmic period and $[\mathrm{Fe/H}]$ for both RRab and RRc stars supports the view that the Oosterhoff dichotomy is not a fundamental bimodality of pulsation but follows from the lack of intermediate-metallicity globular clusters with large RR Lyrae samples.
  • High-amplitude short-period (HASP) and small-amplitude short-period (SASP) stars are metal-rich and sit on radial orbits associated with the Gaia-Sausage-Enceladus merger in large numbers, so they can serve as chemical tracers of massive accreted satellites that enriched early and were later disrupted.
  • The period-ratio versus $[\mathrm{Fe/H}]$ relation for classical RRd stars turns the Petersen diagram into a spectroscopic metallicity indicator and, combined with existing models, places classical RRd masses above about $0.69\,M_\odot$ and anomalous RRd masses in a narrow $0.68$--$0.77\,M_\odot$ range.
  • Empirical red and blue edges with roughly constant width can replace theoretical assumptions in stellar population models that predict RRc-to-RRab ratios across metallicity.
  • The eight metal-rich candidates with $[\mathrm{Fe/H}]>-0.5$ dex, about half on disk-like orbits, give concrete targets for testing whether some RR Lyrae stars form through binary mass-stripping channels rather than single-star evolution.

Reading between the lines

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

  • If the blue-edge shift is real, then period-luminosity-metallicity relations used to measure distances with RR Lyrae stars may need a metallicity-dependent temperature correction, because a cooler instability strip at low $[\mathrm{Fe/H}]$ changes the expected pulsation properties at fixed luminosity.
  • The trend can be checked with independent, model-free temperature estimates, such as multiband colors or temperatures from eclipsing binary companions; if stars with $[\mathrm{Fe/H}]<-2.5$ are not actually as cool as the spectroscopic fits say, the blue-edge slope would shrink or vanish.
  • The paper's own candidate explanations for the model discrepancy (small numbers near the edges at low metallicity, or decreasing accuracy in $[\mathrm{Fe/H}]$ and $T_{\rm eff}$ at the metal-poor end) suggest a targeted search for low-metallicity RRc stars in deep wide-field photometry could separate an intrinsic strip shift from a selection artifact.
  • If the Oosterhoff dichotomy is a selection effect, then globular cluster systems with continuous metallicity distributions should show continuous mean RRab periods rather than two clumps; applying the same DESI spectra to a larger cluster sample would test this directly.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper uses the DESI Year 1 RR Lyrae catalog from the companion paper M25 (6,240 RRLs with homogeneously derived RVS/SP spectroscopic parameters and phase-corrected effective temperatures) to study (1) correlations between [Fe/H] and pulsation period/amplitude in the Bailey diagram, including the Oosterhoff dichotomy; (2) the metallicities and kinematics of HASP and SASP variables; (3) the period-ratio--[Fe/H] relation of double-mode RRd stars; (4) the claimed empirical, metallicity-dependent topology of the RR Lyrae instability strip; and (5) a small sample of metal-rich RRL candidates. The central claim, stated in the abstract and in Section 5.1, is that the instability strip moves toward cooler Teff with declining [Fe/H] while its width remains roughly constant, based on percentile-based blue and red edges fit as linear functions of [Fe/H] in Eqs. (4)-(5).

Significance. If established, the instability-strip topology result would be a genuinely new empirical constraint, using a large sample and pulsation-phase-corrected effective temperatures, and would be of interest to both stellar pulsation and Galactic archaeology communities. The paper also provides useful confirmation of period--[Fe/H] trends and an RRd period-ratio relation in agreement with Braga et al. (2022). The data product (the DESI Y1 RRL catalog with described fitting procedures and planned public release) is itself a contribution. However, the headline topology claim currently rests on percentile statistics and on the assumption that the [Fe/H] and Teff scales do not have metallicity-dependent systematics; the paper's own text acknowledges this as a possible explanation, and the existing checks do not exclude it. The supporting claims (Oosterhoff interpretation, HASP/SASP properties, RRd relation) are more robust and independently useful.

major comments (3)
  1. [Section 5.1, Eqs. (4)-(5)] The central claim that the instability strip moves to cooler Teff with declining [Fe/H] is carried almost entirely by the blue edge. The reported red-edge slopes are 8 +/- 9 K/dex (1-sigma definition) and 40 +/- 27 K/dex (2-sigma definition), both consistent with zero at roughly the 1.5-sigma level. Consequently, Eqs. (4)-(5) do not show that the strip shifts as a whole. Moreover, the strip width implied by these fits is not constant: using the 1-sigma definitions, the BE - RE separation changes by roughly 96 K/dex (104 - 8), which is about 3.8 sigma from zero, while the 2-sigma separation changes by 43 +/- 34 K/dex, only marginally consistent with constant width. The abstract's statement 'an instability strip that moves towards cooler Teff with declining [Fe/H] with a width roughly consistent with stellar-evolution models' is therefore oversold relative to the fitted relations; the text should either qualify the claim as a blue-edge shift or provide a joint fit that explicitly tests and reports the width trend.
  2. [Section 5.1 and Figure 12] The blue edge is defined as the 84th or 95th percentile of the RRc Teff distribution, and the red edge as the 16th or 5th percentile of the RRab distribution. These are arbitrary statistical summaries of the observed Teff distributions, not physical boundaries derived from a pulsation model. Because DESI-MWS is not a complete or selection-function-corrected sample, a metallicity-dependent target-selection or phase-sampling effect that changes the occupancy of the hot tail of the RRc distribution would shift the derived blue edge without any change in the true instability strip. The paper does not quantify the selection function or test how the inferred slopes in Eqs. (4)-(5) respond to plausible incompleteness or to the choice of percentile definition (e.g., a fixed number of stars above a threshold, or a fit to the underlying distribution rather than percentiles). This is a load-bearing issue for the 'first empirical constraint' claim, because the entire metallicity shift is of order 100 K/dex over the fitted range, comparable to the width of the percentile tails being used.
  3. [Section 5.1 and Summary] The manuscript itself identifies 'systematic lost of precision and accuracy for [Fe/H] and/or Teff in the very metal-poor regime' as a potential explanation for the discrepancy with Marconi et al. (2015), whose models predict the opposite metallicity trend. The authors' check using non-phase-corrected RVS and SP temperatures rules out the phase-correction step as the sole cause, but it does not rule out a shared metallicity-dependent systematic in the RVSpecFit/PHOENIX Teff scale or a compression of the RVS [Fe/H] scale at low [Fe/H]. The fitted blue-edge slope of 83-104 K/dex over a range of about 1.6 dex corresponds to a total shift of roughly 130-170 K; a Teff zero-point drift of order 100-200 K across the metallicity range, or an equivalent [Fe/H] scale error, could produce the entire claimed trend. A concrete test would be to compare the M25 Teff against an independent photometric or spectroscopic temperature scale (e.g., period-color relations or high-resolution analyses of a calibration subset) and to repeat the edge fits using the SP and Delta-S [Fe/H] scales, showing that the slopes are stable. Without such a test, the central topology result remains vulnerable to the systematic uncertainty the authors themselves flag.
minor comments (5)
  1. [Abstract] The phrase 'Using a sample 6,240 RRLs' is missing 'of'; it should read 'Using a sample of 6,240 RRLs'.
  2. [Section 5.1] In the sentence 'Potential explanations for this shift include a systematic lost of precision and accuracy,' the word 'lost' should be 'loss'.
  3. [Section 6.1] In Figure 13's caption, 'S/N is < 3 at wavelengths < 5500 K' should refer to a wavelength in angstroms, not kelvin; likely '5500 A' is intended.
  4. [Section 6 and Table 2] The metal-rich candidate sample is very small (eight stars with good spectra, of which one is concordant across all three metallicity estimators and two are explicitly flagged as having poor RVS fits). The orbital classification into 'disk-like' versus 'halo-like' kinematics is therefore sensitive to individual measurement errors; the text should state more prominently that these are candidate-level findings and that no inference about the fraction of metal-rich RRLs from binary channels is made.
  5. [Figure 12] The figure would benefit from showing the actual data points or binned medians for RRab and RRc together with the percentile fits, rather than only the fitted lines and the Marconi et al. (2015) shaded regions; this would help the reader assess how much of the blue-edge trend is driven by a few high-TeFF stars in the sparsely populated most metal-poor bins.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the paper's correlations are descriptive fits to independent spectroscopic measurements, and the instability-strip comparison uses external theoretical models.

