Pith. sign in

REVIEW 3 major objections 5 minor 85 references

NIR filter transformations across the HR diagram: JWST, Roman, and Euclid

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

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

Pith's one-line read New near-infrared color transformations put JWST, Euclid, Roman, HST, and ground-based photometry on one grid, with ~0.01 mag scatter for distance-scale stars and tip-of-the-red-giant-branch predictions that match JWST.

desk verdict Solid calibration paper; the transformations are the real deliverable and hold up, while the TRGB predictions are honestly labeled extrapolations that would benefit from a sensitivity refit and published coefficient uncertainties. read the letter →

arxiv 2506.13627 v2 pith:74IY4FX4 submitted 2025-06-16 astro-ph.IM

M. J. Durbin , R. L. Beaton , A. J. Monson , B. Swidler This is my paper · ORCID
classification astro-ph.IM
keywords calibrationinfraredastronomyphotometricsystemsstellarcolorspopulationsnear-infraredtipoftheredgiantbranchsyntheticphotometry
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper aims to give the community a single, consistent set of color transformations for converting near-infrared photometry among the major space and ground-based systems: JWST/NIRCam, Euclid/NISP, Roman/WFI, HST, and ground-based izY and JHKs. It derives these from synthetic photometry of over a thousand real stellar spectra spanning the full HR diagram, fitting continuous piecewise-linear relations for 105 unique filter combinations. For the stars most used in distance-scale astronomy—Cepheids, RR Lyrae variables, and red giants—the typical residual scatter is about 0.01 mag, while oxygen- and carbon-rich asymptotic-giant-branch stars scatter by up to 0.1 mag. The paper then applies the transformations to predict the tip of the red giant branch (TRGB) distance indicator in the JWST, Euclid, and Roman bands, and shows that the JWST predictions agree with an empirical calibration to within about 0.06 mag. This matters because Euclid and Roman will cover huge sky areas, and a common photometric grid lets their NIR measurements be compared directly with existing HST and ground-based data.

What carries the argument

The central object is the continuous piecewise-linear color transformation, fit with the pwlf package, which expresses the magnitude difference between two filters $Y$ as a sum of linear segments in a color $X$, with breakpoints chosen by Bayesian optimization; the output is a table of slopes and intercepts per segment for each filter pair. The engine behind it is synthetic photometry: each library spectrum is integrated against each filter's transmission curve, with fluxes and covariances propagated, and Vega zero-points set by the CALSPEC alpha Lyrae spectrum. The same machinery that converts any star's colors between systems is then applied to theoretical TRGB models to predict the tip's absolute magnitude as a function of color in the new filters.

What would settle it

Measure the tip of the red giant branch in the same nearby galaxies with both Roman/WFI and JWST/NIRCam once Roman data exist, or with Euclid/NISP in fields already observed by JWST, and check whether the predicted Roman F106-F158 and Euclid YE-HE tip relations reproduce the JWST-derived tip to within the claimed 0.01-0.05 mag; alternatively, recompute the transformations after adding upper-red-giant-branch spectra with $[\mathrm{Fe/H}]$ below $-2$ and above $-0.3$ from an independent library and see whether the piecewise-linear extrapolation shifts by more than the quoted scatter.

Watch

Extended reading notes

Core claim

Working with 1269 spectra of 1061 stars drawn from four spectral libraries, the authors fit continuous piecewise-linear transformations of the form $Y = c_0 + c_1(X - X_0) + \cdots$ between the near-infrared filters of JWST/NIRCam, Euclid/NISP, Roman/WFI, HST, and ground-based izY+IJHKs, producing coefficients for 105 unique filter combinations. The typical residual scatter is 0.01 mag for Cepheid, RR Lyrae, and RGB stars, and rises to around 0.1 mag for oxygen- and carbon-rich thermally-pulsing AGB stars. Using these transformations, the authors convert two recent theoretical TRGB calibrations into the Euclid, JWST, and Roman bandpasses, yielding color-magnitude relations for the tip of the red giant branch in each system. When the JWST F090W and F150W predictions are compared with a recent empirical calibration, the mean residuals are -0.06 and -0.05 mag over the common color range.

Load-bearing premise

The load-bearing premise is that the spectral libraries contain enough stars in the relevant regimes for the piecewise fits to be valid; they have almost no upper red-giant-branch stars and none at the extreme low or high metallicities where the tip-of-the-red-giant-branch color-magnitude relation is least certain, so the Euclid and Roman tip predictions rest on fits calibrated mostly on main-sequence, giant, and asymptotic-giant-branch stars.

