Pith. sign in

REVIEW 3 major objections 6 minor 54 references

The GaiaNIR spectrograph should observe a 42 nm window at 1926–1968 nm in the K band at R≈16,000–20,000, where it can match Gaia's radial-velocity and stellar-parameter precision while seeing through roughly 7.4 times less interstellar dust

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-01 22:17 UTC pith:UYXYEVJD

load-bearing objection Plausible case for the K-band GaiaNIR window, but the central claim still needs empirical K-band validation before it should drive hardware decisions. the 3 major comments →

arxiv 2607.15796 v2 pith:UYXYEVJD submitted 2026-07-17 astro-ph.IM astro-ph.SR

Radial velocity and atmospheric parameter calculations for the GaiaNIR spectrograph

Szabolcs M\'esz\'aros , David Hobbs , Anna Liptrott , David Katz , Ricardo Schiavon , Vikt\'oria Pap , Anthony G. A. Brown , George Seabroke
show 3 more authors
Joss Bland-Hawthorn Ronny Blomme Nicholas A. Walton
This is my paper
classification astro-ph.IM astro-ph.SR
keywords GaiaNIRnear-infrared spectroscopyradial velocity precisionstellar atmospheric parametersK bandsynthetic spectraBOSZinterstellar extinction
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper identifies the wavelength window that a proposed near-infrared all-sky survey should use for its high-resolution spectrograph. Scanning 800–2300 nm with 10,000 synthetic stellar spectra, the authors find that a 42 nm window centered near 1947 nm—between 1926 and 1968 nm in the K band—offers the best balance of radial-velocity and atmospheric-parameter precision. At resolutions of 16,000–20,000, it reaches radial-velocity scatter of about 160–260 m/s for bright FGKM stars, temperature precision better than 100 K, and metallicity precision better than 0.08 dex, all comparable to Gaia's Radial Velocity Spectrometer. Because interstellar extinction is about 7.4 times lower at these wavelengths than in the optical, this window would let the mission map the dust-obscured disk and far side of the Milky Way. A secondary window at 1158–1202 nm reaches hotter stars but offers less extinction relief.

Core claim

The central claim is that the optimal spectral range for the GaiaNIR spectrograph is the K-band window 1926–1968 nm at a resolution around 16,100–20,100. Using synthetic BOSZ spectra with injected noise and Doppler shifts, the authors show that this window delivers radial-velocity precision of roughly 160–260 m/s for the brightest FGKM stars and atmospheric-parameter precisions better than 100 K in effective temperature and 0.08 dex in metallicity—values they argue are on par with Gaia's RVS. The same window supports abundance measurements of ten species (O, Na, Mg, Si, Ca, Ti, V, Cr, Mn, Ni) for cool giants while taking advantage of the K band's roughly 7.4-fold reduction in interstellar ex

What carries the argument

The analysis is carried by a simulation pipeline built on the BOSZ synthetic spectral library: 10,000 random stellar parameter combinations (Teff 2800–10,000 K, log g 0–5.5, [M/H] −1.5 to 0.5) were rendered at resolutions 5000–20,000, shifted by random radial velocities, given Gaussian noise, and cross-correlated against noise-free templates to measure velocity scatter. Candidate windows were then fit with FERRE to estimate Teff, log g, and [M/H] precision. The detector-resolution relation R = λC·NR/(λr·NP) ties window width to achievable resolution, and a 1% flux-difference threshold defines detectable abundance species.

Load-bearing premise

The recommendation assumes the BOSZ synthetic spectra are accurate enough in the 1926–1968 nm window—especially the line list and H2O opacity—to make the relative ranking of windows by scatter trustworthy; the method is validated only in the optical RVS window, not in the K band.

