pith. sign in

arxiv: 2606.06234 · v1 · pith:76ZFVXRDnew · submitted 2026-06-04 · 🌌 astro-ph.SR · astro-ph.EP· astro-ph.IM

gr8stars II : judgement day for spectroscopic parameter model systematics

Alix Violet Freckelton , Annelies Mortier , Megan Bedell , Michael Cretignier , Jared R. Kolecki , Andreas J. Korn , S\'ergio G. Sousa , Maria Tsantaki
show 13 more authors
John M. Brewer Lars A. Buchhave Guy R. Davies J. I. Gonz\'alez Hern\'andez Sam Morrell Martin B. Nielsen Vera Maria Passegger Andreas Quirrenbach Arpita Roy Nuno C. Santos A. Su\'arez Mascare\~no Christopher Allan Watson Lily L. Zhao
This is my paper

Pith reviewed 2026-06-27 23:29 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EPastro-ph.IM
keywords stellar parametersspectroscopic methodsexoplanet propertiesFGK dwarfsisochrone fittingsystematicsSOPHIE spectra
0
0 comments X

The pith

Scatter across five spectroscopic methods on 585 FGK stars induces at most 3% fractional uncertainty in exoplanet radii and 5% in masses.

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

The paper applies five different spectroscopic pipelines to the same high-quality spectra of 585 bright FGK dwarfs to measure effective temperature, surface gravity, and metallicity. It then feeds each set of results into isochrone fitting to obtain stellar masses, radii, and ages, and compares the resulting radii against independent values from spectral energy distribution fitting. The observed method-to-method scatter is propagated forward to show the impact on derived exoplanet parameters. A sympathetic reader would care because the exercise quantifies a previously under-reported noise floor that affects many exoplanet studies. The work concludes that the induced errors on planetary radius and mass remain smaller than values commonly quoted in the literature.

Core claim

Five spectroscopic methods yield typical scatters of 76 K in effective temperature, 0.14 dex in surface gravity, and 0.07 dex in metallicity; when propagated through isochrone fitting, these produce fractional uncertainties of ≲3% in planetary radius and ≲5% in planetary mass, with a lower limit of ≈4% on planetary equilibrium temperature uncertainty.

What carries the argument

The scatter among five spectroscopic parameter sets, propagated through isochrone-derived stellar masses and radii to exoplanet properties and compared against SED radii.

If this is right

  • Planetary radius uncertainties arising from spectroscopic method choice stay at or below 3 percent.
  • Planetary mass uncertainties arising from spectroscopic method choice stay at or below 5 percent.
  • Planetary equilibrium temperature carries a minimum fractional uncertainty of approximately 4 percent from this source alone.
  • These limits lie below the uncertainties typically reported for exoplanet parameters in the literature.

Where Pith is reading between the lines

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

  • Other error sources such as orbital fitting or photometric calibration may now dominate the error budget in many exoplanet radius and mass determinations.
  • A combined analysis that averages or selects among multiple spectroscopic methods could reduce the effective scatter below the single-method values reported here.
  • The 4 percent floor on equilibrium temperature uncertainty would propagate directly into retrievals of planetary atmospheric properties and into assessments of potential habitability.

Load-bearing premise

The radii obtained by SED fitting in the companion paper form an independent benchmark free of shared systematics with the spectroscopic and isochrone results.

What would settle it

A measurement showing that the SED radii and isochronal radii share common systematics larger than the reported method-to-method scatter would remove the basis for claiming the induced planetary uncertainties are truly below literature values.

Figures

Figures reproduced from arXiv: 2606.06234 by Alix Violet Freckelton, Andreas J. Korn, Andreas Quirrenbach, Annelies Mortier, Arpita Roy, A. Su\'arez Mascare\~no, Christopher Allan Watson, Guy R. Davies, Jared R. Kolecki, J. I. Gonz\'alez Hern\'andez, John M. Brewer, Lars A. Buchhave, Lily L. Zhao, Maria Tsantaki, Martin B. Nielsen, Megan Bedell, Michael Cretignier, Nuno C. Santos, Sam Morrell, S\'ergio G. Sousa, Vera Maria Passegger.