Editorial extensions

If this is right

  • Photometry from JWST, Roman, Euclid, HST, and ground-based surveys can be shifted onto one grid with ~0.01 mag accuracy for Cepheids, RR Lyrae stars, and RGB stars, enabling direct apples-to-apples comparisons of distance-scale measurements.
  • TRGB distances measured with Roman and Euclid survey data can be calibrated directly with the published color-absolute-magnitude relations, without waiting for new empirical anchors.
  • The near-equivalent filter pairs (F090W and z, F106 and YE, F115W and F110W, F150W/F158/F160W, F200W/F213/KS) can be treated as interchangeable at the ~0.1 mag level in planning cross-mission observations.
  • The larger scatter for O- and C-rich AGB stars (up to 0.1 mag) implies that cross-calibrating AGB photometry between these systems needs more careful, type-specific treatment rather than relying on the global color terms.
  • Future revisions of the fits, as JWST, Euclid, and Roman calibrations mature, will directly propagate into the predicted TRGB zero points, so the published relations are tied to the current calibration state of each instrument.

Reading between the lines

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

  • One consequence the authors leave implicit is that the Roman and Euclid TRGB relations can be tested before those surveys deliver: compare the transformed JWST relations against TRGB measurements in galaxies with geometric distances, to separate a filter-transformation offset from a TRGB calibration offset.
  • The sparse upper-RGB coverage implies the ~0.01 mag scatter is a property of the fitted stars, not of the extrapolated TRGB regimes; a dedicated library of upper-RGB spectra at metallicities below -2 and above -0.3 in [Fe/H] would directly test whether the extrapolation holds.
  • Because the machinery is filter-agnostic, the same coefficient-generation workflow could be applied to any bandpass set with known transmission curves, allowing the tables to be extended as new filter systems are defined.
  • The piecewise breakpoints track known opacity features (the Paschen jump at 0.82 µm and the 1.65 µm H- continuum turnover), so the coefficient tables also serve as a map of where different stellar atmospheres drive the largest cross-instrument corrections.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper constructs empirical color transformations between near-infrared broadband filters on JWST/NIRCam, Euclid/NISP, Roman/WFI, HST, and ground-based DECam/OGLE-IV/2MASS systems, using synthetic photometry from CALSPEC, IRTF/EIRTF, and XSL spectral libraries. The authors fit continuous piecewise linear transformations for 105 filter combinations, report coefficients, segment boundaries, per-segment residual RMS, and stellar counts, and apply the transformations to theoretical TRGB models to predict TRGB absolute magnitudes and color-magnitude relations in JWST, Roman, and Euclid bands. The JWST predictions are compared with the empirical Newman et al. (2024a) calibration, with mean residuals of -0.06 and -0.05 mag in F090W and F150W over the overlapping metallicity range.

Significance. If the transformations hold up, this is a broadly useful calibration product for the distance-scale and stellar-population communities, and the TRGB predictions provide a concrete bridge between theoretical models and upcoming JWST/Roman/Euclid observations. The paper is careful in several respects: it tabulates Vega/AB/ST/Sirius-Vega conversions for all filters, reports residual scatter by stellar type, compares its Euclid transformation with an existing Euclid Collaboration transformation, and explicitly acknowledges library coverage gaps. The method is a well-defined extension of the authors' earlier published work, and the self-citation is not circular because the underlying method was published independently. The main limitations are the absence of uncertainties on the fitted coefficients and the extrapolated nature of the TRGB predictions at extreme metallicities and for Roman/Euclid, which currently have no empirical validation.