full rationale

The paper's central claims are empirical correlations fitted to DESI Y1 RRL data, with metallicities from RVSpecfit/PHOENIX and phase-corrected effective temperatures from the companion M25 catalog. No 'prediction' or 'constraint' is defined in terms of the fitted relations themselves. Equations (1)-(3) and (4)-(5) are linear fits to binned medians and percentiles; they are descriptive rather than self-fulfilling, and the comparison to Marconi et al. (2015) uses external theoretical predictions. The paper explicitly flags the alternative that 'a systematic lost of precision and accuracy for [Fe/H] and/or Teff in the very metal-poor regime' could explain the discrepancy with models, showing that the observed trend is not forced by construction. Reliance on M25 is a data-product self-citation, not a circular argument: the Teff and [Fe/H] measurements are independent empirical products, not outputs of the instability-strip model being constrained. External anchors such as Fabrizio et al. (2019, 2021), Braga et al. (2022), and Marconi et al. (2015) provide independent checks. No circular step is exhibited.

Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

The analysis uses empirical fits and external models. The main hand-set choices are the Teff outlier cuts and the percentile definitions for the instability strip edges. No new physical entities are introduced.

free parameters (2)
  • Teff outlier cuts = 4800 K and 8250 K
    Stars outside these effective temperature bounds are removed as outliers in Section 5, and the choice of bounds affects the percentile-derived instability strip edges.
  • Instability strip edge percentiles = 5th/95th and 16th/84th
    The red and blue edges are defined as fixed percentiles of the RRab and RRc Teff distributions; this choice sets the measured edge temperatures in Equations 4 and 5.
assumptions (4)
  • domain assumption Gaia DR3 RR Lyrae classification and periods are reliable.
    The sample uses Gaia DR3 classifications and periods directly, and the paper notes possible contamination among distant SASP stars with low best class scores.
  • domain assumption Phase-corrected Teff from M25 accurately represent mean systemic effective temperatures.
    The instability strip analysis in Section 5 relies entirely on these Teff estimates; systematic errors in the pulsation-phase correction would directly bias the derived edges.
  • domain assumption The DESI Y1 sample is representative of field RRL populations across metallicity.
    The percentile-based Teff distributions are assumed to trace the true instability strip boundaries; survey target selection or incompleteness that varies with metallicity would distort the edges.
  • domain assumption MWPotential2014 with an LMC perturber is an adequate model for orbital integration.
    Orbital parameters and disk versus halo classifications in Sections 3.2 and 6 use this potential model, including a mass scaling and dynamical friction treatment for the LMC.

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Cite this review

Pith. "Pith review of The DESI Y1 RR Lyrae catalog II: The metallicity dependency of pulsational properties, the shape of the RR Lyrae instability strip, and metal rich RR Lyrae." pith.science (2026). https://pith.science/paper/75BESMC4

@misc{pith2026250510614,
  author       = {Pith},
  title        = {Pith review of: The DESI Y1 RR Lyrae catalog II: The metallicity dependency of pulsational properties, the shape of the RR Lyrae instability strip, and metal rich RR Lyrae},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/75BESMC4}},
  note         = {Machine review of arXiv:2505.10614}
}
abstract

RR Lyrae stars (RRLs) are valuable probes of both Milky Way assembly and stellar-evolution physics. Using a sample 6,240 RRLs obtained in the first year of the Dark Energy Spectroscopic Instrument (DESI) survey, we investigate the metallicity of RRLs and its correlation with their pulsation properties. We find that (1) a clear correlation between period and [Fe/H] reinforces the view that the long-standing Oosterhoff dichotomy arises from the scarcity of intermediate-metallicity Galactic globular clusters hosting sizeable RRL samples; (2) high-amplitude short-period and small-amplitude short-period variables are comparatively metal-rich, with mean [Fe/H] = $-1.39 \pm 0.27$ and $-1.30 \pm 0.28$, respectively; (3) in double-mode pulsators (RRd) the metallicity declines smoothly with increasing fundamental-mode period, and anomalous RRd stars occupy a remarkably narrow [Fe/H] range relative to classical RRd stars; (4) this spectroscopic sample let us, for the first time, place empirical constraints on the metallicity-dependent topology of the instability strip using phase-corrected effective temperatures and a large number of RRLs, where we observe an instability strip that moves towards cooler $T_{\rm eff}$ with declining [Fe/H] with a width roughly consistent with stellar-evolution models; and (5) a subset of metal-rich RRLs exhibits orbits consistent with disk membership and halo kinematics. Our results confirm the tantalizing potential of DESI for Galactic and stellar astrophysics and highlight the importance of the even larger samples of RRLs and data-processing improvements forthcoming in future DESI data releases.

Figures

Figures reproduced from arXiv: 2505.10614 by the authors.