What would settle it

Observe a set of bright FGKM standard stars with an existing high-resolution K-band spectrograph covering 1926–1968 nm and compare measured radial velocities and atmospheric parameters against precise literature values. If the empirical scatter is substantially larger than the 160–260 m/s and <100 K/0.08 dex predicted here—or if the synthetic line list is found to miss strong lines in that window—the optimal wavelength and resolution recommendation would need to move.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • If adopted, a single 42 nm K-band window would give GaiaNIR the same radial-velocity and stellar-parameter capabilities as Gaia's optical RVS, but for stars hidden behind dust.
  • The quoted precisions hold for bright (S/N>40) FGKM stars; the paper cautions that low-S/N velocities are underestimated by a factor of 2–3 and need further study.
  • The K-band window yields ten measurable species in cool giants (O, Na, Mg, Si, Ca, Ti, V, Cr, Mn, Ni), enabling chemical-tagging and accretion-history science in the obscured Milky Way.
  • M-dwarf spectra in the K band are dominated by H2O, leaving Ca as the only measurable abundance; the 1158–1202 nm window would recover six species for the coolest dwarfs.
  • The recommended window is a compromise: the 1984–2000 nm sub-window gives better radial velocities (~118 m/s) but much worse atmospheric parameters, while the full 1926–2000 nm range gives poorer velocities unless resolution is pushed to ~14,000.

Where Pith is reading between the lines

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

  • The paper validates its precision estimates only against Gaia's 845–872 nm window, so the K-band numbers carry an implicit assumption that the synthetic line list is complete in that region; an empirical K-band accuracy test against a few dozen standard stars would be the natural next step.
  • If the K-band window is selected, the mission's ability to study M dwarfs—expected to be a large fraction of targets—depends on either improving H2O line treatment or pairing the K-band spectrograph with the 1158–1202 nm window.
  • The 7.4× extinction advantage rests on a standard extinction law; in dense, highly variable sightlines the actual gain may differ, which could shift the optimal wavelength choice for specific survey fields.
  • The same simulation pipeline could be rerun for a hypothetical two-window configuration—one K-band channel for giants and a shorter channel for dwarfs/hot stars—to test whether the abundance and temperature coverage gains outweigh detector and crowding costs.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. This manuscript addresses the design of the GaiaNIR spectrograph by searching the 800–2300 nm range for the wavelength window that best balances radial-velocity (RV) precision, atmospheric-parameter precision, and interstellar extinction. Using 10,000 BOSZ synthetic spectra with injected noise and Doppler shifts, the authors cross-correlate mock observations with ideal templates to map RV scatter versus wavelength and resolution, then use FERRE to estimate Teff/logg/[M/H] precision in six down-selected windows. They validate their simulation pipeline against Gaia RVS performance at 845–872 nm (§3.1), then recommend 1926–1968 nm at R ≈ 16100–20100 as the optimal compromise, with a secondary 1158–1202 nm window, claiming RVs of 160–260 m/s for bright FGKM stars and atmospheric-parameter precisions better than 100 K in Teff and 0.08 dex in metallicity.

Significance. The result is potentially important: if the K-band window performs as predicted, GaiaNIR could obtain Gaia-RVS-comparable spectroscopy through roughly 7 times lower extinction than the optical, enabling the mission's core obscured-Milky-Way science. The study is systematic and transparent: the parameter sweep is broad, the RV and atmospheric-parameter metrics are clearly defined, and the comparison with Gaia DR3 provides a useful external check. No parameter is fitted to force the recommended window; the recommendation emerges from the simulations. The main caveat is external validity: the Gaia validation is at 845–872 nm only, and the K-band recommendation rests entirely on BOSZ synthetic spectra whose line lists and opacities are unvalidated in this region. The paper itself acknowledges major line-list work remains.

