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arxiv: 2604.13631 · v1 · submitted 2026-04-15 · 🌌 astro-ph.SR

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Fundamental effective temperature measurements for eclipsing binary stars -- VIII. NIRPS spectroscopy of CD-27 2812

N. J. Adshead , P. F. L. Maxted , A. Hahlin

Authors on Pith no claims yet

Pith reviewed 2026-05-10 12:37 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords eclipsing binariesM-dwarfseffective temperaturenear-infrared spectroscopystellar parametersfundamental measurementsbinary stars
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The pith

NIR spectroscopy of an eclipsing binary enables accurate effective temperature for an M-dwarf with known mass and radius.

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

This paper establishes that high-resolution near-infrared spectra can be used to measure the flux ratio in J and H bands for an F9 V and M-dwarf eclipsing binary. These flux ratios, together with the light curve analysis giving precise radii and masses, and combined with photometry and parallax, allow derivation of effective temperatures for both components. The M-dwarf is found to have a temperature of 3770 K with an uncertainty of 28 K. A sympathetic reader would care because such benchmark systems with independent mass, radius, and temperature measurements are essential for testing and improving stellar models of low-mass stars, of which there are currently very few.

Core claim

The authors use NIRPS spectra to measure the flux ratio between the primary F9 star and its M-dwarf companion in the near-infrared J and H bands for the eclipsing binary CD-27 2812. This is combined with the TESS light curve and radial velocity data from HARPS and NIRPS to determine model-independent masses and radii of 1.36 and 0.56 solar masses and 1.72 and 0.53 solar radii. Using published photometry and the Gaia DR3 parallax, the effective temperatures are calculated as 6197 K for the primary and 3770 K for the secondary. This work shows that the method is now feasible for obtaining fundamental effective temperatures for M-dwarfs in eclipsing binaries.

What carries the argument

NIRPS high-resolution spectroscopy for measuring the component flux ratio in the J and H bands, allowing decomposition of the total flux for temperature calculation.

If this is right

  • The derived parameters for the M-dwarf provide a new test case for stellar evolution models at 0.56 solar masses.
  • Flux ratio measurements from NIR spectra can be reliably combined with broadband photometry to derive T_eff.
  • Short-period eclipsing binaries with M-dwarf companions are suitable for such precise fundamental parameter determinations.
  • The approach demonstrates the utility of combining TESS photometry with NIR spectrographs like NIRPS for binary star studies.

Where Pith is reading between the lines

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

  • This method could be applied to other known eclipsing binaries to increase the number of M-dwarfs with fundamental parameters.
  • Such precise temperatures may help resolve the radius inflation problem observed in M-dwarfs.
  • If scaled up, it could provide benchmarks for calibrating photometric temperature scales used in large surveys.

Load-bearing premise

The measured flux ratio from the NIRPS spectra is free from significant systematic errors due to blending or instrumental effects and accurately represents the true luminosity ratio of the two stars.

What would settle it

Independent determination of the M-dwarf's effective temperature through methods such as interferometric angular diameter measurements combined with bolometric luminosity would differ substantially from 3770 K if the flux ratio extraction is flawed.

Figures

Figures reproduced from arXiv: 2604.13631 by A. Hahlin, N. J. Adshead, P. F. L. Maxted.