Figure 1
Figure 1. Figure 1: Histograms of the differences between results from each method and PASTEL for 𝑇eff, [Fe/H], and log 𝑔. The standard deviation (STD) and mean of these histograms is marked on each plot, with a grey dashed line representing 0 in each plot. Parameter RMSD Median Difference Median Uncertainty P A+M F Y MP P A+M F Y MP P A+M F Y MP Δ 𝑇eff (K) 94 94 90 89 101 -8 34 51 -14 -27 105 30 26 70 93 Δ [Fe/H] 0.08 0.10 0… view at source ↗
Figure 2
Figure 2. Figure 2: The mean value from all spectral analysis codes in this work plotted against the PASTEL value for 𝑇eff (left), log 𝑔 (centre), and [Fe/H] (right). The pink line in all panels represents the one-to-one relationship. Lower panels show the residuals between the data sets. Y axes errors represent the standard deviation in the results from this work [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Differences in 𝑇eff from this work and those from PASTEL, coloured by the [Fe/H] from each method on the top row, and the PASTEL [Fe/H] on the second row. The top row additionally includes linear regression lines fitted to the data, as well as the Pearson Correlaton Coefficient (PCC) for the five sets of results. MNRAS 000, 1–19 (2025) [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Histograms of the whole-sample masses obtained using isochrones, with 𝑇eff and [Fe/H] from PAWS, ARES+MOOG, FASMA, YARARA, Metal Pipe, and the combined results. Grey dashed lines indicate the median of each distribution of results [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of stellar ages across the sample from this work. Stellar ages were determined using isochrones, with results from inputting spectroscopic 𝑇eff and [Fe/H] from PAWS, ARES+MOOG, FASMA, YARARA, Metal Pipe, and the combined results. Grey dashed lines display the median age from each distribution of results. MNRAS 000, 1–19 (2025) [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: The difference between spectroscopic and fundamental (interfero￾metric) 𝑇eff for each method applied in this work, for each of the 6 stars in common with Soubiran et al. (2024). sults here are therefore within the broad expectations of comparing spectroscopic to interferometric 𝑇eff. An additional observation from [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: First row : difference between the 𝑇eff derived by each method and the 𝑇eff from SED fitting, plotted against SED 𝑇eff. The Pearson Correlation Coefficient (PCC) and regression lines are additionally included. Second row : Histograms of the differences between spectroscopic and SED 𝑇eff, with standard deviation (STD) and median values displayed [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Difference between the log 𝑔 derived by each spectroscopic method and that from webSME, plotted against the webSME log 𝑔. This covers the 30 stars with the most discrepant log 𝑔 from the different spectroscopic methods. isochrones, and hence log 𝑔, are significantly model dependent and may not agree with empirical measurements (e.g. Boyajian et al. 2015). We additionally investigate whether the use of the … view at source ↗
Figure 9
Figure 9. Figure 9: Box-and-whisker plot of the log 𝑔 values determined by each code for the sample of 30 discrepant log 𝑔 targets, in addition to the log 𝑔 for these produced by only the equivalent widths section of PAWS. Open circles represent log 𝑔 values that extend beyond the minimum or maximum extremes of the data. 5.4 Microturbulent Velocity 𝑣mic An important consideration in our analysis is the influence of spectro￾sc… view at source ↗
Figure 10
Figure 10. Figure 10: Reduced chisquared of each forward-modelled spectrum when compared to the observed one, using the results from each method. This covers all 30 discrepant log 𝑔 targets. From the NASA Exoplanet Archive (Christiansen et al. 2025), the median fractional uncertainty on exoplanetary radius in the literature is 7.36%, higher than uncertainty predicted to arise from scatter in stellar radius alone. It is importa… view at source ↗
Figure 11
Figure 11. Figure 11: Histograms of the differences between the isochronal log 𝑔 for each method and the PASTEL log 𝑔, with standard deviation (STD) and median shown for each distribution [PITH_FULL_IMAGE:figures/full_fig_p015_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Left panel : Difference between the log 𝑔 from the full PAWS pipeline and from the combined isochronal posteriors, plotted against PAWS 𝑇eff. Right panel : Difference between the log 𝑔 from the EW section of PAWS and the combined isochronal posteriors, plotted against the PAWS 𝑇eff. Both panels additionally show the Pearson Correlation Coefficient (PCC) of the data, in addition to the fitted linear regres… view at source ↗
Figure 13
Figure 13. Figure 13: Histograms of the determined microturblent velocity (𝑣mic) from PAWS, FASMA, and ARES+MOOG. Each histogram also notes the standard deviation (STD) and median (Med.) values from each code [PITH_FULL_IMAGE:figures/full_fig_p016_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: The relationship between 𝑣mic and 𝑇eff for ARES+MOOG (left), PAWS (centre), and FASMA (right). The slope (m) and intercept (c) of the fitted linear regression lines are shown in the legend of each subplot. ity, we show that the precision errors often quoted for spectroscopic parameters are far outweighed by the scatter that comes from the use of different methods. Given that we consistently see disagreeme… view at source ↗
Figure 15
Figure 15. Figure 15: Differences in radii from each spectroscopic method + isochrones, and the radii from SED fitting, plotted against SED radius for each method. The lower right hand panel shows the results from combining all isochrones results. Four SED outliers have been removed from all of these plots. The Pearson Correlation Coefficient (PCC) and linear regression lines fitted to the data are shown in each panel. look pa… view at source ↗
read the original abstract