major comments (3)
  1. [§3.1 / §4] The method is validated only in the 845–872 nm RVS range against Gaia DR3; no observed K-band spectra are used to test BOSZ in the recommended 1926–1968 nm window. Because the central conclusion is a ranking of windows based on simulated scatter, a line-list defect, missing opacity, or wrong gf-values in the K band could change the ranking and the recommended window. The paper's own conclusion ('significant effort will need to be put forward creating a new line list') underscores this risk. I ask for either (a) a direct validation of BOSZ K-band spectra against high-resolution observed spectra (e.g., infrared atlases of FGK standards), or (b) a sensitivity analysis that perturbs line lists/opacities in the candidate windows and shows the 1926–1968 nm recommendation is robust. Without this, the headline recommendation is not fully supported.
  2. [§3.1] The authors report that at low S/N their simulated RV scatter is a factor of 2–3 smaller than Gaia DR3's observed precision, and they note that 'the bulk of GaiaNIR targets will be fainter.' This is a load-bearing limitation: the quoted 160–260 m/s applies to the brightest stars at S/N>40, while the mission's scientific return for the dust-obscured Milky Way depends on fainter targets. The paper should either model the expected S/N distribution of GaiaNIR targets and propagate the corrected low-S/N errors, or clearly scope the recommendation as applying only to the bright-star regime and explain why the window choice is insensitive to the low-S/N correction.
  3. [§3.2] The abundance detectability test uses a +0.2 dex perturbation and a 1% flux-difference threshold at S/N=100 with no noise realizations or recovery fraction. The list of 'available species' in Table 1 and the abstract is a central part of the optimal-window argument, since the paper weighs the number of measurable species when comparing windows. A more robust injection-recovery test (varying the perturbation size, including noise, and quantifying completeness) is needed to support the claim that ten species can be derived from the recommended window.
minor comments (6)
  1. [Table 1 / Abstract / Conclusions] Species counts are inconsistent: the abstract lists 'O, Na, Mg, Si, Ca, Ti, V, Cr, Mn, Ni' for the K band, but Table 1 and §3.5 indicate that in the recommended 1926–1968 nm window Mn is absent and Al is present; the Conclusions say 'nine distinct species' and then enumerate 11. Please harmonize.
  2. [§3.2] 'Figures 8−7' should be 'Figures 7−8'.
  3. [Fig. 2] The bottom panel caption should specify the line styles/colors used for the four resolutions (5000, 10000, 15000, 20000).
  4. [§2.3] Provide a version or citation for PyAstronomy's crosscorrRV function.
  5. [Table 1] Define σ_v, σ_Teff, σ_logg, and σ_[M/H] in the caption and visually separate the five detector configurations per window for readability.
  6. [§3.1] Clarify the S/N definition (per pixel? per resolution element?) and whether 'scatter' is the standard deviation of residuals after the ±50 km/s outlier rejection.

Circularity Check

0 steps flagged

No significant circularity; the 1926–1968 nm recommendation is an externally benchmarked simulation, not a fitted prediction.

full rationale

The derivation chain is self-contained and does not reduce to its inputs. The RV precision per 100 nm window is measured by injecting noise and a random Doppler shift into BOSZ spectra and cross-correlating each mock with its own noise-free 'ideal template' (§2.3). This is a controlled self-consistency experiment; the paper explicitly states that it 'excluded systematic errors from a template mismatch,' and it applies the identical procedure to all windows, so the relative ranking of windows is meaningful even if absolute precision is optimistic. No parameter is fitted to force the recommended window: the six candidates emerge from uniform scatter statistics, and the preference for longer wavelengths is an exogenous science priority (7.4 times lower extinction, Cardelli et al. 1989), not an output of the fit. The method is externally anchored in §3.1: simulated precisions for the 845–872 nm window (83.1 K in Teff, 0.15 dex in logg, 0.06 dex in [M/H], ~157 m/s at S/N=100) are compared with Gaia DR3 empirical scatter (90.3 K, 0.19 dex, 0.13 dex, 120–140 m/s), i.e., independent external benchmarks; the comparison is favorable and honestly notes the low-S/N mismatch. The only notable self-citation is the BOSZ grid (Mészáros et al. 2024), co-authored by the paper's first author, which is the input spectral library. This is not load-bearing circularity: BOSZ is a published, parameter-free grid with stated assumptions, and the target result (optimal window selection) is not an input to its construction; the window recommendation is not used to validate BOSZ. The genuine risk is K-band model fidelity — line-list completeness and opacity accuracy at 1926–1968 nm are not validated against observed K-band spectra, a limitation the authors themselves flag ('Significant effort will need to be put forward creating a new line list'). That is an external-validity correctness risk, not an internal circular step. Accordingly the score is a low 2, reflecting the minor self-citation and the self-consistent (ideal-template) methodology, with the central derivation otherwise independent.