Figure 1
Figure 1. Bailey diagram of the DESI Y1 RRL sam￾ple (adapted from M25). The light curve amplitudes in the V −band (AV ) shown are computed using the peak-to-peak G−band magnitudes listed in the Gaia catalog and the trans￾formation equation from Clementini et al. (2019). The clas￾sification of RRLs between RRab, RRc, and RRd is taken directly from the Gaia DR3 catalog (Clementini et al. 2023). minosity amplitudes decreasing wi… view at source ↗
Figure 2
Figure 2. Same as [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Distribution of logP (left panels) and visual amplitude AV (right panels) of the DESI Y1 RRL sample as a function of iron abundance. To illustrate existing correlations, the data is split into eight metallicity bins containing the same number of stars. In each panel, a blue histogram is used to represent RRc stars, whereas the logP and AV distribution of RRab is shown in red (towards longer periods and higher amplit… view at source ↗
Figures from the paper (10 more)
Figure 4
Figure 4. Figure 4: Iron-abundance dependence of the logarithm of the period and visual amplitude for RRab (red) and RRc (blue). The data is split into [Fe/H] bins with equal number of stars, in the range [−2.60, −1.19] dex for RRab stars, and [−2.79, −1.19] dex for RRc stars. In each pan…
Figure 5
Figure 5. Figure 5: Bailey diagram of the DESI Y1 RRL sample separated by system. This distinction is made to better il￾lustrate the distribution of RRLs in the halo, the Sagittarius stream (Sgr), Draco, and the combined sample of globular cluster RRLs. We note that the HASP region is dom…
Figure 6
Figure 6. Figure 6: Normalized [Fe/H] (top) and Galactocentric dis￾tance (center) histograms of HASPs (red) and SASPs (blue) in the DESI Y1 RRL sample. The bottom panel displays the metallicity as a function of RGC for both RRL subsamples. with previous theoretical and empirical predictio…
Figure 7
Figure 7. Figure 7: Vertical angular momentum LZ and energy E of the stars in the DESI Y1 RRL sample, computed from the integration of their orbits using GALPY (Bovy 2015). Red, blue, and purple markers represent HASPs, SASPs, and RRLs with [Fe/H]> 0.5 dex, respectively, whereas stars tha…
Figure 9
Figure 9. Figure 9: Period ratio as a function of [Fe/H] for the DESI Y1 RRd stars, fit with a linear function. In addition to the curve obtained from the median of the linear model parameters’ posterior distributions, 100 curves drawn from the MCMC chains are shown to visualize the varia…
Figure 10
Figure 10. Figure 10: Top: Normalized distribution of (systemic) effective temperatures for the different RRL sub-types in our field sample, in Teff bins of 150 K. Vertical dashed lines depict the median of the for each sub-type. The 5th and 95th percentiles of the Teff of RRab and RRc var…
Figure 11
Figure 11. Figure 11: Same as [PITH_FULL_IMAGE:figures/full_fig_p014_11.png]
Figure 12
Figure 12. Figure 12: Similar to [PITH_FULL_IMAGE:figures/full_fig_p015_12.png]
Figure 13
Figure 13. Figure 13: Spectra of the eight RRLs in the DESI catalog that display [Fe/H] > −0.5 dex (from the RVS pipeline), which are described in Section 6. The observed spectra are depicted with thinner and more transparent lines, whereas the best-fitting RVSpec models are shown with thi…
Figure 14
Figure 14. Figure 14: Orbits of four of the metal-rich candidates discussed in Section 6, in Galactocentric Cartesian coordinates (X, Y , and Z) and Galactocentric radius (RGC), integrated for 0.65 Gyr. In each panel, a solid line is used to represent the stars’ orbits integrated backwards…

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Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. On the use of field RR Lyrae as Galactic probes:. IX. Radial velocities

    astro-ph.SR 2026-07 conditional novelty 5.0 of 10

    The largest homogeneous catalog of RR Lyrae radial velocities (17,563 stars), with template-based systemic velocities, amplitude scaling relations, and metallicity/Blazhko trends.

  2. The mass of the Milky Way from outer halo stars measured by DESI DR1

    astro-ph.GA 2025-08 conditional novelty 5.0 of 10

    DESI DR1 blue horizontal-branch and RR Lyrae stars give a Milky Way mass of about 0.57e12 Msun within 100 kpc and a virial mass of about 0.8e12 Msun.

Reference graph

Works this paper leans on

144 extracted references · 18 canonical work pages · cited by 2 Pith papers

  1. [1]

    2025, arXiv e-prints, arXiv:2503.01018, doi: 10.48550/arXiv.2503.01018

    Abdollahi, H., Moln´ ar, L., & Varga, V. 2025, arXiv e-prints, arXiv:2503.01018, doi: 10.48550/arXiv.2503.01018

    arXiv doi:10.48550/arxiv.2503.01018 2025

  2. [2]

    A., Alves, D., et al

    Alcock, C., Allsman, R. A., Alves, D., et al. 1999, ApJ, 511, 185, doi: 10.1086/306638 Allende Prieto, C., Beers, T. C., Wilhelm, R., et al. 2006, ApJ, 636, 804, doi: 10.1086/498131 Allende Prieto, C., Aguado, D. S., Gonz´ alez Hern´ andez, J. I., et al. 2023, ApJ, 957, 76, doi: 10.3847/1538-4357/acfa96 Astropy Collaboration, Robitaille, T. P., Tollerud, ...

    doi:10.1086/306638 1999

  3. [3]

    I., & Pickering, E

    Bailey, S. I., & Pickering, E. C. 1913, Annals of Harvard College Observatory, 78, 1

    1913

  4. [4]

    L., Bono, G., Braga, V

    Beaton, R. L., Bono, G., Braga, V. F., et al. 2018, SSRv, 214, 113, doi: 10.1007/s11214-018-0542-1

    doi:10.1007/s11214-018-0542-1 2018

  5. [5]

    2014, in The Third Hot-wiring the Transient Universe Workshop, ed

    Bellm, E. 2014, in The Third Hot-wiring the Transient Universe Workshop, ed. P. R. Wozniak, M. J. Graham, A. A. Mahabal, & R. Seaman, 27–33, doi: 10.48550/arXiv.1410.8185 24 Medina, Li, et al

    arXiv doi:10.48550/arxiv.1410.8185 2014

  6. [6]

    C., Kulkarni, S

    Bellm, E. C., Kulkarni, S. R., Graham, M. J., et al. 2019, PASP, 131, 018002, doi: 10.1088/1538-3873/aaecbe

    doi:10.1088/1538-3873/aaecbe 2019

  7. [7]

    J., Koposov, S

    Belokurov, V., Deason, A. J., Koposov, S. E., et al. 2018, MNRAS, 477, 1472, doi: 10.1093/mnras/sty615 Blaˇ zko, S. 1907, Astronomische Nachrichten, 175, 325, doi: 10.1002/asna.19071752002

    doi:10.1093/mnras/sty615 2018

  8. [8]

    2024, MNRAS, 527, 12196, doi: 10.1093/mnras/stad3996

    Bobrick, A., Iorio, G., Belokurov, V., et al. 2024, MNRAS, 527, 12196, doi: 10.1093/mnras/stad3996

    doi:10.1093/mnras/stad3996 2024

Show all 144 references
  1. [9]

    1997a, ApJ, 479, 279, doi: 10.1086/303872

    Marconi, M. 1997a, ApJ, 479, 279, doi: 10.1086/303872

    doi

  2. [10]