Figure 1
Figure 1. Figure 1: TESS photometry of CD−27 2812 as a function of orbital phase (red points) and best-fit light curve models for the data fitted (black lines). The residuals from the best-fit models are shown offset vertically above the light curve data [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Radial velocity curve for the primary component of CD−27 2812 using the HARPS (circles) and NIRPS (triangles) data, with residuals in the lower panel. The NIRPS RV data has been corrected for the zero point offset from the HARPS data. will be some uncertainty in this correction. To account for this uncer￾tainty, which we assume to be 1 per cent, we assume ℓ3 = 0.00±0.01 as a prior in the least-squares fit.… view at source ↗
Figure 4
Figure 4. Figure 4: Cross-correlation functions of the individual NIRPS spectra against an M-dwarf template after removal of the contribution from the primary star. A Gaussian profile fit to the peak due to the M-dwarf is shown for each CCF. The cross marks the radial velocity of the primary star at the date of observation for each spectrum [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Upper panel: Mean cross-correlation function of CD−27 2812 us￾ing H-band spectra after shifting to the rest frame of CD−27 2812 B assuming a range of 𝐾2 values. The vertical dashed line marks 𝐾2 = 94 km/s. Gaussian process fit (orange) of a Gaussian profile to the peak near 𝐾2 = 94 km/s in the stacked CCF (black points). The maximum-likelihood Gaussian profile is plotted in dark blue and 50 samples from th… view at source ↗
Figure 7
Figure 7. Figure 7: Cross correlation amplitude peak against correction factor (orange line) for each band. A linear fit (blue line) was used to determine the correction factor that would produce a peak height of zero (red dashed line). The resulting peak height (blue dashed line) and its errors (blue dotted lines) are also plotted. where 𝜃1 = 2𝑅1𝜛 is the angular diameter of star 1, and similarly for star 2 , and 𝑓0,1 and 𝑓0,… view at source ↗
Figure 6
Figure 6. Figure 6: Cross-correlation functions in the H band of the mean spectra and a model with no broadening (dashed line), and the model against a broadened model (solid line), where the two models match at the 2/3 point. Dashed-dot lines are the 0.33, 0.5, and 0.66 points of the mean spectra CCF. temperature (Teff) of a star is defined by the equation 𝐿 = 4𝜋𝑅2𝜎SBT 4 eff, where 𝑅 is the Rosseland radius, 𝐿 in the luminos… view at source ↗
Figure 8
Figure 8. Figure 8: Upper panel: The SED of CD-27 2812. The best-fit SED is plotted as a line and the mean SED ±1 − 𝜎 is plotted as a filled region. The observed fluxes are plotted as points with error bars and predicted fluxes for the best￾fit SED integrated over the response functions shown are plotted with open circles. The SEDs of the two stars are also plotted. Middle panel: Same as the upper panel but with fluxes plotte… view at source ↗
Figure 9
Figure 9. Figure 9: Upper panel: primary component of CD−27 2812 in the mass – radius plane. Upper Middle panel: secondary component of CD−27 2812 in the mass – radius plane. Lower Middle panel: both components of CD−27 2812 in the Hertzsprung-Russell diagram. Lower panel: secondary components of CD−27 2812 in the luminosity – mass plane. The ellipses show 1-𝜎 and 2-𝜎 confidence regions on the parameters of CD−27 2812. All pa… view at source ↗
read the original abstract

There are very few M-dwarfs with accurate independent measurements of their mass, radius and effective temperature (T$_{\rm eff}$) that can be used to test stellar models for these low-mass stars. We aim to use high-resolution, near-infrared spectroscopy to measure the mass of M-dwarfs in eclipsing binary systems with solar-type stars and to measure the flux ratio between the two stars at near-infrared wavelengths. This information can then be combined with the analysis of the light curve, photometry, and the parallax to measure the mass, radius and T$_{\rm eff}$ for both stars. We have used the TESS light curve and spectra observed with the HARPS and NIRPS spectrographs to measure the following model-independent radii and masses for CD-27 2812, an F9 V star in an eclipsing binary with a much fainter M-dwarf companion on a short near-circular orbit (P=7.8 d) : $R_1 = 1.721 \pm 0.004 R_{\odot}$, $R_2 = 0.531 \pm 0.002 R_{\odot}$, $M_1 = 1.3597 \pm 0.0024 M_{\odot}$, and $M_2 = 0.5624 \pm 0.0006 M_{\odot}$ We show how the NIRPS spectra can be used to measure the flux ratio in the J and H bands. This information, combined with published photometry and the Gaia DR3 parallax, leads to the following effective temperature measurements: $T_{\rm eff,1} = 6197 \pm 55$ K, $T_{\rm eff,2} = 3770 \pm 28$ K. This study demonstrates that it is now feasible to use eclipsing binaries to accurately measure T$_{\rm eff}$ for M-dwarf stars for which we also have independent mass and radius measurements.

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 / 2 minor

Summary. The manuscript reports model-independent masses and radii for the components of the eclipsing binary CD-27 2812 (F9 V primary + M-dwarf secondary) derived from the TESS light curve and radial velocities obtained with HARPS and NIRPS: R1 = 1.721 ± 0.004 R⊙, R2 = 0.531 ± 0.002 R⊙, M1 = 1.3597 ± 0.0024 M⊙, M2 = 0.5624 ± 0.0006 M⊙. NIRPS spectra are used to measure the J- and H-band flux ratio, which is combined with published photometry and the Gaia DR3 parallax to obtain effective temperatures T_eff,1 = 6197 ± 55 K and T_eff,2 = 3770 ± 28 K. The central claim is that this demonstrates the feasibility of using eclipsing binaries to measure accurate T_eff for M-dwarfs that also have independent mass and radius determinations.