Axiom & Free-Parameter Ledger

4 free parameters · 6 axioms · 0 invented entities

The central recommendation rests on model-fidelity assumptions rather than newly fitted constants. The only hand-chosen numbers are detection thresholds, S/N cuts, and the fixed microturbulence; none are fitted to force the K-band result. The most important unvalidated input is the BOSZ synthetic grid in the K band, which is exactly where the recommendation lives.

free parameters (4)
  • Abundance detectability threshold = 1% flux residual for +0.2 dex abundance change
    Chosen by hand in §3.2; directly sets which species appear as 'available' in Table 2.4.
  • RV outlier exclusion cut = ±50 km/s
    Applied in §2.3 before computing scatter; changes the quoted σvrad values and thus the window ranking.
  • Microturbulent velocity = 2 km/s
    Fixed for both the BOSZ grid and the FERRE fitting grids; real stars with different microturbulence could shift recovered Teff, logg, and [M/H].
  • Atmospheric-parameter sample cuts = S/N > 40; 4000 < Teff < 7000 K for Table 2.4
    Used to quote atmospheric-parameter precisions; different cuts would change the comparisons between windows.
axioms (6)
  • domain assumption BOSZ LTE synthetic spectra with MARCS/ATLAS9 atmospheres and 23 molecular line lists are realistic enough to rank RV and parameter precision across 800–2300 nm.
    Central to the whole method; §2.3 states no comprehensive empirical NIR library exists, and §3.1 validates the approach only at 845–872 nm.
  • domain assumption The Cardelli et al. extinction law describes NIR extinction, with K-band extinction roughly 7.4 times lower than optical.
    Used in §2.2 and §3.5 as the strategic reason to prefer the K band over shorter-wavelength candidates.
  • domain assumption Cross-correlation against the true noiseless template is a valid proxy for relative RV precision across different windows.
    Explicit in §2.3; this removes template mismatch and makes the estimates optimistic, especially at low S/N as acknowledged in §3.1.
  • domain assumption FERRE's grid interpolation with χ² minimization recovers Teff, logg, and [M/H] without bias beyond the reported scatter.
    Invoked in §2.4; the appendix notes noding effects when spectra are weakly sensitive to a parameter.
  • domain assumption A Gaia-RVS-like architecture with 3 pixels per resolution element and Equation 1 determines the achievable resolution for a given window and detector size.
    Equation 1 in §2.1 sets all resolutions reported in Table 2.4.
  • domain assumption The atomic and molecular line lists used in the abundance detectability study (VALD3 plus Plez molecular lists) are complete enough in the K band.
    Used in §3.2; the conclusions call for significant future K-band line-list work, undermining completeness confidence.

pith-pipeline@v1.3.0-alltime-deepseek · 28892 in / 12683 out tokens · 109175 ms · 2026-08-01T22:17:27.426798+00:00 · methodology

0 comments
read the original abstract

Context. The upcoming GaiaNIR mission is currently planning to add a near-infrared spectrograph to its payload in order to enhance its scientific return, particularly for mapping the dust-obscured regions of the Milky Way. Aims. This study aims to identify the optimal wavelength region between 800 and 2300 nm for the proposed GaiaNIR spectrograph to maximize the precision of radial velocities and atmospheric parameters. Methods. To find its spectral range, we generated 10000 synthetic spectra from the BOSZ library across a wide range of stellar parameters, with resolutions varying from 5000 to 20000. By cross-correlating these mock observations with ideal templates, we assessed the statistical scatter of velocity residuals to isolate six candidate windows for further atmospheric parameter testing. Results. Our analysis finds that the 1926 - 1968 nm window at R = 16100 - 20100 in the K-band is the preferred strategic choice, because it has the potential to reach radial velocity precision for the brightest FGKM stars of about 160 - 260 m/s depending on resolution, while providing precision of the atmospheric parameters close to Gaia's Radial Velocity Spectrometer. We also identified a second region between 1158 and 1202 nm (R = 9300 - 11600), that has slightly lower radial velocity precision, but at a wider temperature range than the K-band. Both regions make it possible to derive abundances of ten species at these resolutions: O, Na, Mg, Si, Ca, Ti, V, Cr, Mn, Ni in the K-band, and Mg, Si, K, Ca, Ti, V, Cr, Mn, Co, Ni between 1158 - 1202 nm. Conclusions. The K-band delivers sufficiently precise measurements for the mission's primary cool star targets while taking advantage of significantly lower interstellar extinction, enabling the mapping of the dust-obscured regions of the Milky Way.