major comments (3)
  1. [§2.2 and §3.1, Tables 2–4] The fitted coefficients c0, c1 and segment breakpoints X0, X1 in Tables 2–4 are reported without uncertainties. Because the TRGB predictions in Table 5 and the color-magnitude relations in Table 6 are obtained by applying these coefficients to theoretical models, the precision of the central TRGB product is unquantified. Please provide coefficient uncertainties, for example via bootstrap resampling over the spectra or via covariance propagation from the piecewise least-squares fit, and propagate them to Tables 5 and 6, or state explicitly that the tabulated TRGB values are point estimates with no formal uncertainty.
  2. [§3.2, Figure 3, Tables 5–6] The empirical check against Newman et al. (2024a) covers only the intermediate metallicity range -1.9 ≤ [Fe/H] ≤ -0.7, while Table 5 extends from [Fe/H] = -3.2 to +0.06 and Table 6 spans large color ranges. Section 4 acknowledges that the spectral libraries contain few upper RGB stars and no extreme-metallicity stars, so the reported JWST residuals of -0.06 and -0.05 mag do not constrain behavior at the metal-poor and metal-rich ends, and Roman and Euclid have no independent empirical check at all. The skeptical concern therefore lands: the TRGB predictions in Tables 5 and 6 are extrapolations in precisely the regimes where the theoretical TRGB slope is least certain. Please add a sensitivity test, for example refitting the transformations using only stars in the TRGB-relevant stellar-parameter range and recomputing the predictions, or at minimum quantify the library coverage in the color-metallicity cells used by Tables 5 and 6 and explicitly mark extrapolated entries.
  3. [Abstract and §3.1] The abstract's 'typical residual dispersion around these transformations of 0.01 mag for Cepheid and RR Lyrae variables and RGB stars' is the in-sample RMS scatter about the fitted piecewise lines (σfit in Tables 2–4). It is not an estimate of the prediction uncertainty for the TRGB magnitudes in Tables 5 and 6, which additionally includes extrapolation error and spectral-library coverage effects. The text should state this distinction explicitly so that readers do not carry the 0.01 mag in-sample value over as the precision of the TRGB predictions.
minor comments (5)
  1. [§3.1] The phrase 'regularization parameterl' appears to contain a typo; it should read 'regularization parameter λ'.
  2. [§3.1] The value of the regularization parameter λ is described as 'the minimum uncertainty on Y', but the reader cannot reproduce the analysis without knowing the per-star total uncertainties; please define the quantity explicitly.
  3. [§2.2] The manuscript states that individual output magnitudes and uncertainties are available upon request; for reproducibility, consider depositing the synthetic photometry and fitting code in a permanent archive.
  4. [Figure 4] The residual distribution figure would be clearer with sample sizes and either error bars or percentile labels for each stellar type, so that the reader can judge the statistical weight of the 0.01 mag and 0.1 mag dispersions.
  5. [Table 6] The quadratic terms with large coefficients (25.78 and 44.95) look surprising; a brief note explaining the curvature, or showing the underlying points, would help readers trust the extrapolation.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: transformations are empirical fits applied to independent theoretical TRGB models, with external empirical validation.

full rationale

The paper's central products are piecewise-linear color transformations fit from synthetic photometry of four independent spectral libraries (CALSPEC, IRTF/EIRTF, XSL). These fits are not derived from the TRGB predictions: the TRGB absolute magnitudes in Tables 5 and 6 are produced by applying the fitted transformations to independent theoretical TRGB models (Pietrinferni et al. 2021; Serenelli et al. 2017), and the JWST comparison in Figure 3 is against the external empirical calibration of Newman et al. (2024a), converted using Table 1 zeropoints. No equation defines the transformation coefficients in terms of the predicted TRGB magnitudes, and no fitted TRGB quantity is fed back into the fits. The self-citation to Durbin et al. (2023) imports a previously published and reproducible methodology (synthetic photometry, global rejection criteria, piecewise-linear fitting) rather than a result whose validity depends on the present paper; it is therefore not load-bearing circularity. The paper explicitly acknowledges, in Section 4 and Figure 4, that the libraries contain few upper RGB stars and none at extreme low or high metallicities, and that Roman and Euclid lack direct empirical checks; this is an extrapolation caveat, not a circularity. The abstract's 0.01 mag dispersion is an in-sample scatter about the fitted lines, which is correctly described as residual dispersion, not as a validated prediction. Accordingly, no specific circular reduction can be exhibited, and the appropriate score is 0.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

This is a calibration paper: the fit coefficients are the product, not assumptions. The central claim rests mainly on the representativeness of spectral libraries and filter curves, plus the model assumptions for TRGB predictions. No new physical entities are introduced.

free parameters (3)
  • piecewise segment breaks and counts per filter pair = 1 to 4 segments (49 two-segment, 28 three-segment, 17 one-segment, 11 four-segment)
    Chosen by Bayesian optimization (GPyOpt) rather than derived from stellar physics; the number and location of breakpoints directly set the transformation coefficients.
  • uncertainty cut for inclusion (0.05 mag total in three filters) = 0.05 mag
    Applied as an additional rejection criterion in Section 3.1; it changes the sample from 856 to 605 to 815 spectra per combination and affects fitted slopes.
  • minimum segment span and occupancy = 0.1 mag span, 25 stars per segment
    Constraints imposed in Section 3.1 to regularize the Bayesian optimization; they trade bias against noise in the fit.
assumptions (5)
  • domain assumption Synthetic photometry via bandpass-weighted mean flux (Eq. 1) accurately represents observed magnitudes
    Used throughout Section 2.2 to compute integrated fluxes; assumes filter curves and spectra are on consistent, accurate wavelength and flux scales.
  • domain assumption Adopted filter throughput curves for Roman/WFI and Euclid/NISP are representative of the instruments
    The authors use CRDS, JWST docs, Euclid MRD and Roman curves, but note AOI variations and chip-to-chip differences are not modeled (Section 2.1).
  • domain assumption Line-of-sight reddening corrections from Lallement et al. 2022 and Skowron et al. 2021 are correct for all library stars
    Used to deredden spectra (Section 2.1); incorrect reddening biases colors and thus transformation slopes.
  • domain assumption Theoretical TRGB models (Serenelli et al. 2017 and Pietrinferni et al. 2021) provide accurate intrinsic TRGB magnitudes and colors
    The TRGB predictions in Table 6 inherit any inaccuracy in these models; only the JWST bands are checked against an empirical calibration.
  • ad hoc to paper Piecewise linear functions in a single color adequately capture filter-to-filter transformations across the HR diagram
    Adopted as the fitting family in Section 3.1; the good but not perfect residuals, up to 0.1 mag for AGB stars, show this is only approximate for some stellar types.