    1997b, ApJ, 483, 811, doi: 10.1086/304284

    Bono, G., Caputo, F., Cassisi, S., Incerpi, R., & Marconi, M. 1997b, ApJ, 483, 811, doi: 10.1086/304284

    doi

  3. [11]

    1996, ApJL, 471, L33, doi: 10.1086/310320

    Bono, G., Caputo, F., Castellani, V., & Marconi, M. 1996, ApJL, 471, L33, doi: 10.1086/310320

    1996 doi

  4. [12]

    1995a, ApJ, 442, 159, doi: 10.1086/175430 —

    Bono, G., Caputo, F., Castellani, V., et al. 1995a, ApJ, 442, 159, doi: 10.1086/175430 —. 2003, MNRAS, 344, 1097, doi: 10.1046/j.1365-8711.2003.06878.x

    2003

  5. [13]

    1995b, AJ, 110, 2365, doi: 10.1086/117694

    Bono, G., Caputo, F., & Marconi, M. 1995b, AJ, 110, 2365, doi: 10.1086/117694

    doi

  6. [14]

    Bono, G., Caputo, F., & Stellingwerf, R. F. 1994, ApJ, 423, 294, doi: 10.1086/173806

    1994 doi

  7. [15]

    Bono, G., & Stellingwerf, R. F. 1994, ApJS, 93, 233, doi: 10.1086/192054

    1994 doi

  8. [16]

    F., Crestani, J., et al

    Bono, G., Braga, V. F., Crestani, J., et al. 2020, ApJL, 896, L15, doi: 10.3847/2041-8213/ab9538

    2020 doi

  9. [17]

    2015, ApJS, 216, 29, doi: 10.1088/0067-0049/216/2/29

    Bovy, J. 2015, ApJS, 216, 29, doi: 10.1088/0067-0049/216/2/29

    2015 doi

  10. [18]

    F., Stetson, P

    Braga, V. F., Stetson, P. B., Bono, G., et al. 2016, AJ, 152, 170, doi: 10.3847/0004-6256/152/6/170

    2016 doi

  11. [19]

    F., Fiorentino, G., Bono, G., et al

    Braga, V. F., Fiorentino, G., Bono, G., et al. 2022, MNRAS, 517, 5368, doi: 10.1093/mnras/stac2813 Bystr¨ om, A., Koposov, S. E., Lilleengen, S., et al. 2024, arXiv e-prints, arXiv:2410.09149, doi: 10.48550/arXiv.2410.09149

    2022 doi arXiv

  12. [20]

    1989, A&A, 222, 121

    Caputo, F., Castellani, V., & Tornambe, A. 1989, A&A, 222, 121

    1989

  13. [21]

    1998, MNRAS, 293, 364, doi: 10.1046/j.1365-8711.1998.01171.x

    Caputo, F., Santolamazza, P., & Marconi, M. 1998, MNRAS, 293, 364, doi: 10.1046/j.1365-8711.1998.01171.x

    1998

  14. [22]

    2009, A&A, 508, 695, doi: 10.1051/0004-6361/200913003

    Lucatello, S. 2009, A&A, 508, 695, doi: 10.1051/0004-6361/200913003

    2009 doi

  15. [23]

    2004, A&A, 426, 641, doi: 10.1051/0004-6361:20041048

    Cassisi, S., Castellani, M., Caputo, F., & Castellani, V. 2004, A&A, 426, 641, doi: 10.1051/0004-6361:20041048

    2004 doi

  16. [24]

    2003, A&A, 410, 871, doi: 10.1051/0004-6361:20031381

    Castellani, M., Caputo, F., & Castellani, V. 2003, A&A, 410, 871, doi: 10.1051/0004-6361:20031381

    2003 doi

  17. [25]

    2009, Ap&SS, 320, 261, doi: 10.1007/s10509-009-9987-8

    Catelan, M. 2009, Ap&SS, 320, 261, doi: 10.1007/s10509-009-9987-8

    2009 doi

  18. [26]

    J., & Smith, H

    Catelan, M., Pritzl, B. J., & Smith, H. A. 2004, ApJS, 154, 633, doi: 10.1086/422916

    2004 doi

  19. [27]

    Catelan, M., & Smith, H. A. 2015, Pulsating Stars

    2015

  20. [28]

    2023, Nature Astronomy, 7, 1081, doi: 10.1038/s41550-023-02011-y

    Chen, X., Zhang, J., Wang, S., & Deng, L. 2023, Nature Astronomy, 7, 1081, doi: 10.1038/s41550-023-02011-y

    2023 doi

  21. [29]

    2019, A&A, 622, A60, doi: 10.1051/0004-6361/201833374

    Clementini, G., Ripepi, V., Molinaro, R., et al. 2019, A&A, 622, A60, doi: 10.1051/0004-6361/201833374

    2019 doi

  22. [30]

    2023, A&A, 674, A18, doi: 10.1051/0004-6361/202243964

    Clementini, G., Ripepi, V., Garofalo, A., et al. 2023, A&A, 674, A18, doi: 10.1051/0004-6361/202243964

    2023 doi

  23. [31]

    P., Koposov, S

    Cooper, A. P., Koposov, S. E., Allende Prieto, C., et al. 2023, ApJ, 947, 37, doi: 10.3847/1538-4357/acb3c0

    2023 doi

  24. [32]

    N., King, D

    Cox, A. N., King, D. S., & Hodson, S. W. 1980, ApJ, 236, 219, doi: 10.1086/157736

    1980 doi

  25. [33]

    F., et al

    Crestani, J., Fabrizio, M., Braga, V. F., et al. 2021a, ApJ, 908, 20, doi: 10.3847/1538-4357/abd183

    doi

  26. [34]

    F., Fabrizio, M., et al

    Crestani, J., Braga, V. F., Fabrizio, M., et al. 2021b, ApJ, 914, 10, doi: 10.3847/1538-4357/abfa23 Cruz Reyes, M., Anderson, R. I., Johansson, L., Netzel, H., & Medaric, Z. 2024, A&A, 684, A173, doi: 10.1051/0004-6361/202348961

    2024 doi

  27. [35]

    C., Garavito-Camargo, N., Deason, A

    Cunningham, E. C., Garavito-Camargo, N., Deason, A. J., et al. 2020, ApJ, 898, 4, doi: 10.3847/1538-4357/ab9b88 D’Cruz, N. L., Dorman, B., Rood, R. T., & O’Connell, R. W. 1996, ApJ, 466, 359, doi: 10.1086/177515 de Jong, R. S., Barden, S., Bellido-Tirado, O., et al. 2014, in S...