Figures

Figures reproduced from arXiv: 2607.15796 by Anna Liptrott, Anthony G. A. Brown, David Hobbs, David Katz, George Seabroke, Joss Bland-Hawthorn, Nicholas A. Walton, Ricardo Schiavon, Ronny Blomme, Szabolcs M\'esz\'aros, Vikt\'oria Pap.

Figure 1
Figure 1. Figure 1 [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Estimated precision of vrad as a function of central wavelength using a wavelength region of 100 nm. The top panel shows the scatter, P95, and median absolute deviation of the differences between the derived and assigned velocities for R = 10 000. The bottom panel illustrates the variation in the scatter when the resolution changes from 5000 to 20 000. The wavelength range covered by the Gaia and APOGEE sp… view at source ↗
Figure 3
Figure 3. Figure 3: Estimated average scatter in the radial velocity differences as a function of central wavelength. The gray areas highlight the initial three regions that were selected for the further analysis. These regions were selected to provide a low scatter of vrad across a wide range of effective temperatures. The solid line shows the scatter, and the dotted line denotes the MAD. atmospheric parameters (Teff, log g,… view at source ↗
Figure 4
Figure 4. Figure 4: Normalized flux of sample spectra in the three 100 nm windows selected in the first phase. Six windows were chosen for the further analysis of atmospheric parameter precision, these are shaded gray in the figure. The normalized flux was shifted by arbitrary numbers to aid visibility. 175−200 m s−1 at S/N ≈ 100, which flattens out at 120−140 m s−1 for the brightest stars. Our estimated precision is 157 m s−… view at source ↗
Figure 5
Figure 5. Figure 5: Average scatter in the radial velocity differences as a function of R for the six wavelength windows selected in Section 2. The S/N > 40 in all panels. The synthetic spectra were computed using MARCS (Gustafsson et al. 2008) model atmospheres in combination with the radiative transfer code Turbospectrum, assuming LTE for all elements. Atomic line data were adopted from VALD3 (Ryabchikova et al. 2015), and … view at source ↗
Figure 6
Figure 6. Figure 6: Average scatter in the differences of vrad, Teff, log g, and [M/H] as a function of R for the six wavelength windows selected in Section 2. Each colored line represent a different down-selected window listed in [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Elements in the λC = 1947 nm window with residuals larger than 0.01 for an abundance change of 0.2 dex in the selected synthetic spectra, as indicated in the figure. appear from the spectra above 9000−10 000 K, making it very difficult to measure radial velocities or atmospheric parameters of OBA stars. When we take the decreased ability to measure radial veloc￾ities and atmospheric parameters into account… view at source ↗
Figure 8
Figure 8. Figure 8: Elements in the λC = 1180 nm window with residuals larger than 0.01 for an abundance change of 0.2 dex in the selected synthetic spectra, as indicated in the figure. tailed chemical abundance studies of the inner Milky Way and the far side of the Galactic disk. While the λC = 1984 nm region gives the most precise vrad values, a decent compromise might therefore be achieved by selecting the λC = 1947 nm reg… view at source ↗

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

54 extracted references · 45 linked inside Pith

  1. [1]

    Summary of the contents and survey properties

    Gaia Early Data Release 3. Summary of the contents and survey properties. , keywords =. doi:10.1051/0004-6361/202039657 , archivePrefix =. 2012.01533 , primaryClass =

    Pith/arXiv arXiv 2012

  2. [2]

    InfTars - Információs Társadalom , keywords =

    The Past, Present and Future of the ELKH Cloud. InfTars - Információs Társadalom , keywords =. doi:inftars.XXII.2022.2.8 , adsurl =

    2022

  3. [3]

    , keywords =

    The Solar Chemical Composition. , keywords =. doi:10.1007/s11214-007-9173-7 , adsurl =

    doi:10.1007/s11214-007-9173-7

  4. [4]

    , year = 2015, month = may, volume =

    A major upgrade of the VALD database. , year = 2015, month = may, volume =. doi:10.1088/0031-8949/90/5/054005 , adsurl =

    doi:10.1088/0031-8949/90/5/054005 2015

  5. [5]

    , keywords =

    The Relationship between Infrared, Optical, and Ultraviolet Extinction. , keywords =. doi:10.1086/167900 , adsurl =

    doi:10.1086/167900

  6. [6]