how reviews work

0 comments
Cite this review

Pith. "Pith review of NIR filter transformations across the HR diagram: JWST, Roman, and Euclid." pith.science (2026). https://pith.science/paper/74IY4FX4

@misc{pith2026250613627,
  author       = {Pith},
  title        = {Pith review of: NIR filter transformations across the HR diagram: JWST, Roman, and Euclid},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/74IY4FX4}},
  note         = {Machine review of arXiv:2506.13627}
}
abstract

We present new color transformations between select near-infrared filters on JWST/NIRCam, Euclid/NISP, Roman/WFI, HST, and ground-based $izY+IJHK_S$, for a total of 105 unique filter combinations. Additionally, we apply these transformations to predict the color-magnitude relation of the tip of the red giant branch as seen with JWST, Euclid, and Roman based on theoretical results for HST and 2MASS filters; for JWST we find good agreement with empirical results in the literature. We also find typical residual dispersion around these transformations of 0.01 mag for Cepheid and RR Lyrae variables and RGB stars, but up to 0.1 mag for O- and C-rich TP-AGB stars.

Figures

Figures reproduced from arXiv: 2506.13627 by the authors.

Figure 1
Figure 1. Throughput curves for all filters considered in this work. 2.1. Data We combine data products from four spectral libraries to maximize coverage of the full HR diagram at the rel￾evant wavelengths. These are the HST flux standard library CALSPEC (D. A. Turnshek et al. 1990; R. C. Bohlin et al. 2001; R. C. Bohlin 2007; R. C. Bohlin & M. Cohen 2008; R. C. Bohlin et al. 2014; R. C. Bohlin & S. E. Deustua 2019, and refer… view at source ↗
Figure 2
Figure 2. Euclid/NISP YE, JE, and HE TRGB magnitudes as a function of YE − HE color for the A. Serenelli et al. (2017) and A. Pietrinferni et al. (2021) theoretical TRGB calibrations. fective as a distance indicator (R. L. Beaton et al. 2018, 2019). We choose two recent theoretical calibrations of the TRGB to translate to Euclid, JWST, and Roman bands. While a plethora of empirical calibrations in −6.5 −6.0 −5.5 −5.0 −4.5 −4.… view at source ↗
Figure 4
Figure 4. Distributions of average transformation residuals (transformation-predicted magnitudes – spectra-synthesized magnitudes) for Cepheids, RR Lyrae, RGB stars, and O- and C-rich AGB stars. A similar study of filter transforms for integrated light, such as with the XSL simple stellar population models (K. Verro et al. 2022b), would be of interest as well for unresolved populations. ACKNOWLEDGMENTS Support for this work w… view at source ↗
Figures from the paper (10 more)
Figure 5
Figure 5. Figure 5: Filter transformations (black lines) for converting HST filters to JWST, with scatter as grey bands, and original data points and errors as blue points and ellipses [PITH_FULL_IMAGE:figures/full_fig_p016_5.png]
Figure 6
Figure 6. Figure 6: As [PITH_FULL_IMAGE:figures/full_fig_p017_6.png]
Figure 7
Figure 7. Figure 7: As [PITH_FULL_IMAGE:figures/full_fig_p018_7.png]
Figure 8
Figure 8. Figure 8: As [PITH_FULL_IMAGE:figures/full_fig_p019_8.png]
Figure 9
Figure 9. Figure 9: As [PITH_FULL_IMAGE:figures/full_fig_p020_9.png]
Figure 10
Figure 10. Figure 10: As [PITH_FULL_IMAGE:figures/full_fig_p021_10.png]
Figure 11
Figure 11. Figure 11: As [PITH_FULL_IMAGE:figures/full_fig_p022_11.png]
Figure 12
Figure 12. Figure 12: As [PITH_FULL_IMAGE:figures/full_fig_p023_12.png]
Figure 13
Figure 13. Figure 13: As [PITH_FULL_IMAGE:figures/full_fig_p024_13.png]
Figure 14
Figure 14. Figure 14: As [PITH_FULL_IMAGE:figures/full_fig_p025_14.png]