Many areas of astrophysics, including exoplanetary studies, rely on precise and accurate stellar parameters. This demands that uncertainties on these parameters truly reflect all biases and systematics. Within this second work of the \texttt{gr8stars} collaboration, we take a set of 585 bright FGK dwarfs with high resolution, high signal-to-noise ratio spectra from the SOPHIE spectrograph. We determine stellar effective temperature, surface gravity, and metallicity using five different spectroscopic methods for each star, with an additional method used for comparisons. We find a typical scatter of 76 K in \teff, 0.14 dex in \logg, and 0.07 dex in \feh. These deviations are significantly larger than the average precision error on these parameters. We furthermore use isochrone fitting to determine mass, radius, and age for all 585 stars, using input from all results. We use the radii determined by SED fitting in the first \texttt{gr8stars} paper as a comparison to our isochronal radii from this work, in addition to comparing the isochronal \logg to spectroscopic \logg. The scatter in mass and radius from the use of different spectroscopic methods is investigated and propagated to exoplanetary parameters. The induced fractional uncertainties in planetary radius ($\lesssim$ 3 \%) and mass ($\lesssim$ 5\%) are found to be below those typically found in the literature. We estimate a lower limit on planetary equilibrium temperature fractional uncertainty of $\approx$ 4\%, a noise floor that is currently not sufficiently represented in the literature.

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 paper analyzes spectroscopic parameters (Teff, log g, [Fe/H]) for 585 bright FGK dwarfs from SOPHIE spectra using five methods, reporting typical scatters of 76 K, 0.14 dex, and 0.07 dex. It performs isochrone fitting for masses, radii, and ages using these inputs, compares the resulting radii to SED-fitting radii from the companion gr8stars I paper (and isochronal vs. spectroscopic log g), and propagates the method-to-method scatter to estimate induced fractional uncertainties on exoplanet radius (≲3%), mass (≲5%), and a lower limit of ≈4% on equilibrium temperature.

Significance. If the benchmark comparison is independent, the work provides a concrete quantification of how spectroscopic method choice propagates to stellar and planetary parameters in a large, homogeneous sample. The finding that these systematics are smaller than typical literature values could help establish realistic uncertainty floors for exoplanet studies; the multi-method approach on 585 stars is a clear strength.

major comments (1)
  1. [the isochrone fitting and gr8stars I comparison section] The section describing the comparison of isochronal radii to SED-fitting radii from gr8stars I (and the propagation of scatters to planetary parameters): the central claim that the observed scatters (76 K, 0.14 dex, 0.07 dex) induce the quoted ≲3%/≲5%/≈4% fractional uncertainties on planetary radius/mass/Teq rests on treating the SED radii as an independent benchmark. The manuscript provides no quantitative test (e.g., overlap in photometry, model grids, or calibration steps) that the two pipelines are free of shared systematics; without this, the benchmark cannot independently confirm that the spectroscopic scatter is the dominant, well-quantified systematic.
minor comments (2)
  1. [Abstract] The abstract states that 'an additional method [is] used for comparisons' but does not identify the method or its role; this should be clarified in the methods section for reproducibility.
  2. [results on planetary uncertainties] The propagation to planetary parameters is described only at the level of the abstract; a dedicated subsection or table showing the exact error-propagation steps (including any assumptions on stellar mass/radius correlations) would improve clarity.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive comments and the opportunity to clarify aspects of our analysis. We address the major comment below.

read point-by-point responses

  1. Referee: [the isochrone fitting and gr8stars I comparison section] The section describing the comparison of isochronal radii to SED-fitting radii from gr8stars I (and the propagation of scatters to planetary parameters): the central claim that the observed scatters (76 K, 0.14 dex, 0.07 dex) induce the quoted ≲3%/≲5%/≈4% fractional uncertainties on planetary radius/mass/Teq rests on treating the SED radii as an independent benchmark. The manuscript provides no quantitative test (e.g., overlap in photometry, model grids, or calibration steps) that the two pipelines are free of shared systematics; without this, the benchmark cannot independently confirm that the spectroscopic scatter is the dominant, well-quantified systematic.