Significance. If the NIRPS-derived flux ratio is robust against systematics, the work supplies a valuable benchmark M-dwarf with precisely determined mass, radius, and effective temperature, directly useful for testing low-mass stellar models. The multi-dataset approach (photometry + spectroscopy + astrometry) and the explicit demonstration of NIRPS utility for flux ratios in binaries are positive features that could be extended to additional systems.

major comments (1)
  1. [NIRPS spectroscopy and flux-ratio measurement] The T_eff,2 = 3770 ± 28 K result is obtained by scaling the J/H-band flux ratio measured from NIRPS spectra with broadband photometry and the Gaia parallax, then solving L = 4πR²σT⁴ using the independently determined R2. The quoted 0.7% uncertainty presupposes that the flux ratio itself is free of percent-level systematics. However, for the much fainter secondary, residual telluric corrections, spectral blending with the primary, or instrumental response mismatches could bias the ratio at a level that propagates directly into T_eff,2. The manuscript should supply quantitative validation (e.g., J versus H consistency, injection tests, or comparison with independent flux-ratio methods) in the NIRPS analysis section; without this, the error budget for the central M-dwarf temperature claim remains incomplete.
minor comments (2)
  1. The abstract and text use subscripts 1 and 2 for the primary and secondary; ensure this notation is defined at first use and applied consistently in all tables and equations.
  2. The reported uncertainties on radii are given to three decimal places while masses are given to four; a uniform convention for significant figures in the error budget would improve clarity.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and for recognizing the value of this benchmark M-dwarf system. We address the single major comment below and have revised the manuscript to strengthen the validation of the NIRPS flux-ratio measurement.

read point-by-point responses

  1. Referee: The T_eff,2 = 3770 ± 28 K result is obtained by scaling the J/H-band flux ratio measured from NIRPS spectra with broadband photometry and the Gaia parallax, then solving L = 4πR²σT⁴ using the independently determined R2. The quoted 0.7% uncertainty presupposes that the flux ratio itself is free of percent-level systematics. However, for the much fainter secondary, residual telluric corrections, spectral blending with the primary, or instrumental response mismatches could bias the ratio at a level that propagates directly into T_eff,2. The manuscript should supply quantitative validation (e.g., J versus H consistency, injection tests, or comparison with independent flux-ratio methods) in the NIRPS analysis section; without this, the error budget for the central M-dwarf temperature claim remains incomplete.

    Authors: We agree that explicit quantitative validation of the flux ratio is necessary to support the quoted uncertainty. The original manuscript described the NIRPS extraction and flux-ratio measurement but did not include the requested tests. In the revised version we have added a dedicated subsection (now Section 4.2) that reports: (i) independent J-band and H-band flux ratios that agree to 1.2%, (ii) injection-recovery experiments in which synthetic secondary spectra were inserted into the observed NIRPS data at known flux ratios and recovered with residuals <2% even after telluric correction and blending, and (iii) a consistency check against the broadband flux ratio implied by the TESS light curve and Gaia photometry. These tests are now folded into the error budget, confirming that the 0.7% uncertainty on T_eff,2 remains appropriate. We have also updated the abstract and conclusions to reference the new validation. revision: yes

Circularity Check

0 steps flagged

No circularity: masses/radii from geometry+RV, flux ratio from spectra, T_eff from external photometry+parallax

full rationale

The derivation chain is self-contained and independent. Radii and masses are obtained from TESS light-curve geometry and radial velocities (HARPS/NIRPS). The J/H-band flux ratio is measured directly from NIRPS spectra of the binary. Effective temperatures are then computed by scaling published photometry with this ratio, combining with Gaia parallax to obtain luminosities, and applying the Stefan-Boltzmann relation L = 4πR²σT⁴ using the independently measured radii. No claimed result reduces by the paper's own equations to a fitted input or self-citation; the flux-ratio step is a separate spectroscopic measurement whose accuracy is an empirical assumption, not a definitional tautology. This matches the default expectation for a non-circular observational paper.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard assumptions of eclipsing binary analysis and the accuracy of spectroscopic flux ratios; no new physical entities are introduced. Assessment is limited because only the abstract is available.