Review history (2 revisions) →

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

85 extracted references · 17 canonical work pages

  1. [1]

    Abbott , T. M. C., Abdalla , F. B., Allam , S., et al. 2018, title The Dark Energy Survey: Data Release 1 , , 239, 18, 10.3847/1538-4365/aae9f0

    doi:10.3847/1538-4365/aae9f0 2018

  2. [2]

    Abbott , T. M. C., Adam \'o w , M., Aguena , M., et al. 2021, title The Dark Energy Survey Data Release 2 , , 255, 20, 10.3847/1538-4365/ac00b3

    doi:10.3847/1538-4365/ac00b3 2021

  3. [3]

    2019, title The Wide Field Infrared Survey Telescope: 100 Hubbles for the 2020s , arXiv e-prints, arXiv:1902.05569

    Akeson , R., Armus , L., Bachelet , E., et al. 2019, title The Wide Field Infrared Survey Telescope: 100 Hubbles for the 2020s , arXiv e-prints, arXiv:1902.05569. 1902.05569

    arXiv 2019

  4. [4]

    2023, title The Shapes of Stellar Spectra , Atoms, 11, 61, 10.3390/atoms11030061

    Allende Prieto , C. 2023, title The Shapes of Stellar Spectra , Atoms, 11, 61, 10.3390/atoms11030061

    doi:10.3390/atoms11030061 2023

  5. [5]

    S., Riess , A

    Anand , G. S., Riess , A. G., Yuan , W., et al. 2024, title Tip of the Red Giant Branch Distances with JWST: An Absolute Calibration in NGC 4258 and First Applications to Type Ia Supernova Hosts , , 966, 89, 10.3847/1538-4357/ad2e0a

    doi:10.3847/1538-4357/ad2e0a 2024

  6. [6]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, title Astropy: A community Python package for astronomy , , 558, A33, 10.1051/0004-6361/201322068

    doi:10.1051/0004-6361/201322068 2013

  7. [7]

    M., Sip o cz , B

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, title The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package , , 156, 123, 10.3847/1538-3881/aabc4f

    doi:10.3847/1538-3881/aabc4f 2018

  8. [8]

    Bailer-Jones , C. A. L., Rybizki , J., Fouesneau , M., Demleitner , M., & Andrae , R. 2021, title Estimating Distances from Parallaxes. V. Geometric and Photogeometric Distances to 1.47 Billion Stars in Gaia Early Data Release 3 , , 161, 147, 10.3847/1538-3881/abd806

    doi:10.3847/1538-3881/abd806 2021

Show all 85 references
  1. [9]

    L., Bono , G., Braga , V

    Beaton , R. L., Bono , G., Braga , V. F., et al. 2018, title Old-Aged Primary Distance Indicators , , 214, 113, 10.1007/s11214-018-0542-1

    2018 doi

  2. [10]

    L., Seibert , M., Hatt , D., et al

    Beaton , R. L., Seibert , M., Hatt , D., et al. 2019, title The Carnegie-Chicago Hubble Program. VII. The Distance to M101 via the Optical Tip of the Red Giant Branch Method , , 885, 141, 10.3847/1538-4357/ab4263

    2019 doi

  3. [11]

    2021, in European Planetary Science Congress, EPSC2021--298, 10.5194/epsc2021-298

    Beaulieu , J.-P., & Bachelet , E. 2021, in European Planetary Science Congress, EPSC2021--298, 10.5194/epsc2021-298

    2021 doi

  4. [12]

    Bohlin , R. C. 2007, in Astronomical Society of the Pacific Conference Series, Vol. 364, The Future of Photometric, Spectrophotometric and Polarimetric Standardization, ed. C. Sterken , 315, 10.48550/arXiv.astro-ph/0608715

    2007 doi arXiv

  5. [13]

    C., & Cohen , M

    Bohlin , R. C., & Cohen , M. 2008, title NICMOS Spectrophotometry and Models for a Stars , , 136, 1171, 10.1088/0004-6256/136/3/1171

    2008 doi

  6. [14]

    C., & Deustua , S

    Bohlin , R. C., & Deustua , S. E. 2019, title CALSPEC: Wide Field Camera 3 Infrared Grism Spectrophotometry , , 157, 229, 10.3847/1538-3881/ab1b50

    2019 doi

  7. [15]