    Authors: The fractional uncertainties on planetary radius (≲3%), mass (≲5%), and equilibrium temperature (≈4%) are derived solely from the observed method-to-method scatter among the five spectroscopic pipelines applied to the SOPHIE spectra (76 K in Teff, 0.14 dex in log g, 0.07 dex in [Fe/H]). These scatters are measured internally to the spectroscopic analysis and propagated through isochrone fitting; the gr8stars I SED radii are used only as an external consistency check for the resulting isochrone radii and for comparing isochronal versus spectroscopic log g. They play no role in quantifying or propagating the scatters themselves. We will revise the manuscript to state this distinction explicitly and to add a short discussion of why the spectroscopic and SED approaches are expected to have limited shared systematics (distinct input data—high-resolution spectra versus broadband photometry—and different modeling frameworks). This addresses the concern without requiring new quantitative overlap tests. revision: partial

Circularity Check

0 steps flagged

No significant circularity; derivation from measured method scatter and propagation is self-contained.

full rationale

The paper measures inter-method scatter (76 K, 0.14 dex, 0.07 dex) across five spectroscopic pipelines on the same 585 spectra, performs isochrone fitting on those inputs, and directly propagates the resulting mass/radius scatter to planetary parameters to obtain the ≲3 % / ≲5 % / ≈4 % figures. The gr8stars I SED radii appear only as an external comparison benchmark (abstract: "We use the radii determined by SED fitting in the first gr8stars paper as a comparison to our isochronal radii from this work"), not as an input that defines or forces the reported scatters or propagated uncertainties. No equation reduces a claimed prediction to a fitted quantity by construction, and the central result does not rest on a self-citation chain. The derivation is therefore independent of the benchmark comparison.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard stellar-evolution models and the assumption that SED radii are independent of spectroscopic results; no new free parameters or entities are introduced.

axioms (2)
  • domain assumption Isochrone models provide reliable mass, radius, and age estimates when supplied with spectroscopic Teff, log g, and [Fe/H].
    Invoked when converting the five sets of spectroscopic parameters into isochronal masses, radii, and ages for all 585 stars.
  • domain assumption SED-fitting radii from the companion paper are independent of the spectroscopic methods tested here.
    Used as the external benchmark for isochronal radii and for the log g comparison.

pith-pipeline@v0.9.1-grok · 5938 in / 1454 out tokens · 13694 ms · 2026-06-27T23:29:35.993530+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

130 extracted references · 118 canonical work pages · 55 internal anchors

  1. [1]

    Stellar Activity Masquerading as Planets in the Habitable Zone of the M dwarf Gliese 581

    Stellar activity masquerading as planets in the habitable zone of the M dwarf Gliese 581. Science , keywords =. doi:10.1126/science.1253253 , archivePrefix =. 1407.1049 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1253253

  2. [2]

    , keywords =

    Metal Pipe: A Broadly Applicable Stellar Abundance Pipeline Using Isochronal Parameters. , keywords =. doi:10.3847/1538-4357/ae3c0b , archivePrefix =. 2601.10794 , primaryClass =

    work page doi:10.3847/1538-4357/ae3c0b

  3. [3]

    Determining stellar macroturbulence using asteroseismic rotational velocities from Kepler

    Determining stellar macroturbulence using asteroseismic rotational velocities from Kepler. , keywords =. doi:10.1093/mnras/stu1692 , archivePrefix =. 1408.3988 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu1692

  4. [4]

    A new extensive library of PHOENIX stellar atmospheres and synthetic spectra

    A new extensive library of PHOENIX stellar atmospheres and synthetic spectra. , keywords =. doi:10.1051/0004-6361/201219058 , archivePrefix =. 1303.5632 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201219058

  5. [5]

    Using the Sun to estimate Earth-like planet detection capabilities. VI. Simulation of granulation and supergranulation radial velocity and photometric time series. , keywords =. doi:10.1051/0004-6361/201525721 , adsurl =

    work page doi:10.1051/0004-6361/201525721

  6. [6]

    RASSINE: Interactive tool for normalising stellar spectra. I. Description and performance of the code. , keywords =. doi:10.1051/0004-6361/202037722 , archivePrefix =. 2006.13098 , primaryClass =

    work page doi:10.1051/0004-6361/202037722 2006

  7. [7]

    , keywords =

    YARARA: Significant improvement in RV precision through post-processing of spectral time series. , keywords =. doi:10.1051/0004-6361/202140986 , archivePrefix =. 2106.07301 , primaryClass =

    work page doi:10.1051/0004-6361/202140986

  8. [8]

    , keywords =

    YARARA V2: Reaching sub-m s ^ -1 precision over a decade using PCA on line-by-line radial velocities. , keywords =. doi:10.1051/0004-6361/202347232 , archivePrefix =. 2308.11812 , primaryClass =

    work page doi:10.1051/0004-6361/202347232

  9. [9]

    Defining better activity proxies

    Stellar surface information from the Ca II H&K lines - II. Defining better activity proxies. , keywords =. doi:10.1093/mnras/stae2508 , archivePrefix =. 2411.00557 , primaryClass =

    work page doi:10.1093/mnras/stae2508

  10. [10]