    2020 doi

  28. [36]

    Ramsay, I. S. McLean, & H. Takami, 91470M, doi: 10.1117/12.2055826 De Silva, G. M., Freeman, K. C., Bland-Hawthorn, J., et al. 2015, MNRAS, 449, 2604, doi: 10.1093/mnras/stv327 D´ ek´ any, I., Grebel, E. K., & Pojma´ nski, G. 2021, ApJ, 920, 33, doi: 10.3847/1538-4357/ac106f

    2015 doi

  29. [37]

    J., Liu, C., et al

    Deng, L.-C., Newberg, H. J., Liu, C., et al. 2012, Research in Astronomy and Astrophysics, 12, 735, doi: 10.1088/1674-4527/12/7/003 DESI Collaboration, Aghamousa, A., Aguilar, J., et al. 2016a, arXiv e-prints, arXiv:1611.00036, doi: 10.48550/arXiv.1611.00036 —. 2016b, arXiv e-...

    2012 doi arXiv

  30. [38]

    J., Djorgovski, S

    Drake, A. J., Djorgovski, S. G., Mahabal, A., et al. 2009, ApJ, 696, 870, doi: 10.1088/0004-637X/696/1/870

    2009 doi

  31. [39]

    J., Catelan, M., Djorgovski, S

    Drake, A. J., Catelan, M., Djorgovski, S. G., et al. 2013, ApJ, 763, 32, doi: 10.1088/0004-637X/763/1/32

    2013 doi

  32. [40]

    J., Djorgovski, S

    Drake, A. J., Djorgovski, S. G., Catelan, M., et al. 2017, MNRAS, 469, 3688, doi: 10.1093/mnras/stx1085

    2017 doi

  33. [41]

    S., Koposov, S

    Erkal, D., Li, T. S., Koposov, S. E., et al. 2018, MNRAS, 481, 3148, doi: 10.1093/mnras/sty2518

    2018 doi

  34. [42]

    F., et al

    Fabrizio, M., Bono, G., Braga, V. F., et al. 2019, ApJ, 882, 169, doi: 10.3847/1538-4357/ab3977

    2019 doi

  35. [43]

    F., Crestani, J., et al

    Fabrizio, M., Braga, V. F., Crestani, J., et al. 2021, ApJ, 919, 118, doi: 10.3847/1538-4357/ac1115

    2021 doi

  36. [44]

    2015, ApJL, 798, L12, doi: 10.1088/2041-8205/798/1/L12

    Fiorentino, G., Bono, G., Monelli, M., et al. 2015, ApJL, 798, L12, doi: 10.1088/2041-8205/798/1/L12

    2015 doi

  37. [45]

    B., et al

    Fiorentino, G., Monelli, M., Stetson, P. B., et al. 2017, A&A, 599, A125, doi: 10.1051/0004-6361/201629501

    2017 doi

  38. [46]

    F., et al

    Fiorentino, G., Bono, G., Braga, V. F., et al. 2022, in Memorie della Societa Astronomica Italiana, Vol. 93, 47, doi: 10.36116/MEMSAIT 93N4.2022.47

    2022 doi

  39. [47]

    2010, AJ, 140, 1694, doi: 10.1088/0004-6256/140/6/1694

    For, B.-Q., & Sneden, C. 2010, AJ, 140, 1694, doi: 10.1088/0004-6256/140/6/1694

    2010 doi

  40. [48]

    For, B.-Q., Sneden, C., & Preston, G. W. 2011, ApJS, 197, 29, doi: 10.1088/0067-0049/197/2/29

    2011 doi

  41. [49]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, PASP, 125, 306, doi: 10.1086/670067 Gaia Collaboration, Helmi, A., van Leeuwen, F., et al. 2018, A&A, 616, A12, doi: 10.1051/0004-6361/201832698

    2013 doi

  42. [50]

    E., Sarro, L

    Garofalo, A., Delgado, H. E., Sarro, L. M., et al. 2022, MNRAS, 513, 788, doi: 10.1093/mnras/stac735

    2022 doi

  43. [51]

    2013, A&A, 554, A46, doi: 10.1051/0004-6361/201220840

    Gillet, D. 2013, A&A, 554, A46, doi: 10.1051/0004-6361/201220840

    2013 doi

  44. [52]

    2019, A&A, 623, A109, doi: 10.1051/0004-6361/201833869 GRAVITY Collaboration, Abuter, R., Amorim, A., et al

    Gillet, D., Mauclaire, B., Lemoult, T., et al. 2019, A&A, 623, A109, doi: 10.1051/0004-6361/201833869 GRAVITY Collaboration, Abuter, R., Amorim, A., et al. 2021, A&A, 647, A59, doi: 10.1051/0004-6361/202040208

    2019 doi

  45. [53]

    2023, AJ, 165, 144, doi: 10.3847/1538-3881/acb212

    Guy, J., Bailey, S., Kremin, A., et al. 2023, AJ, 165, 144, doi: 10.3847/1538-3881/acb212

    2023 doi

  46. [54]

    2015, MNRAS, 449, L113, doi: 10.1093/mnrasl/slv024

    Hajdu, G., Catelan, M., Jurcsik, J., et al. 2015, MNRAS, 449, L113, doi: 10.1093/mnrasl/slv024

    2015 doi

  47. [55]

    2021, ApJ, 915, 50, doi: 10.3847/1538-4357/abff4b

    Hajdu, G., Pietrzy´ nski, G., Jurcsik, J., et al. 2021, ApJ, 915, 50, doi: 10.3847/1538-4357/abff4b

    2021 doi

  48. [56]

    J., Nordstr¨ om, B., Bonifacio, P., et al

    Hansen, C. J., Nordstr¨ om, B., Bonifacio, P., et al. 2011, A&A, 527, A65, doi: 10.1051/0004-6361/201015076

    2011 doi

  49. [57]

    1990, ApJ, 356, 359, doi: 10.1086/168845

    Hernquist, L. 1990, ApJ, 356, 359, doi: 10.1086/168845

    1990 doi

  50. [58]

    Hunter, J. D. 2007, Computing in Science and Engineering, 9, 90, doi: 10.1109/MCSE.2007.55

    2007 doi

  51. [59]

    O., Wende-von Berg, S., Dreizler, S., et al

    Husser, T. O., Wende-von Berg, S., Dreizler, S., et al. 2013, A&A, 553, A6, doi: 10.1051/0004-6361/201219058

    2013 doi

  52. [60]

    2023, The Messenger, 190, 10, doi: 10.18727/0722-6691/5301

    Ibata, R., Battaglia, G., Bellazzini, M., et al. 2023, The Messenger, 190, 10, doi: 10.18727/0722-6691/5301

    2023 doi

  53. [61]

    1971, ApJ, 166, 131, doi: 10.1086/150946

    Iben, Icko, J. 1971, ApJ, 166, 131, doi: 10.1086/150946

    1971 doi

  54. [62]

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

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

    2021 doi

  55. [63]

    Irwin, J. B. 1952, ApJ, 116, 211, doi: 10.1086/145604 —. 1959, AJ, 64, 149, doi: 10.1086/107913

    1952 doi

  56. [64]

    S., Stanek, K

    Jayasinghe, T., Kochanek, C. S., Stanek, K. Z., et al. 2018, MNRAS, 477, 3145, doi: 10.1093/mnras/sty838

    2018 doi

  57. [65]