    C., Dickinson , M

    Bohlin , R. C., Dickinson , M. E., & Calzetti , D. 2001, title Spectrophotometric Standards from the Far-Ultraviolet to the Near-Infrared: STIS and NICMOS Fluxes , , 122, 2118, 10.1086/323137

    2001 doi

  8. [16]

    C., Gordon , K

    Bohlin , R. C., Gordon , K. D., & Tremblay , P. E. 2014, title Techniques and Review of Absolute Flux Calibration from the Ultraviolet to the Mid-Infrared , , 126, 711, 10.1086/677655

    2014 doi

  9. [17]

    C., M \'e sz \'a ros , S., Fleming , S

    Bohlin , R. C., M \'e sz \'a ros , S., Fleming , S. W., et al. 2017, title A New Stellar Atmosphere Grid and Comparisons with HST/STIS CALSPEC Flux Distributions , , 153, 234, 10.3847/1538-3881/aa6ba9

    2017 doi

  10. [18]

    L., Anderson , J., Gennaro , M., et al

    Boyer , M. L., Anderson , J., Gennaro , M., et al. 2022, title The JWST Resolved Stellar Populations Early Release Science Program. I. NIRCam Flux Calibration , Research Notes of the American Astronomical Society, 6, 191, 10.3847/2515-5172/ac923a

    2022 doi

  11. [19]

    Burgasser , A. J. 2014, in Astronomical Society of India Conference Series, Vol. 11, Astronomical Society of India Conference Series, 7--16, 10.48550/arXiv.1406.4887

    2014 doi arXiv

  12. [20]

    A., et al

    Carleton , T., Ellsworth-Bowers , T., Windhorst , R. A., et al. 2024, title PEARLS: A Potentially Isolated Quiescent Dwarf Galaxy with a Tip of the Red Giant Branch Distance of 30 Mpc , , 961, L37, 10.3847/2041-8213/ad1b56

    2024 doi

  13. [21]

    2020, title Joint Survey Processing of Euclid, Rubin and Roman: Final Report , arXiv e-prints, arXiv:2008.10663, 10.48550/arXiv.2008.10663

    Chary , R., Helou , G., Brammer , G., et al. 2020, title Joint Survey Processing of Euclid, Rubin and Roman: Final Report , arXiv e-prints, arXiv:2008.10663, 10.48550/arXiv.2008.10663

    2020 doi arXiv

  14. [22]

    C., Peletier , R

    Chen , Y.-P., Trager , S. C., Peletier , R. F., et al. 2014, title The X-shooter Spectral Library (XSL). I. DR1: Near-ultraviolet through optical spectra from the first year of the survey , , 565, A117, 10.1051/0004-6361/201322505

    2014 doi

  15. [23]

    J., Williams , B

    Dalcanton , J. J., Williams , B. F., Melbourne , J. L., et al. 2012, title Resolved Near-infrared Stellar Populations in Nearby Galaxies , , 198, 6, 10.1088/0067-0049/198/1/6

    2012 doi

  16. [24]

    E., & Mack , J

    Deustua , S. E., & Mack , J. 2018, title Comparing the ACS/WFC and WFC3/UVIS Calibration and Photometry , , Instrument Science Report WFC3 2018-02, 33 pages

    2018

  17. [25]

    J., Beaton , R

    Durbin , M. J., Beaton , R. L., Dalcanton , J. J., Williams , B. F., & Boyer , M. L. 2020, title MCR-TRGB: A Multiwavelength-covariant, Robust Tip of the Red Giant Branch Measurement Method , , 898, 57, 10.3847/1538-4357/ab9cbb

    2020 doi

  18. [26]

    J., Beaton , R

    Durbin , M. J., Beaton , R. L., Monson , A. J., Swidler , B., & Dalcanton , J. J. 2023, title Empirical 2MASS-WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry , , 166, 236, 10.3847/1538-3881/acfaa1

    2023 doi

  19. [27]

    2022, title astropy/specutils: V1.7.0, , v1.7.0 Zenodo, 10.5281/zenodo.6207491

    Earl, N., Tollerud, E., Jones, C., et al. 2022, title astropy/specutils: V1.7.0, , v1.7.0 Zenodo, 10.5281/zenodo.6207491

    2022 doi

  20. [28]

    2022, title Euclid preparation

    Euclid Collaboration , Schirmer , M., Jahnke , K., et al. 2022, title Euclid preparation. XVIII. The NISP photometric system , , 662, A92, 10.1051/0004-6361/202142897

    2022 doi

  21. [29]

    2024, title Euclid

    Euclid Collaboration et al. 2024, title Euclid. I. Overview of the Euclid mission , arXiv e-prints, arXiv:2405.13491, 10.48550/arXiv.2405.13491