    State of the Field: Extreme Precision Radial Velocities

    State of the Field: Extreme Precision Radial Velocities. , keywords =. doi:10.1088/1538-3873/128/964/066001 , archivePrefix =. 1602.07939 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1538-3873/128/964/066001

  11. [11]

    Characterisation of the radial velocity signal induced by rotation in late-type dwarfs

    Characterization of the radial velocity signal induced by rotation in late-type dwarfs. , keywords =. doi:10.1093/mnras/stx771 , archivePrefix =. 1703.08884 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx771

  12. [12]

    Measuring the masses of the two transiting planets

    One year of AU Mic with HARPS - I. Measuring the masses of the two transiting planets. , keywords =. doi:10.1093/mnras/stac614 , archivePrefix =. 2203.01750 , primaryClass =

    work page doi:10.1093/mnras/stac614

  13. [13]

    , keywords =

    Stellar signal components seen in HARPS and HARPS-N solar radial velocities. , keywords =. doi:10.1051/0004-6361/202244663 , archivePrefix =. 2211.04251 , primaryClass =

    work page doi:10.1051/0004-6361/202244663

  14. [14]

    The PLATO 2.0 Mission

    The PLATO 2.0 mission. Experimental Astronomy , keywords =. doi:10.1007/s10686-014-9383-4 , archivePrefix =. 1310.0696 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s10686-014-9383-4

  15. [15]

    On the Feasibility of Intense Radial Velocity Surveys for Earth-twin Discoveries

    On the Feasibility of Intense Radial Velocity Surveys for Earth-Twin Discoveries. , keywords =. doi:10.1093/mnras/sty1464 , archivePrefix =. 1806.00518 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1464

  16. [16]

    HARPS3 for a Roboticized Isaac Newton Telescope

    HARPS3 for a roboticized Isaac Newton Telescope. Ground-based and Airborne Instrumentation for Astronomy VI , year = 2016, editor =. doi:10.1117/12.2232111 , archivePrefix =. 1608.04611 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1117/12.2232111 2016

  17. [17]

    , keywords =

    Target Prioritization and Observing Strategies for the NEID Earth Twin Survey. , keywords =. doi:10.3847/1538-3881/abd79e , archivePrefix =. 2101.11689 , primaryClass =

    work page doi:10.3847/1538-3881/abd79e

  18. [18]

    The NEID Earth Twin Survey. I. Confirmation of a 31 Day Planet Orbiting HD 86728. , keywords =. doi:10.3847/1538-3881/ad89bf , archivePrefix =. 2409.12315 , primaryClass =

    work page doi:10.3847/1538-3881/ad89bf

  19. [19]

    Ground-based and Airborne Instrumentation for Astronomy X , year = 2024, editor =

    Development and design of Second Earth Initiative Spectrograph (2ES). Ground-based and Airborne Instrumentation for Astronomy X , year = 2024, editor =. doi:10.1117/12.3019107 , adsurl =

    work page doi:10.1117/12.3019107 2024

  20. [20]

    arXiv e-prints , keywords =

    Extreme Precision Radial Velocity Working Group Final Report. arXiv e-prints , keywords =. doi:10.48550/arXiv.2107.14291 , archivePrefix =. 2107.14291 , primaryClass =

    work page doi:10.48550/arxiv.2107.14291

  21. [21]

    , keywords =

    Catalog for the ESPRESSO blind radial velocity exoplanet survey. , keywords =. doi:10.1051/0004-6361/201834729 , archivePrefix =. 1908.04627 , primaryClass =

    work page doi:10.1051/0004-6361/201834729 1908

  22. [22]

    , keywords =

    Search for lithium-rich giants in 32 open clusters with high-resolution spectroscopy★. , keywords =. doi:10.1051/0004-6361/202244374 , archivePrefix =. 2303.16124 , primaryClass =

    work page doi:10.1051/0004-6361/202244374

  23. [23]

    Constraining planet structure and composition from stellar chemistry: trends in different stellar populations

    Constraining planet structure and composition from stellar chemistry: trends in different stellar populations. , keywords =. doi:10.1051/0004-6361/201731359 , archivePrefix =. 1711.00777 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731359

  24. [24]

    New and updated stellar parameters for 71 evolved planet hosts. On the metallicity - giant planet connection

    New and updated stellar parameters for 71 evolved planet hosts. On the metallicity-giant planet connection. , keywords =. doi:10.1051/0004-6361/201321641 , archivePrefix =. 1307.7870 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321641

  25. [25]