    Z., Kochanek, C

    Jayasinghe, T., Stanek, K. Z., Kochanek, C. S., et al. 2020, MNRAS, 491, 13, doi: 10.1093/mnras/stz2711

    2020 doi

  58. [66]

    1996, A&A, 312, 111

    Jurcsik, J., & Kovacs, G. 1996, A&A, 312, 111

    1996

  59. [67]

    2015, ApJS, 219, 25, doi: 10.1088/0067-0049/219/2/25

    Jurcsik, J., Smitola, P., Hajdu, G., et al. 2015, ApJS, 219, 25, doi: 10.1088/0067-0049/219/2/25

    2015 doi

  60. [68]

    2017, MNRAS, 466, 2842, doi: 10.1093/mnras/stw3286

    Karczmarek, P., Wiktorowicz, G., I lkiewicz, K., et al. 2017, MNRAS, 466, 2842, doi: 10.1093/mnras/stw3286

    2017 doi

  61. [69]

    2019, A&A, 623, A116, doi: 10.1051/0004-6361/201834210

    Kervella, P., Gallenne, A., Remage Evans, N., et al. 2019, A&A, 623, A116, doi: 10.1051/0004-6361/201834210

    2019 doi

  62. [70]

    E., Li, T

    Kim, B., Koposov, S. E., Li, T. S., et al. 2025, arXiv e-prints, arXiv:2504.20327, doi: 10.48550/arXiv.2504.20327

    2025 doi arXiv

  63. [71]

    Koposov, S. E. 2019a, RVSpecFit: Radial velocity and stellar atmospheric parameter fitting, Astrophysics Source Code Library, record ascl:1907.013 —. 2019b, RVSpecFit: Radial velocity and stellar atmospheric parameter fitting. http://ascl.net/1907.013

    1907

  64. [72]

    E., Belokurov, V., Li, T

    Koposov, S. E., Belokurov, V., Li, T. S., et al. 2019, MNRAS, 485, 4726, doi: 10.1093/mnras/stz457

    2019 doi

  65. [73]

    E., Allende Prieto, C., Cooper, A

    Koposov, S. E., Allende Prieto, C., Cooper, A. P., et al. 2024, MNRAS, 533, 1012, doi: 10.1093/mnras/stae1842 Kov´ acs, G., & Walker, A. R. 1999, ApJ, 512, 271, doi: 10.1086/306755

    2024 doi

  66. [74]

    Kundu, R., Minniti, D., & Singh, H. P. 2019, MNRAS, 483, 1737, doi: 10.1093/mnras/sty3239

    2019 doi

  67. [75]

    Lee, J.-W., & Carney, B. W. 1999, AJ, 118, 1373, doi: 10.1086/301008

    1999 doi

  68. [76]

    2013, arXiv e-prints, arXiv:1308.0847, doi: 10.48550/arXiv.1308.0847

    Levi, M., Bebek, C., Beers, T., et al. 2013, arXiv e-prints, arXiv:1308.0847, doi: 10.48550/arXiv.1308.0847

    2013 doi arXiv

  69. [77]

    J., Qian, S

    Li, L. J., Qian, S. B., Zhu, L. Y., Shi, X. D., & Liao, W. P. 2024, arXiv e-prints, arXiv:2404.00911, doi: 10.48550/arXiv.2404.00911

    2024 doi arXiv

  70. [78]

    2013, Research in Astronomy and Astrophysics, 13, 1307, doi: 10.1088/1674-4527/13/11/003 Liˇ ska, J., Skarka, M., Zejda, M., Mikul´ aˇ sek, Z., & de

    Liu, S., Zhao, G., Chen, Y.-Q., Takeda, Y., & Honda, S. 2013, Research in Astronomy and Astrophysics, 13, 1307, doi: 10.1088/1674-4527/13/11/003 Liˇ ska, J., Skarka, M., Zejda, M., Mikul´ aˇ sek, Z., & de

    2013 doi

  71. [79]

    Villiers, S. N. 2016, MNRAS, 459, 4360, doi: 10.1093/mnras/stw851 26 Medina, Li, et al

    2016 doi

  72. [80]

    2021, in Astronomical Society of the Pacific Conference Series, Vol

    Luo, C., Liu, C., Zhang, X., et al. 2021, in Astronomical Society of the Pacific Conference Series, Vol. 529, RR Lyrae/Cepheid 2019: Frontiers of Classical Pulsators, ed. K. Kinemuchi, C. Lovekin, H. Neilson, & K. Vivas, 147

    2021

  73. [81]

    2024, arXiv e-prints, arXiv:2409.04259, doi: 10.48550/arXiv.2409.04259

    Luongo, E., Ripepi, V., Marconi, M., et al. 2024, arXiv e-prints, arXiv:2409.04259, doi: 10.48550/arXiv.2409.04259

    2024 doi arXiv

  74. [82]

    R., Schiavon, R

    Majewski, S. R., Schiavon, R. P., Frinchaboy, P. M., et al. 2017, AJ, 154, 94, doi: 10.3847/1538-3881/aa784d

    2017 doi

  75. [83]

    J., G¨ ansicke, B

    Manser, C. J., G¨ ansicke, B. T., Inight, K., et al. 2023, MNRAS, 521, 4976, doi: 10.1093/mnras/stad727

    2023 doi

  76. [84]

    J., Izquierdo, P., G¨ ansicke, B

    Manser, C. J., Izquierdo, P., G¨ ansicke, B. T., et al. 2024, MNRAS, doi: 10.1093/mnras/stae2205

    2024 doi

  77. [85]

    2015, ApJ, 808, 50, doi: 10.1088/0004-637X/808/1/50

    Marconi, M., Coppola, G., Bono, G., et al. 2015, ApJ, 808, 50, doi: 10.1088/0004-637X/808/1/50

    2015 doi

  78. [86]

    2022, ApJ, 934, 29, doi: 10.3847/1538-4357/ac78ee

    Marconi, M., Molinaro, R., Dall’Ora, M., et al. 2022, ApJ, 934, 29, doi: 10.3847/1538-4357/ac78ee

    2022 doi

  79. [87]

    A., Gozha, M

    Marsakov, V. A., Gozha, M. L., & Koval’, V. V. 2019, Astronomy Reports, 63, 203, doi: 10.1134/S1063772919020069 Mart´ ınez-V´ azquez, C. E., Vivas, A. K., Gurevich, M., et al. 2019, MNRAS, 490, 2183, doi: 10.1093/mnras/stz2609

    2019 doi

  80. [88]

    E., Hansen, C

    Medina, G. E., Hansen, C. J., Mu˜ noz, R. R., et al. 2023, MNRAS, 519, 5689, doi: 10.1093/mnras/stac3800

    2023 doi

  81. [89]

    E., Mu˜ noz, R

    Medina, G. E., Mu˜ noz, R. R., Carlin, J. L., et al. 2024, arXiv e-prints, arXiv:2402.14055, doi: 10.48550/arXiv.2402.14055