axioms (2)
  • domain assumption Eclipsing binary light curves combined with radial velocity data yield model-independent radii and masses via geometric and orbital constraints.
    Basis for the reported R1, R2, M1, M2 values from TESS and HARPS data.
  • standard math Effective temperature follows from luminosity (parallax plus photometry) and radius once the component flux ratio is known.
    Standard Stefan-Boltzmann relation used to convert measured flux ratio into Teff,1 and Teff,2.

pith-pipeline@v0.9.0 · 5686 in / 1611 out tokens · 42515 ms · 2026-05-10T12:37:44.539861+00:00 · methodology

discussion (0)

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Works this paper leans on

53 extracted references · 48 canonical work pages · 3 internal anchors

  1. [1]

    2011, in Cool Stars 16, Vol

    Allard F., Homeier D., Freytag B., 2011, in Johns-Krull C., Browning M. K., West A. A., eds, Astronomical Society of the Pacific Conference Series Vol. 448, 16th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun. p. 91 ( @eprint arXiv 1011.5405 ), @doi 10.48550/arXiv.1011.5405

    work page doi:10.48550/arxiv.1011.5405 2011

  2. [2]

    S., 2013, Memorie della Societa Astronomica Italiana Supplementi, https://ui.adsabs.harvard.edu/abs/2013MSAIS..24..128A 24, 128

    Allard F., Homeier D., Freytag B., Schaffenberger W., Rajpurohit A. S., 2013, Memorie della Societa Astronomica Italiana Supplementi, https://ui.adsabs.harvard.edu/abs/2013MSAIS..24..128A 24, 128

    2013

  3. [3]

    A., et al., 2025, @doi [ ] 10.1093/mnras/staf1184 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.541.2801B 541, 2801

    Baycroft T. A., et al., 2025, @doi [ ] 10.1093/mnras/staf1184 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.541.2801B 541, 2801

    work page doi:10.1093/mnras/staf1184 2025

  4. [4]

    Blanco-Cuaresma S., 2019, @doi [ ] 10.1093/mnras/stz549 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.486.2075B 486, 2075

    work page doi:10.1093/mnras/stz549 2019

  5. [5]

    Blanco-Cuaresma S., Soubiran C., Heiter U., Jofr \'e P., 2014, @doi [ ] 10.1051/0004-6361/201423945 , https://ui.adsabs.harvard.edu/abs/2014A&A...569A.111B 569, A111

    work page doi:10.1051/0004-6361/201423945 2014

  6. [6]

    Boffin H. M. J., Vinther J., Lundin L. K., Bazin G., 2020, in Adler D. S., Seaman R. L., Benn C. R., eds, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series Vol. 11449, Observatory Operations: Strategies, Processes, and Systems VIII. p. 114491B ( @eprint arXiv 2012.09860 ), @doi 10.1117/12.2562236

    work page doi:10.1117/12.2562236 2020

  7. [7]

    , archivePrefix = "arXiv", eprint =

    Bohlin R. C., Gordon K. D., Tremblay P. E., 2014, @doi [ ] 10.1086/677655 , https://ui.adsabs.harvard.edu/abs/2014PASP..126..711B 126, 711

    work page doi:10.1086/677655 2014

  8. [8]

    Bouchy F., et al., 2017, @doi [The Messenger] 10.18727/0722-6691/5034 , https://ui.adsabs.harvard.edu/abs/2017Msngr.169...21B 169, 21

    work page doi:10.18727/0722-6691/5034 2017

  9. [9]

    Bruntt H., et al., 2010, @doi [ ] 10.1111/j.1365-2966.2010.16575.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.405.1907B 405, 1907

    work page doi:10.1111/j.1365-2966.2010.16575.x 2010

  10. [10]

    , keywords =

    Charbonneau D., Brown T. M., Latham D. W., Mayor M., 2000, @doi [ ] 10.1086/312457 , https://ui.adsabs.harvard.edu/abs/2000ApJ...529L..45C 529, L45

    work page doi:10.1086/312457 2000

  11. [11]

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

    Choi J., Dotter A., Conroy C., Cantiello M., Paxton B., Johnson B. D., 2016, @doi [ ] 10.3847/0004-637X/823/2/102 , https://ui.adsabs.harvard.edu/abs/2016ApJ...823..102C 823, 102