    G _ RVS photometry from the RVS spectra

    Gaia Data Release 3. G _ RVS photometry from the RVS spectra. , keywords =. doi:10.1051/0004-6361/202243615 , archivePrefix =. 2206.05725 , primaryClass =

    Pith/arXiv arXiv

  7. [7]

    Properties and validation of the radial velocities

    Gaia Data Release 3. Properties and validation of the radial velocities. , keywords =. doi:10.1051/0004-6361/202244220 , archivePrefix =. 2206.05902 , primaryClass =

    Pith/arXiv arXiv

  8. [8]

    Analysis of RVS spectra using the General Stellar Parametriser from spectroscopy

    Gaia Data Release 3. Analysis of RVS spectra using the General Stellar Parametriser from spectroscopy. , keywords =. doi:10.1051/0004-6361/202243750 , archivePrefix =. 2206.05541 , primaryClass =

    Pith/arXiv arXiv

  9. [9]

    Sloan Digital Sky Survey. V. Pioneering Panoptic Spectroscopy. , keywords =. doi:10.3847/1538-3881/ae0576 , archivePrefix =. 2507.06989 , primaryClass =

    Pith/arXiv arXiv

  10. [10]

    , keywords =

    SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19. , keywords =. doi:10.3847/1538-3881/ade4b9 , archivePrefix =. 2506.07845 , primaryClass =

    Pith/arXiv arXiv

  11. [11]

    Gaia Radial Velocity Spectrometer

    Gaia Data Release 2. Gaia Radial Velocity Spectrometer. , keywords =. doi:10.1051/0004-6361/201832763 , archivePrefix =. 1804.09369 , primaryClass =

    Pith/arXiv arXiv

  12. [12]

    Experimental Astronomy , keywords =

    All-sky visible and near infrared space astrometry. Experimental Astronomy , keywords =. doi:10.1007/s10686-021-09705-z , archivePrefix =. 1907.12535 , primaryClass =

    Pith/arXiv arXiv 1907

  13. [13]

    arXiv e-prints , keywords =

    GaiaNIR: Combining optical and Near-Infra-Red (NIR) capabilities with Time-Delay-Integration (TDI) sensors for a future Gaia-like mission. arXiv e-prints , keywords =. doi:10.48550/arXiv.1609.07325 , archivePrefix =. 1609.07325 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1609.07325

  14. [14]

    Summary of the contents and survey properties

    Gaia Data Release 2. Summary of the contents and survey properties. , keywords =. doi:10.1051/0004-6361/201833051 , archivePrefix =. 1804.09365 , primaryClass =

    Pith/arXiv arXiv

  15. [15]

    Summary of the astrometric, photometric, and survey properties

    Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties. , keywords =. doi:10.1051/0004-6361/201629512 , archivePrefix =. 1609.04172 , primaryClass =

    Pith/arXiv arXiv

  16. [16]

    , keywords =

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

    Pith/arXiv arXiv

  17. [17]

    , keywords =

    The updated BOSZ synthetic stellar spectral library. , keywords =. doi:10.1051/0004-6361/202449306 , archivePrefix =. 2407.10872 , primaryClass =

    Pith/arXiv arXiv

  18. [18]

    , keywords =

    ASPCAP: The APOGEE Stellar Parameter and Chemical Abundances Pipeline. , keywords =. doi:10.3847/0004-6256/151/6/144 , archivePrefix =. 1510.07635 , primaryClass =

    Pith/arXiv arXiv

  19. [19]

    , keywords =

    APOGEE Data and Spectral Analysis from SDSS Data Release 16: Seven Years of Observations Including First Results from APOGEE-South. , keywords =. doi:10.3847/1538-3881/aba592 , archivePrefix =. 2007.05537 , primaryClass =

    Pith/arXiv arXiv 2007

  20. [20]

    , keywords =

    The GALAH survey: effective temperature calibration from the InfraRed Flux Method in the Gaia system. , keywords =. doi:10.1093/mnras/stab2304 , archivePrefix =. 2011.02517 , primaryClass =

    Pith/arXiv arXiv 2011

  21. [21]