    Three regimes of extrasolar planets inferred from host star metallicities

    Three regimes of extrasolar planet radius inferred from host star metallicities. , keywords =. doi:10.1038/nature13254 , archivePrefix =. 1405.7695 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature13254

  26. [26]

    Science , keywords =

    A compositional link between rocky exoplanets and their host stars. Science , keywords =. doi:10.1126/science.abg8794 , archivePrefix =. 2102.12444 , primaryClass =

    work page doi:10.1126/science.abg8794

  27. [27]

    The Dartmouth Stellar Evolution Database

    The Dartmouth Stellar Evolution Database. , keywords =. doi:10.1086/589654 , archivePrefix =. 0804.4473 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/589654

  28. [28]

    Homogeneous stellar analysis of potential circumbinary planet hosts

    BEBOP V. Homogeneous stellar analysis of potential circumbinary planet hosts. , keywords =. doi:10.1093/mnras/stae1405 , archivePrefix =. 2406.03094 , primaryClass =

    work page doi:10.1093/mnras/stae1405

  29. [29]

    Astronomische Nachrichten , keywords =

    FIES: The high-resolution Fiber-fed Echelle Spectrograph at the Nordic Optical Telescope. Astronomische Nachrichten , keywords =. doi:10.1002/asna.201312007 , adsurl =

    work page doi:10.1002/asna.201312007

  30. [30]

    The SOPHIE search for northern extrasolar planets . I. A companion around HD 16760 with mass close to the planet/brown-dwarf transition. , keywords =. doi:10.1051/0004-6361/200912427 , adsurl =

    work page doi:10.1051/0004-6361/200912427

  31. [31]

    Ground-based and Airborne Instrumentation for Astronomy II , year = 2008, editor =

    The SOPHIE spectrograph: design and technical key-points for high throughput and high stability. Ground-based and Airborne Instrumentation for Astronomy II , year = 2008, editor =. doi:10.1117/12.787379 , adsurl =

    work page doi:10.1117/12.787379 2008

  32. [32]

    Determining stellar atmospheric parameters and chemical abundances of FGK stars with iSpec

    Determining stellar atmospheric parameters and chemical abundances of FGK stars with iSpec. , keywords =. doi:10.1051/0004-6361/201423945 , archivePrefix =. 1407.2608 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201423945

  33. [33]

    Modern stellar spectroscopy caveats

    Modern stellar spectroscopy caveats. , keywords =. doi:10.1093/mnras/stz549 , archivePrefix =. 1902.09558 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz549 1902

  34. [34]

    Memorie della Societa Astronomica Italiana Supplementi , keywords =

    ATLAS12, SYNTHE, ATLAS9, WIDTH9, et cetera. Memorie della Societa Astronomica Italiana Supplementi , keywords =

  35. [35]

    ATLAS and SYNTHE under Linux

    ATLAS and SYNTHE under Linux. Memorie della Societa Astronomica Italiana Supplementi , keywords =. doi:10.48550/arXiv.astro-ph/0406268 , archivePrefix =. astro-ph/0406268 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0406268

  36. [36]

    The Calibration of MK Spectral Classes Using Spectral Synthesis. I. The Effective Temperature Calibration of Dwarf Stars. , keywords =. doi:10.1086/116893 , adsurl =

    work page doi:10.1086/116893

  37. [37]

    Memorie della Societa Astronomica Italiana Supplementi , keywords =

    NIST atomic spectra database. Memorie della Societa Astronomica Italiana Supplementi , keywords =

  38. [38]

    isochrones: Stellar model grid package

  39. [39]

    , keywords =

    The Two Micron All Sky Survey (2MASS). , keywords =. doi:10.1086/498708 , adsurl =

    work page doi:10.1086/498708

  40. [40]

    Explanatory Supplement to the AllWISE Data Release Products

  41. [41]

    Improved spectroscopic parameters for transiting planet hosts

    Improved Spectroscopic Parameters for Transiting Planet Hosts. , keywords =. doi:10.1088/0004-637X/757/2/161 , archivePrefix =. 1208.1268 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/757/2/161

  42. [42]

    Correcting the spectroscopic surface gravity using transits and asteroseismology. No significant effect on temperatures or metallicities with ARES+MOOG in LTE

    Correcting the spectroscopic surface gravity using transits and asteroseismology. No significant effect on temperatures or metallicities with ARES and MOOG in local thermodynamic equilibrium. , keywords =. doi:10.1051/0004-6361/201424537 , archivePrefix =. 1410.1310 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201424537

  43. [43]

    , keywords =

    K2-111: an old system with two planets in near-resonance. , keywords =. doi:10.1093/mnras/staa3144 , archivePrefix =. 2010.01993 , primaryClass =

    work page doi:10.1093/mnras/staa3144 2010

  44. [44]