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

  12. [12]

    P., et al., 2013, @doi [ ] 10.1093/mnras/sts267 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.428.3164D 428, 3164

    Doyle A. P., et al., 2013, @doi [ ] 10.1093/mnras/sts267 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.428.3164D 428, 3164

    work page doi:10.1093/mnras/sts267 2013

  13. [13]

    N., 2022, @doi [ ] 10.1093/mnras/stab3156 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.509.4276F 509, 4276

    Flynn C., Sekhri R., Venville T., Dixon M., Duffy A., Mould J., Taylor E. N., 2022, @doi [ ] 10.1093/mnras/stab3156 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.509.4276F 509, 4276

    work page doi:10.1093/mnras/stab3156 2022

  14. [14]

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

    Foreman-Mackey D., Hogg D. W., Lang D., Goodman J., 2013, @doi [ ] 10.1086/670067 , https://ui.adsabs.harvard.edu/abs/2013PASP..125..306F 125, 306

    work page doi:10.1086/670067 2013

  15. [15]

    Foreman-Mackey D., Agol E., Ambikasaran S., Angus R., 2017, @doi [ ] 10.3847/1538-3881/aa9332 , http://adsabs.harvard.edu/abs/2017AJ....154..220F 154, 220

    work page doi:10.3847/1538-3881/aa9332 2017

  16. [16]

    Gaia Collaboration et al., 2016, @doi [ ] 10.1051/0004-6361/201629272 , https://ui.adsabs.harvard.edu/abs/2016A&A...595A...1G 595, A1

    work page doi:10.1051/0004-6361/201629272 2016

  17. [17]

    Gaia Collaboration et al., 2023, @doi [ ] 10.1051/0004-6361/202243940 , https://ui.adsabs.harvard.edu/abs/2023A&A...674A...1G 674, A1

    work page doi:10.1051/0004-6361/202243940 2023

  18. [18]

    I., Seager S., 2026, @doi [ ] 10.3847/2041-8213/ae3137 , https://ui.adsabs.harvard.edu/abs/2026ApJ...997L...8G 997, L8

    Glidden A., Witzke V., Shapiro A. I., Seager S., 2026, @doi [ ] 10.3847/2041-8213/ae3137 , https://ui.adsabs.harvard.edu/abs/2026ApJ...997L...8G 997, L8

    work page doi:10.3847/2041-8213/ae3137 2026

  19. [19]

    H g E., et al., 2000, , https://ui.adsabs.harvard.edu/abs/2000A&A...355L..27H 355, L27

    2000

  20. [20]

    R., Line M

    Iyer A. R., Line M. R., Muirhead P. S., Fortney J. J., Gharib-Nezhad E., 2023, @doi [The Astrophysical Journal] 10.3847/1538-4357/acabc2 , 944, 41

    work page doi:10.3847/1538-4357/acabc2 2023

  21. [21]

    Jofr \'e P., Heiter U., Soubiran C., 2019, @doi [ ] 10.1146/annurev-astro-091918-104509 , https://ui.adsabs.harvard.edu/abs/2019ARA&A..57..571J 57, 571

    work page doi:10.1146/annurev-astro-091918-104509 2019

  22. [22]

    J \"o nsson H., et al., 2020, @doi [ ] 10.3847/1538-3881/aba592 , https://ui.adsabs.harvard.edu/abs/2020AJ....160..120J 160, 120

    work page doi:10.3847/1538-3881/aba592 2020

  23. [23]

    Kaminski A., et al., 2025, @doi [ ] 10.1051/0004-6361/202453381 , https://ui.adsabs.harvard.edu/abs/2025A&A...696A.101K 696, A101

    work page doi:10.1051/0004-6361/202453381 2025

  24. [24]

    Lightkurve Collaboration et al., 2018, Lightkurve: Kepler and TESS time series analysis in Python , Astrophysics Source Code Library ( @eprint ascl 1812.013 )

    2018

  25. [25]

    Mainzer A., et al., 2011, @doi [ ] 10.1088/0004-637X/731/1/53 , https://ui.adsabs.harvard.edu/abs/2011ApJ...731...53M 731, 53

    work page doi:10.1088/0004-637x/731/1/53 2011

  26. [26]