    2024 doi arXiv

  82. [90]

    E., Mu˜ noz, R

    Medina, G. E., Mu˜ noz, R. R., Vivas, A. K., et al. 2017, ApJL, 845, L10, doi: 10.3847/2041-8213/aa821e —. 2018, ApJ, 855, 43, doi: 10.3847/1538-4357/aaad02

    2017 doi

  83. [91]

    E., Li, T

    Medina, G. E., Li, T. S., Koposov, S. E., et al. 2025, arXiv e-prints, arXiv:2504.02924, doi: 10.48550/arXiv.2504.02924

    2025 doi arXiv

  84. [92]

    N., Doel, P., Gutierrez, G., et al

    Miller, T. N., Doel, P., Gutierrez, G., et al. 2024, AJ, 168, 95, doi: 10.3847/1538-3881/ad45fe

    2024 doi

  85. [93]

    1975, PASJ, 27, 533

    Miyamoto, M., & Nagai, R. 1975, PASJ, 27, 533

    1975

  86. [94]

    2022, Universe, 8, 191, doi: 10.3390/universe8030191

    Monelli, M., & Fiorentino, G. 2022, Universe, 8, 191, doi: 10.3390/universe8030191

    2022 doi

  87. [95]

    P., Marengo, M., Mart´ ınez-V´ azquez, C

    Mullen, J. P., Marengo, M., Mart´ ınez-V´ azquez, C. E., et al. 2021, ApJ, 912, 144, doi: 10.3847/1538-4357/abefd4 —. 2022, ApJ, 931, 131, doi: 10.3847/1538-4357/ac67ee

    2021 doi

  88. [96]

    2015, ApJ, 807, 127, doi: 10.1088/0004-637X/807/2/127

    Muraveva, T., Palmer, M., Clementini, G., et al. 2015, ApJ, 807, 127, doi: 10.1088/0004-637X/807/2/127

    2015 doi

  89. [97]

    P., Conroy, C., Bonaca, A., et al

    Naidu, R. P., Conroy, C., Bonaca, A., et al. 2020, ApJ, 901, 48, doi: 10.3847/1538-4357/abaef4

    2020 doi

  90. [98]

    2024, A&A, 689, A138, doi: 10.1051/0004-6361/202450364

    Narloch, W., Hajdu, G., Pietrzy´ nski, G., et al. 2024, A&A, 689, A138, doi: 10.1051/0004-6361/202450364

    2024 doi

  91. [99]

    2015, A&A, 577, A99, doi: 10.1051/0004-6361/201424838

    Navarrete, C., Contreras Ramos, R., Catelan, M., et al. 2015, A&A, 577, A99, doi: 10.1051/0004-6361/201424838

    2015 doi

  92. [100]

    F., Frenk, C

    Navarro, J. F., Frenk, C. S., & White, S. D. M. 1997, ApJ, 490, 493, doi: 10.1086/304888

    1997 doi

  93. [101]

    R., Marengo, M., Bono, G., et al

    Neeley, J. R., Marengo, M., Bono, G., et al. 2017, ApJ, 841, 84, doi: 10.3847/1538-4357/aa713d

    2017 doi

  94. [102]

    Nemec, J. M. 1985, AJ, 90, 240, doi: 10.1086/113728

    1985 doi

  95. [103]

    M., Cohen, J

    Nemec, J. M., Cohen, J. G., Ripepi, V., et al. 2013, ApJ, 773, 181, doi: 10.1088/0004-637X/773/2/181

    2013 doi

  96. [104]

    M., Linnell Nemec, A

    Nemec, J. M., Linnell Nemec, A. F., Moskalik, P., et al. 2024, MNRAS, 529, 296, doi: 10.1093/mnras/stae424

    2024 doi

  97. [105]

    2022, Video Memorie della Societa Astronomica Italiana, 2, 22, doi: 10.36116/VIDEOMEM 2.2022.22

    Netzel, H. 2022, Video Memorie della Societa Astronomica Italiana, 2, 22, doi: 10.36116/VIDEOMEM 2.2022.22

    2022 doi

  98. [106]

    Oosterhoff, P. T. 1939, The Observatory, 62, 104

    1939

  99. [107]

    2011, ApJS, 192, 3, doi: 10.1088/0067-0049/192/1/3

    Paxton, B., Bildsten, L., Dotter, A., et al. 2011, ApJS, 192, 3, doi: 10.1088/0067-0049/192/1/3

    2011 doi

  100. [108]

    2019, ApJS, 243, 10, doi: 10.3847/1538-4365/ab2241

    Paxton, B., Smolec, R., Schwab, J., et al. 2019, ApJS, 243, 10, doi: 10.3847/1538-4365/ab2241

    2019 doi

  101. [109]

    Petersen, J. O. 1973, A&A, 27, 89 Pietrzy´ nski, G., Graczyk, D., Gallenne, A., et al. 2019, Nature, 567, 200, doi: 10.1038/s41586-019-0999-4

    1973 doi

  102. [110]

    L., Dziembowski, W

    Popielski, B. L., Dziembowski, W. A., & Cassisi, S. 2000, AcA, 50, 491, doi: 10.48550/arXiv.astro-ph/0011442

    2000 doi arXiv

  103. [111]

    2024, AJ, 168, 245, doi: 10.3847/1538-3881/ad76a4

    Poppett, C., Tyas, L., Aguilar, J., et al. 2024, AJ, 168, 245, doi: 10.3847/1538-3881/ad76a4

    2024 doi

  104. [112]

    Preston, G. W. 1959, ApJ, 130, 507, doi: 10.1086/146743

    1959 doi

  105. [113]

    W., Sneden, C., Thompson, I

    Preston, G. W., Sneden, C., Thompson, I. B., Shectman, S. A., & Burley, G. S. 2006, AJ, 132, 85, doi: 10.1086/504425

    2006 doi

  106. [114]

    K., & Kunder, A

    Prudil, Z., D´ ek´ any, I., Grebel, E. K., & Kunder, A. 2020, MNRAS, 492, 3408, doi: 10.1093/mnras/staa046

    2020 doi

  107. [115]

    Prudil, Z., & Ferro, A. A. 2024, MNRAS, doi: 10.1093/mnras/stae2335

    2024 doi

  108. [116]

    Prudil, Z., Kunder, A., D´ ek´ any, I., & Koch-Hansen, A. J. 2024, A&A, 684, A176, doi: 10.1051/0004-6361/202347338

    2024 doi

  109. [117]

    K., & Lee, C

    Prudil, Z., Skarka, M., Liˇ ska, J., Grebel, E. K., & Lee, C. U. 2019, MNRAS, 487, L1, doi: 10.1093/mnrasl/slz069

    2019 doi

  110. [118]

    1993, AJ, 106, 703, doi: 10.1086/116676

    Sandage, A. 1993, AJ, 106, 703, doi: 10.1086/116676

    1993 doi

  111. [119]