    2024 doi

  22. [30]

    L., Madore , B

    Freedman , W. L., Madore , B. F., Hatt , D., et al. 2019, title The Carnegie-Chicago Hubble Program. VIII. An Independent Determination of the Hubble Constant Based on the Tip of the Red Giant Branch , , 882, 34, 10.3847/1538-4357/ab2f73

    2019 doi

  23. [31]

    2022, title Gaia Data Release 3: The Galaxy in your preferred colours

    Gaia Collaboration , Montegriffo , P., Bellazzini , M., et al. 2022, title Gaia Data Release 3: The Galaxy in your preferred colours. Synthetic photometry from Gaia low-resolution spectra , arXiv e-prints, arXiv:2206.06215, 10.48550/arXiv.2206.06215

    2022 doi arXiv

  24. [32]

    2017, title Astroquery: Access to online data resources , 1708.004

    Ginsburg , A., Parikh , M., Woillez , J., et al. 2017, title Astroquery: Access to online data resources , 1708.004

    2017

  25. [33]

    M., Brasseur , C

    Ginsburg , A., Sip o cz , B. M., Brasseur , C. E., et al. 2019, title astroquery: An Astronomical Web-querying Package in Python , , 157, 98, 10.3847/1538-3881/aafc33

    2019 doi

  26. [34]

    2020, title The X-shooter Spectral Library (XSL): Data release 2 , , 634, A133, 10.1051/0004-6361/201936825

    Gonneau , A., Lyubenova , M., Lan c on , A., et al. 2020, title The X-shooter Spectral Library (XSL): Data release 2 , , 634, A133, 10.1051/0004-6361/201936825

    2020 doi

  27. [35]

    2022, title dust\_extinction, , v1.1 GitHub

    Gordon, K., Larson, K., McBride, A., et al. 2022, title dust\_extinction, , v1.1 GitHub. https://github.com/karllark/dust_extinction/releases/tag/v1.1

    2022

  28. [36]

    2018, title The Araucaria Project: Multi-band Calibrations of the TRGB Absolute Magnitude , , 156, 278, 10.3847/1538-3881/aaeacb

    G \'o rski , M., Pietrzy \'n ski , G., Gieren , W., et al. 2018, title The Araucaria Project: Multi-band Calibrations of the TRGB Absolute Magnitude , , 156, 278, 10.3847/1538-3881/aaeacb

    2018 doi

  29. [37]

    2014, title PyVO: Python access to the Virtual Observatory , 1402.004

    Graham , M., Plante , R., Tody , D., & Fitzpatrick , M. 2014, title PyVO: Python access to the Virtual Observatory , 1402.004

    2014

  30. [38]

    2018, title dustmaps: A Python interface for maps of interstellar dust , The Journal of Open Source Software, 3, 695, 10.21105/joss.00695

    Green , G. 2018, title dustmaps: A Python interface for maps of interstellar dust , The Journal of Open Source Software, 3, 695, 10.21105/joss.00695

    2018 doi

  31. [39]

    Groenewegen , M. A. T., Cioni , M. R. L., Girardi , L., et al. 2019, title The VMC Survey. XXXIII. The tip of the red giant branch in the Magellanic Clouds , , 622, A63, 10.1051/0004-6361/201833904

    2019 doi

  32. [40]

    R., Millman , K

    Harris , C. R., Millman , K. J., van der Walt , S. J., et al. 2020, title Array programming with NumPy , , 585, 357, 10.1038/s41586-020-2649-2

    2020 doi

  33. [41]

    J., Freedman , W

    Hoyt , T. J., Freedman , W. L., Madore , B. F., et al. 2018, title The Near-infrared Tip of the Red Giant Branch. II. An Absolute Calibration in the Large Magellanic Cloud , , 858, 12, 10.3847/1538-4357/aab7ed

    2018 doi

  34. [42]

    Hunter , J. D. 2007, title Matplotlib: A 2D Graphics Environment , Computing in Science and Engineering, 9, 90, 10.1109/MCSE.2007.55

    2007 doi

  35. [43]

    F., & Venter, G

    Jekel, C. F., & Venter, G. 2019, pwlf: A Python Library for Fitting 1D Continuous Piecewise Linear Functions. https://github.com/cjekel/piecewise_linear_fit_py

    2019

  36. [44]

    John , T. L. 1988, title Continuous absorption by the negative hydrogen ion reconsidered , , 193, 189

    1988

  37. [45]

    L., Babusiaux , C., & Cox , N

    Lallement , R., Vergely , J. L., Babusiaux , C., & Cox , N. L. J. 2022, title Updated Gaia-2MASS 3D maps of Galactic interstellar dust , , 661, A147, 10.1051/0004-6361/202142846