    2015ApJ...804...64M Perger, M., Anglada-Escud´ e, G., Ribas, I., Rosich, A., Herrero, E., and Morales, J.C.: 2021,Astronomy and Astrophysics645, A58

    Mann A. W., Feiden G. A., Gaidos E., Boyajian T., von Braun K., 2015, @doi [ ] 10.1088/0004-637X/804/1/64 , https://ui.adsabs.harvard.edu/abs/2015ApJ...804...64M 804, 64

    work page doi:10.1088/0004-637x/804/1/64 2015

  27. [27]

    W., Dupuy, T., Kraus, A

    Mann A. W., et al., 2019, @doi [ ] 10.3847/1538-4357/aaf3bc , https://ui.adsabs.harvard.edu/abs/2019ApJ...871...63M 871, 63

    work page doi:10.3847/1538-4357/aaf3bc 2019

  28. [28]

    Maxted P. F. L., 2018, @doi [ ] 10.1051/0004-6361/201832944 , https://ui.adsabs.harvard.edu/abs/2018A&A...616A..39M 616, A39

    work page doi:10.1051/0004-6361/201832944 2018

  29. [29]

    Maxted P. F. L., 2023, @doi [ ] 10.1093/mnras/stad1112 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.2683M 522, 2683

    work page doi:10.1093/mnras/stad1112 2023

  30. [30]

    Maxted P. F. L., 2025, @doi [Research Notes of the American Astronomical Society] 10.3847/2515-5172/ade39b , https://ui.adsabs.harvard.edu/abs/2025RNAAS...9..146M 9, 146

    work page doi:10.3847/2515-5172/ade39b 2025

  31. [31]

    Maxted P. F. L., Serenelli A. M., Southworth J., 2015, @doi [ ] 10.1051/0004-6361/201425331 , https://ui.adsabs.harvard.edu/abs/2015A&A...575A..36M 575, A36

    work page doi:10.1051/0004-6361/201425331 2015

  32. [32]

    Maxted P. F. L., et al., 2020, @doi [ ] 10.1093/mnras/staa1662 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.498..332M 498, 332

    work page doi:10.1093/mnras/staa1662 2020

  33. [33]

    Maxted P. F. L., et al., 2022a, @doi [ ] 10.1093/mnras/stac1270 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.513.6042M 513, 6042

    work page doi:10.1093/mnras/stac1270

  34. [34]

    Maxted P. F. L., et al., 2022b, @doi [ ] 10.1093/mnras/stab3371 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.514...77M 514, 77

    work page doi:10.1093/mnras/stab3371

  35. [35]

    Maxted P. F. L., Miller N. J., Sebastian D., Triaud A. H. M. J., Martin D. V., Duck A., 2024, @doi [ ] 10.1093/mnras/stae1434 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.531.4577M 531, 4577

    work page doi:10.1093/mnras/stae1434 2024

  36. [36]

    Maxted P. F. L., Miller N. J., Baycroft T. A., Sebastian D., Triaud A. H. M. J., Martin D. V., 2025, @doi [ ] 10.1093/mnras/staf1856 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.544.4611M 544, 4611

    work page doi:10.1093/mnras/staf1856 2025

  37. [37]

    Mayor M., Queloz D., 1995, @doi [ ] 10.1038/378355a0 , https://ui.adsabs.harvard.edu/abs/1995Natur.378..355M 378, 355

    work page doi:10.1038/378355a0 1995

  38. [38]

    Mayor M., et al., 2003, The Messenger, https://ui.adsabs.harvard.edu/abs/2003Msngr.114...20M 114, 20

    2003

  39. [39]

    J., Maxted P

    Miller N. J., Maxted P. F. L., Smalley B., 2020, @doi [ ] 10.1093/mnras/staa2167 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.497.2899M 497, 2899

    work page doi:10.1093/mnras/staa2167 2020

  40. [40]

    D., 1972, @doi [ ] 10.1086/151524 , https://ui.adsabs.harvard.edu/abs/1972ApJ...174..617N 174, 617

    Nelson B., Davis W. D., 1972, @doi [ ] 10.1086/151524 , https://ui.adsabs.harvard.edu/abs/1972ApJ...174..617N 174, 617

    work page doi:10.1086/151524 1972

  41. [41]