    The Southern clusters and overview

    Homogeneous analysis of globular clusters from the APOGEE survey with the BACCHUS code - II. The Southern clusters and overview. , keywords =. doi:10.1093/mnras/stz3496 , archivePrefix =. 1912.04839 , primaryClass =

    Pith/arXiv arXiv 1912

  22. [22]

    Homogeneous analysis of globular clusters from the APOGEE survey with the BACCHUS code. I. The northern clusters. , keywords =. doi:10.1051/0004-6361/201834550 , archivePrefix =. 1812.08817 , primaryClass =

    Pith/arXiv arXiv

  23. [23]

    , keywords =

    Exploring Anticorrelations and Light Element Variations in Northern Globular Clusters Observed by the APOGEE Survey. , keywords =. doi:10.1088/0004-6256/149/5/153 , archivePrefix =. 1501.05127 , primaryClass =

    Pith/arXiv arXiv

  24. [24]

    The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17. , keywords =. doi:10.3847/1538-3881/ac7ce5 , archivePrefix =. 2206.13650 , primaryClass =

    Pith/arXiv arXiv

  25. [25]

    The Open Cluster Chemical Abundances and Mapping Survey. IV. Abundances for 128 Open Clusters Using SDSS/APOGEE DR16. , keywords =. doi:10.3847/1538-3881/ab77bc , archivePrefix =. 2002.08980 , primaryClass =

    Pith/arXiv arXiv 2002

  26. [26]

    The Open Cluster Chemical Abundances and Mapping Survey. II. Precision Cluster Abundances for APOGEE Using SDSS DR14. , keywords =. doi:10.3847/1538-3881/aad635 , archivePrefix =. 1807.09791 , primaryClass =

    Pith/arXiv arXiv

  27. [27]

    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 =

    Pith/arXiv arXiv

  28. [28]

    , keywords =

    The Gaia-ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy. , keywords =. doi:10.1051/0004-6361/202243141 , archivePrefix =. 2206.02901 , primaryClass =

    Pith/arXiv arXiv

  29. [29]

    , keywords =

    Calibrations of Atmospheric Parameters Obtained from the First Year of SDSS-III APOGEE Observations. , keywords =. doi:10.1088/0004-6256/146/5/133 , archivePrefix =. 1308.6617 , primaryClass =

    Pith/arXiv arXiv

  30. [30]

    , keywords =

    The APOGEE Data Release 16 Spectral Line List. , keywords =. doi:10.3847/1538-3881/abefdc , archivePrefix =. 2103.10112 , primaryClass =

    Pith/arXiv arXiv

  31. [31]

    arXiv e-prints , keywords =

    SDSS-V: Pioneering Panoptic Spectroscopy. arXiv e-prints , keywords =. doi:10.48550/arXiv.1711.03234 , archivePrefix =. 1711.03234 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1711.03234

  32. [32]

    , keywords =

    APOGEE Data Releases 13 and 14: Data and Analysis. , keywords =. doi:10.3847/1538-3881/aad4f9 , archivePrefix =. 1807.09773 , primaryClass =

    Pith/arXiv arXiv

  33. [33]

    , keywords =

    NLTE for APOGEE: simultaneous multi-element NLTE radiative transfer. , keywords =. doi:10.1051/0004-6361/201937054 , archivePrefix =. 2003.13353 , primaryClass =

    Pith/arXiv arXiv 2003

  34. [34]

    arXiv e-prints , keywords =

    TLUSTY and SYNSPEC Users's Guide IV: Upgraded Versions 208 and 54. arXiv e-prints , keywords =. doi:10.48550/arXiv.2104.02829 , archivePrefix =. 2104.02829 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2104.02829

  35. [35]

    , keywords =

    APOGEE Net: An Expanded Spectral Model of Both Low-mass and High-mass Stars. , keywords =. doi:10.3847/1538-3881/ac4de7 , archivePrefix =. 2201.03661 , primaryClass =

    Pith/arXiv arXiv

  36. [36]

    , keywords =

    A Spectroscopic Study of the Ancient Milky Way: F- and G-Type Stars in the Third Data Release of the Sloan Digital Sky Survey. , keywords =. doi:10.1086/498131 , archivePrefix =. astro-ph/0509812 , primaryClass =

    Pith/arXiv arXiv

  37. [37]