    2016, ApJS, 222, 8, doi: 10.3847/0067-0049/222/1/8

    MESA Isochrones and Stellar Tracks (MIST) 0: Methods for the Construction of Stellar Isochrones. , keywords =. doi:10.3847/0067-0049/222/1/8 , archivePrefix =. 1601.05144 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0067-0049/222/1/8

  45. [45]

    ``The Observation and Analysis of Stellar Photospheres, 3rd Edition, by D.F

    The Observation and Analysis of Stellar Photospheres. ``The Observation and Analysis of Stellar Photospheres, 3rd Edition, by D.F. Gray. ISBN 0521851866. <A href=''http://www.cambridge.org/us/catalogue/catalogue.asp?isbn=0521851866. Cambridge``>http://www.cambridge.org/us/catalogue/catalogue.asp?isbn=0521851866. Cambridge</A>, UK: Cambridge University Pre...

    2005

  46. [46]

    , keywords =

    Gaia FGK benchmark stars: Fundamental T _ eff and log g of the third version. , keywords =. doi:10.1051/0004-6361/202347136 , archivePrefix =. 2310.11302 , primaryClass =

    work page doi:10.1051/0004-6361/202347136

  47. [47]

    Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars. , keywords =. doi:10.1088/0004-637X/746/1/101 , archivePrefix =. 1112.3316 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/746/1/101

  48. [48]

    Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer

    Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer. , keywords =. doi:10.3847/1538-3881/aa9d8b , archivePrefix =. 1712.08109 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aa9d8b

  49. [49]

    Surveying the Bright Stars by Optical Interferometry. II. A Volume-limited Multiplicity Survey of Main-sequence F Stars. , keywords =. doi:10.3847/1538-4365/ab32e1 , adsurl =

    work page doi:10.3847/1538-4365/ab32e1

  50. [50]

    , keywords =

    Speckle interferometric observations of binary systems with the Hte-Provence 1.93 M telescope. , keywords =

  51. [51]

    Mn abundances in the stars of the Galactic disc with metallicities -1.0 < [Fe/H] < 0.3

    Mn abundances in the stars of the Galactic disc with metallicities -1.0 < [Fe/H] < 0.3. , keywords =. doi:10.1093/mnras/stv2038 , archivePrefix =. 1509.05341 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2038

  52. [52]

    VizieR Online Data Catalog: Li abundances & vsini for star-planet systems (Gonzalez+, 2010)

    2010

  53. [53]

    , keywords =

    Homogeneous abundance analysis of FGK dwarf, subgiant, and giant stars with and without giant planets. , keywords =. doi:10.1051/0004-6361/201525770 , adsurl =

    work page doi:10.1051/0004-6361/201525770

  54. [54]

    Abundances in the Local Region II: F, G and K Dwarfs and Subgiants

    Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants. , keywords =. doi:10.3847/1538-3881/153/1/21 , archivePrefix =. 1611.02897 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/153/1/21

  55. [55]

    Oxygen Abundances in Nearby Stars. Clues to the formation and evolution of the Galactic disk

    Oxygen abundances in nearby stars. Clues to the formation and evolution of the Galactic disk. , keywords =. doi:10.1051/0004-6361:20066619 , archivePrefix =. astro-ph/0701362 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20066619

  56. [56]

    New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey

    New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey. , keywords =. doi:10.1051/0004-6361/201016276 , archivePrefix =. 1103.4651 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201016276

  57. [57]

    Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue. , keywords =. doi:10.1051/0004-6361/201731533 , archivePrefix =. 1801.09698 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731533

  58. [58]

    Stellar and substellar companions of nearby stars from Gaia DR2 - Binarity from proper motion anomaly

    Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly. , keywords =. doi:10.1051/0004-6361/201834371 , archivePrefix =. 1811.08902 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201834371

  59. [59]

    The Gaia mission

    The Gaia mission. , keywords =. doi:10.1051/0004-6361/201629272 , archivePrefix =. 1609.04153 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629272

  60. [60]

    Summary of the content and survey properties

    Gaia Data Release 3. Summary of the content and survey properties. , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =

    work page doi:10.1051/0004-6361/202243940

  61. [61]

    and Amarsi, A

    The chemical make-up of the Sun: A 2020 vision. , keywords =. doi:10.1051/0004-6361/202140445 , archivePrefix =. 2105.01661 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202140445 2020

  62. [62]

    , keywords =

    Atomic data for the Gaia-ESO Survey. , keywords =. doi:10.1051/0004-6361/201936291 , archivePrefix =. 2011.02049 , primaryClass =

    work page doi:10.1051/0004-6361/201936291 2011

  63. [63]

    Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES-2

    Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES-2. , keywords =. doi:10.1086/519214 , archivePrefix =. 0704.2938 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/519214

  64. [64]

    Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs. , keywords =. doi:10.1086/430500 , adsurl =

    work page doi:10.1086/430500

  65. [65]

    The PASTEL catalogue: 2016 version

    The PASTEL catalogue: 2016 version. , keywords =. doi:10.1051/0004-6361/201628497 , archivePrefix =. 1605.07384 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201628497 2016

  66. [66]

    , keywords =

    A Guide to Realistic Uncertainties on the Fundamental Properties of Solar-type Exoplanet Host Stars. , keywords =. doi:10.3847/1538-4357/ac4bbc , archivePrefix =. 2012.07957 , primaryClass =

    work page doi:10.3847/1538-4357/ac4bbc 2012

  67. [67]

    , keywords =

    Exploring the M-dwarf Luminosity-Temperature-Radius relationships using Gaia DR2. , keywords =. doi:10.1093/mnras/stz2242 , archivePrefix =. 1908.03025 , primaryClass =

    work page doi:10.1093/mnras/stz2242 1908

  68. [68]

    , keywords =

    Erratum: Exploring the M-dwarf Luminosity-Temperature-Radius relationships using Gaia DR2. , keywords =. doi:10.1093/mnras/staa926 , adsurl =

    work page doi:10.1093/mnras/staa926

  69. [69]

    SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs. I. New atmospheric parameters and masses for 48 stars with planets. , keywords =. doi:10.1051/0004-6361/201321286 , archivePrefix =. 1307.0354 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321286

  70. [70]

    Determination of Atmospheric Parameters of B , publisher =

    ARES + MOOG: A Practical Overview of an Equivalent Width (EW) Method to Derive Stellar Parameters. Determination of Atmospheric Parameters , publisher =. doi:10.1007/978-3-319-06956-2_26 , adsurl =

    work page doi:10.1007/978-3-319-06956-2_26

  71. [71]

    Higher quality spectra and precise parallaxes from Gaia eDR3

    SWEET-Cat 2.0: The Cat just got SWEETer. Higher quality spectra and precise parallaxes from Gaia eDR3. , keywords =. doi:10.1051/0004-6361/202141584 , archivePrefix =. 2109.04781 , primaryClass =

    work page doi:10.1051/0004-6361/202141584

  72. [72]

    A new code for automatic determination of equivalent widths: Automatic Routine for line Equivalent widths in stellar Spectra (ARES)

    A new code for automatic determination of equivalent widths: Automatic Routine for line Equivalent widths in stellar Spectra (ARES). , keywords =. doi:10.1051/0004-6361:20077288 , archivePrefix =. astro-ph/0703696 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20077288

  73. [73]

    ARES v2 - new features and improved performance

    ARES v2: new features and improved performance. , keywords =. doi:10.1051/0004-6361/201425463 , archivePrefix =. 1504.02725 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201425463

  74. [74]

    Spectroscopic parameters for 451 stars in the HARPS GTO planet search program. Stellar [Fe/H] and the frequency of exo-Neptunes

    Spectroscopic parameters for 451 stars in the HARPS GTO planet search program. Stellar [Fe/H] and the frequency of exo-Neptunes. , keywords =. doi:10.1051/0004-6361:200809698 , archivePrefix =. 0805.4826 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:200809698

  75. [75]

    SYNTHE spectrum synthesis programs and line data

  76. [76]

    Carbon and Nitrogen Abundances in Metal-Poor Stars

  77. [77]

    Deriving precise parameters for cool solar-type stars. Optimizing the iron line list

    Deriving precise parameters for cool solar-type stars. Optimizing the iron line list. , keywords =. doi:10.1051/0004-6361/201321103 , archivePrefix =. 1304.6639 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321103

  78. [78]

    aren, mit besonderer Ber\

    Physik der Sternatmosph\"aren, mit besonderer Ber\"ucksichtigung der Sonne. Berlin, Springer, 1955. 2. Aufl. Berlin, Springer, 1955. 2. Aufl. , year = 1955, adsurl =

    1955

  79. [79]

    Atmospheric stellar parameters for large surveys using FASMA, a new spectral synthesis package

    Atmospheric stellar parameters for large surveys using FASMA, a new spectral synthesis package. , keywords =. doi:10.1093/mnras/stx2564 , archivePrefix =. 1710.00260 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx2564

  80. [80]

    The Journal of Open Source Software , keywords =

    FASMA 2.0: A Python package for stellar parameters and chemical abundances. The Journal of Open Source Software , keywords =. doi:10.21105/joss.02048 , adsurl =

    work page doi:10.21105/joss.02048

Showing first 80 references.