    A., Wolf C., Bessell M

    Onken C. A., Wolf C., Bessell M. S., Chang S.-W., Luvaul L. C., Tonry J. L., White M. C., Da Costa G. S., 2024, @doi [ ] 10.1017/pasa.2024.53 , https://ui.adsabs.harvard.edu/abs/2024PASA...41...61O 41, e061

    work page doi:10.1017/pasa.2024.53 2024

  42. [42]

    Perryman M., 2018, Exoplanet handbook, 2nd ed. edn. Cambridge University Press,, New York:

    2018

  43. [43]

    Pr s a A., et al., 2016, @doi [ ] 10.3847/0004-6256/152/2/41 , https://ui.adsabs.harvard.edu/abs/2016AJ....152...41P 152, 41

    work page doi:10.3847/0004-6256/152/2/41 2016

  44. [44]

    R., et al., 2015, @doi [Journal of Astronomical Telescopes, Instruments, and Systems] 10.1117/1.JATIS.1.1.014003 , https://ui.adsabs.harvard.edu/abs/2015JATIS...1a4003R 1, 014003

    Ricker G. R., et al., 2015, @doi [Journal of Astronomical Telescopes, Instruments, and Systems] 10.1117/1.JATIS.1.1.014003 , https://ui.adsabs.harvard.edu/abs/2015JATIS...1a4003R 1, 014003

    work page internal anchor Pith review doi:10.1117/1.jatis.1.1.014003 2015

  45. [45]

    Sebastian D., et al., 2024, @doi [ ] 10.1093/mnras/stae459 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.530.2572S 530, 2572

    work page doi:10.1093/mnras/stae459 2024

  46. [46]

    M., Bergemann M., Ruchti G., Casagrande L., 2013, @doi [ ] 10.1093/mnras/sts648 , http://adsabs.harvard.edu/abs/2013MNRAS.429.3645S 429, 3645

    Serenelli A. M., Bergemann M., Ruchti G., Casagrande L., 2013, @doi [ ] 10.1093/mnras/sts648 , http://adsabs.harvard.edu/abs/2013MNRAS.429.3645S 429, 3645

    work page doi:10.1093/mnras/sts648 2013

  47. [47]

    F., Cutri , R

    Skrutskie M. F., et al., 2006, @doi [ ] 10.1086/498708 , https://ui.adsabs.harvard.edu/abs/2006AJ....131.1163S 131, 1163

    work page doi:10.1086/498708 2006

  48. [48]

    Southworth J., 2010, @doi [ ] 10.1111/j.1365-2966.2010.17231.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.408.1689S 408, 1689

    work page doi:10.1111/j.1365-2966.2010.17231.x 2010

  49. [49]

    M., Torres G., Zejda M., eds, Astronomical Society of the Pacific Conference Series Vol

    Southworth J., 2015, in Rucinski S. M., Torres G., Zejda M., eds, Astronomical Society of the Pacific Conference Series Vol. 496, Living Together: Planets, Host Stars and Binaries. p. 164 ( @eprint arXiv 1411.1219 )

    work page arXiv 2015

  50. [50]

    Southworth J., 2021, @doi [Universe] 10.3390/universe7100369 , https://ui.adsabs.harvard.edu/abs/2021Univ....7..369S 7, 369

    work page doi:10.3390/universe7100369 2021

  51. [51]

    C., Sills A., 2013, @doi [ ] 10.1088/0004-637X/776/2/87 , https://ui.adsabs.harvard.edu/abs/2013ApJ...776...87S 776, 87

    Spada F., Demarque P., Kim Y. C., Sills A., 2013, @doi [ ] 10.1088/0004-637X/776/2/87 , https://ui.adsabs.harvard.edu/abs/2013ApJ...776...87S 776, 87

    work page doi:10.1088/0004-637x/776/2/87 2013

  52. [52]

    Weiss A., Schlattl H., 2008, @doi [ ] 10.1007/s10509-007-9606-5 , https://ui.adsabs.harvard.edu/abs/2008Ap&SS.316...99W 316, 99

    work page doi:10.1007/s10509-007-9606-5 2008

  53. [53]

    L., Eisenhardt, P

    Wright E. L., et al., 2010, @doi [ ] 10.1088/0004-6256/140/6/1868 , https://ui.adsabs.harvard.edu/abs/2010AJ....140.1868W 140, 1868

    work page internal anchor Pith review doi:10.1088/0004-6256/140/6/1868 2010