    , keywords =

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

    Pith/arXiv arXiv

  38. [38]

    The Galaxy in your preferred colours: Synthetic photometry from Gaia low-resolution spectra

    Gaia Data Release 3. The Galaxy in your preferred colours: Synthetic photometry from Gaia low-resolution spectra. , keywords =. doi:10.1051/0004-6361/202243709 , archivePrefix =. 2206.06215 , primaryClass =

    Pith/arXiv arXiv

  39. [39]

    , keywords =

    Gaia FGK benchmark stars: Effective temperatures and surface gravities. , keywords =. doi:10.1051/0004-6361/201526319 , archivePrefix =. 1506.06095 , primaryClass =

    Pith/arXiv arXiv

  40. [40]

    SF2A-2023: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics , year = 2023, month = dec, pages =

    The third version of the Gaia FGK Benchmark Stars. SF2A-2023: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics , year = 2023, month = dec, pages =

    2023

  41. [41]

    , keywords =

    A new implementation of the infrared flux method using the 2MASS catalogue. , keywords =. doi:10.1051/0004-6361/200810904 , archivePrefix =. 0901.3034 , primaryClass =

    Pith/arXiv arXiv

  42. [42]

    , keywords =

    The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Spectrographs. , keywords =. doi:10.1088/1538-3873/ab0075 , archivePrefix =. 1902.00928 , primaryClass =

    Pith/arXiv arXiv 1902

  43. [43]

    telescope and of the Ir \'e n \'e e DuPont telescope at Las Campanas Observatory, Chile

    The optical design of the 40-in. telescope and of the Ir \'e n \'e e DuPont telescope at Las Campanas Observatory, Chile. , year = 1973, month = jan, volume =. doi:10.1364/AO.12.001430 , adsurl =

    doi:10.1364/ao.12.001430 1973

  44. [44]

    , keywords =

    The 2.5 m Telescope of the Sloan Digital Sky Survey. , keywords =. doi:10.1086/500975 , archivePrefix =. astro-ph/0602326 , primaryClass =

    Pith/arXiv arXiv

  45. [45]

    , 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 =

    Pith/arXiv arXiv

  46. [46]

    Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis , year = 2005, editor =

    The Solar Chemical Composition. Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis , year = 2005, editor =

    2005

  47. [47]

    A grid of MARCS model atmospheres for late-type stars. I. Methods and general properties. , keywords =. doi:10.1051/0004-6361:200809724 , archivePrefix =. 0805.0554 , primaryClass =

    Pith/arXiv arXiv

  48. [48]

    , keywords =

    New ATLAS9 and MARCS Model Atmosphere Grids for the Apache Point Observatory Galactic Evolution Experiment (APOGEE). , keywords =. doi:10.1088/0004-6256/144/4/120 , archivePrefix =. 1208.1916 , primaryClass =

    Pith/arXiv arXiv 1916

  49. [49]

    , keywords =

    Model atmospheres for G, F, A, B, and O stars. , keywords =. doi:10.1086/190589 , adsurl =

    doi:10.1086/190589

  50. [50]

    , keywords =

    The GALAH+ survey: Third data release. , keywords =. doi:10.1093/mnras/stab1242 , archivePrefix =. 2011.02505 , primaryClass =

    Pith/arXiv arXiv 2011

  51. [51]

    , keywords =

    The Apache Point Observatory Galactic Evolution Experiment (APOGEE). , keywords =. doi:10.3847/1538-3881/aa784d , archivePrefix =. 1509.05420 , primaryClass =

    Pith/arXiv arXiv

  52. [52]

    , keywords =

    The Gaia-ESO Survey: Homogenisation of stellar parameters and elemental abundances. , keywords =. doi:10.1051/0004-6361/202345910 , archivePrefix =. 2304.07720 , primaryClass =

    Pith/arXiv arXiv

  53. [53]

    , keywords =

    The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar, and APOGEE-2 Data. , keywords =. doi:10.3847/1538-4365/ac4414 , archivePrefix =. 2112.02026 , primaryClass =

    arXiv

  54. [54]

    , keywords =

    Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe. , keywords =. doi:10.3847/1538-3881/aa7567 , archivePrefix =. 1703.00052 , primaryClass =

    Pith/arXiv arXiv