    2020, A&A, 641, A96, doi: 10.1051/0004-6361/202038305

    Savino, A., Koch, A., Prudil, Z., Kunder, A., & Smolec, R. 2020, A&A, 641, A96, doi: 10.1051/0004-6361/202038305

    2020 doi

  112. [120]

    1956, Annales d’Astrophysique, 19, 51

    Schatzman, E. 1956, Annales d’Astrophysique, 19, 51

    1956

  113. [121]

    F., Kirkby, D., Schlegel, D

    Schlafly, E. F., Kirkby, D., Schlegel, D. J., et al. 2023, AJ, 166, 259, doi: 10.3847/1538-3881/ad0832

    2023 doi

  114. [122]

    2017, AJ, 153, 204, doi: 10.3847/1538-3881/aa661b

    Sesar, B., Hernitschek, N., Mitrovi´ c, S., et al. 2017, AJ, 153, 204, doi: 10.3847/1538-3881/aa661b

    2017 doi

  115. [123]

    2021, arXiv e-prints, arXiv:2107.13004

    Shipp, N., Erkal, D., Drlica-Wagner, A., et al. 2021, arXiv e-prints, arXiv:2107.13004. https://arxiv.org/abs/2107.13004

    2021 arXiv

  116. [124]

    2005, AcA, 55, 59, doi: 10.48550/arXiv.astro-ph/0503614 The metallicity of DESI Y1 RR Lyrae 27

    Smolec, R. 2005, AcA, 55, 59, doi: 10.48550/arXiv.astro-ph/0503614 The metallicity of DESI Y1 RR Lyrae 27

    2005 doi arXiv

  117. [125]

    2013, MNRAS, 428, 3034, doi: 10.1093/mnras/sts258

    Smolec, R., Pietrzy´ nski, G., Graczyk, D., et al. 2013, MNRAS, 428, 3034, doi: 10.1093/mnras/sts258

    2013 doi

  118. [126]

    2015, MNRAS, 447, 3756, doi: 10.1093/mnras/stu2684

    Smolec, R., Soszy´ nski, I., Udalski, A., et al. 2015, MNRAS, 447, 3756, doi: 10.1093/mnras/stu2684

    2015 doi

  119. [127]

    W., Chadid, M., & Adam´ ow, M

    Sneden, C., Preston, G. W., Chadid, M., & Adam´ ow, M. 2017, ApJ, 848, 68, doi: 10.3847/1538-4357/aa8b10 Soszy´ nski, I., Dziembowski, W. A., Udalski, A., et al. 2011, AcA, 61, 1, doi: 10.48550/arXiv.1105.6126 Soszy´ nski, I., Udalski, A., Szyma´ nski, M. K., et al. 2014, AcA,...

    2017 doi arXiv

  120. [128]

    2005, in Astronomical Society of the Pacific Conference Series, Vol

    Sterken, C. 2005, in Astronomical Society of the Pacific Conference Series, Vol. 335, The Light-Time Effect in Astrophysics: Causes and cures of the O-C diagram, ed. C. Sterken, 3

    2005

  121. [129]

    M., Drlica-Wagner, A., Macri, L., et al

    Stringer, K. M., Drlica-Wagner, A., Macri, L., et al. 2021, ApJ, 911, 109, doi: 10.3847/1538-4357/abe873

    2021 doi

  122. [130]

    S., Chiba, M., et al

    Takada, M., Ellis, R. S., Chiba, M., et al. 2014, PASJ, 66, R1, doi: 10.1093/pasj/pst019

    2014 doi

  123. [131]

    2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Tamura, N., Takato, N., Shimono, A., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Ground-based and Airborne Instrumentation for Astronomy VI, ed. C. J

    2016

  124. [132]

    Simard, & H

    Evans, L. Simard, & H. Takami, 99081M, doi: 10.1117/12.2232103

    doi

  125. [133]

    J., et al

    Torrealba, G., Catelan, M., Drake, A. J., et al. 2015, MNRAS, 446, 2251, doi: 10.1093/mnras/stu2274

    2015 doi

  126. [134]

    E., et al

    Torrealba, G., Belokurov, V., Koposov, S. E., et al. 2019, MNRAS, 488, 2743, doi: 10.1093/mnras/stz1624 van Albada, T. S., & Baker, N. 1971, ApJ, 169, 311, doi: 10.1086/151144 —. 1973, ApJ, 185, 477, doi: 10.1086/152434 van der Marel, R. P., Alves, D. R., Hardy, E., & Suntzeff...

    2019 doi

  127. [135]

    2024, AJ, 168, 43, doi: 10.3847/1538-3881/ad5180

    Varma, V., & Ngeow, C.-C. 2024, AJ, 168, 43, doi: 10.3847/1538-3881/ad5180

    2024 doi

  128. [136]

    2021, MNRAS, 501, 2279, doi: 10.1093/mnras/staa3673

    Vasiliev, E., Belokurov, V., & Erkal, D. 2021, MNRAS, 501, 2279, doi: 10.1093/mnras/staa3673

    2021 doi

  129. [137]

    E., et al

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

    2020 doi

  130. [138]

    K., Mart´ ınez-V´ azquez, C., & Walker, A

    Vivas, A. K., Mart´ ınez-V´ azquez, C., & Walker, A. R. 2020, ApJS, 247, 35, doi: 10.3847/1538-4365/ab67c0

    2020 doi

  131. [139]

    2000, A&AS, 143, 9, doi: 10.1051/aas:2000332

    Wenger, M., Ochsenbein, F., Egret, D., et al. 2000, A&AS, 143, 9, doi: 10.1051/aas:2000332

    2000 doi

  132. [140]

    1982, ChA&A, 6, 43, doi: 10.1016/0275-1062(82)90063-7

    Xiong, D.-r. 1982, ChA&A, 6, 43, doi: 10.1016/0275-1062(82)90063-7

    1982 doi

  133. [141]

    2025, arXiv e-prints, arXiv:2504.06720, doi: 10.48550/arXiv.2504.06720

    Zhang, H., Iorio, G., Belokurov, V., et al. 2025, arXiv e-prints, arXiv:2504.06720, doi: 10.48550/arXiv.2504.06720

    2025 doi

  134. [142]

    2023, MNRAS, 525, 5915, doi: 10.1093/mnras/stad2681

    Zhang, S., Liu, G., Huang, Y., et al. 2023, MNRAS, 525, 5915, doi: 10.1093/mnras/stad2681

    2023 doi

  135. [143]

    C., & Casetti-Dinescu, D

    Zinn, R., Chen, X., Layden, A. C., & Casetti-Dinescu, D. I. 2020, MNRAS, 492, 2161, doi: 10.1093/mnras/stz3580

    2020 doi

  136. [144]

    K., et al

    Zinn, R., Horowitz, B., Vivas, A. K., et al. 2014, ApJ, 781, 22, doi: 10.1088/0004-637X/781/1/22

    2014 doi

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