    2022 doi

  38. [46]

    G., Freedman , W

    Lee , M. G., Freedman , W. L., & Madore , B. F. 1993, title The Tip of the Red Giant Branch as a Distance Indicator for Resolved Galaxies , , 417, 553, 10.1086/173334

    1993 doi

  39. [47]

    2024, title JWST's PEARLS: Improved Flux Calibration for NIRCam , , 136, 024501, 10.1088/1538-3873/ad1f3e

    Ma , Z., Yan , H., Sun , B., et al. 2024, title JWST's PEARLS: Improved Flux Calibration for NIRCam , , 136, 024501, 10.1088/1538-3873/ad1f3e

    2024 doi

  40. [48]

    2010, in Proceedings of the 9th Python in Science Conference , ed

    McKinney , W. 2010, in Proceedings of the 9th Python in Science Conference , ed. S. van der Walt & Jarrod Millman , Austin, TX , 56--61, 10.25080/Majora-92bf1922-00a

    2010 doi

  41. [49]

    2011, title Pandas: A Foundational Python Library for Data Analysis and Statistics, Python for High Performance and Scientific Computing, 14

    McKinney , W. 2011, title Pandas: A Foundational Python Library for Data Analysis and Statistics, Python for High Performance and Scientific Computing, 14. https://www.semanticscholar.org/paper/pandas

    2011

  42. [50]

    2024, title The updated BOSZ synthetic stellar spectral library , , 688, A197, 10.1051/0004-6361/202449306

    M \'e sz \'a ros , S., Bohlin , R., Allende Prieto , C., et al. 2024, title The updated BOSZ synthetic stellar spectral library , , 688, A197, 10.1051/0004-6361/202449306

    2024 doi

  43. [51]

    Newman , M. J. B., McQuinn , K. B. W., Skillman , E. D., et al. 2024 a , title An Empirical Calibration of the Tip of the Red Giant Branch Distance Method in the Near Infrared. II. JWST NIRCam Wide Filters , arXiv e-prints, arXiv:2406.03532, 10.48550/arXiv.2406.03532

    2024 doi arXiv

  44. [52]

    Newman , M. J. B., McQuinn , K. B. W., Skillman , E. D., et al. 2024 b , title An Empirical Calibration of the Tip of the Red Giant Branch Distance Method in the Near Infrared. I. Hubble Space Telescope WFC3/IR F110W and F160W Filters , , 966, 175, 10.3847/1538-4357/ad306d

    2024 doi

  45. [53]

    2000, title The VizieR database of astronomical catalogues , , 143, 23, 10.1051/aas:2000169

    Ochsenbein , F., Bauer , P., & Marcout , J. 2000, title The VizieR database of astronomical catalogues , , 143, 23, 10.1051/aas:2000169

    2000 doi

  46. [54]

    Oke , J. B. 1974, title Absolute Spectral Energy Distributions for White Dwarfs , , 27, 21, 10.1086/190287

    1974 doi

  47. [55]

    2021, title Updated BaSTI Stellar Evolution Models and Isochrones

    Pietrinferni , A., Hidalgo , S., Cassisi , S., et al. 2021, title Updated BaSTI Stellar Evolution Models and Isochrones. II. -enhanced Calculations , , 908, 102, 10.3847/1538-4357/abd4d5

    2021 doi

  48. [56]

    T., Cushing , M

    Rayner , J. T., Cushing , M. C., & Vacca , W. D. 2009, title The Infrared Telescope Facility (IRTF) Spectral Library: Cool Stars , , 185, 289, 10.1088/0067-0049/185/2/289

    2009 doi

  49. [57]

    H., Su , K., Sloan , G

    Rieke , G. H., Su , K., Sloan , G. C., & Schlawin , E. 2022, title Infrared Absolute Calibration. I. Comparison of Sirius with Fainter Calibration Stars , , 163, 45, 10.3847/1538-3881/ac3b5d

    2022 doi

  50. [58]

    2023, title The Science Performance of JWST as Characterized in Commissioning , , 135, 048001, 10.1088/1538-3873/acb293

    Rigby , J., & et al. 2023, title The Science Performance of JWST as Characterized in Commissioning , , 135, 048001, 10.1088/1538-3873/acb293

    2023 doi

  51. [59]

    R., Lightsey , P

    Rigby , J. R., Lightsey , P. A., Garc \' a Mar \' n , M., et al. 2023, title How Dark the Sky: The JWST Backgrounds , , 135, 048002, 10.1088/1538-3873/acbcf4

    2023 doi

  52. [60]

    M., Aldering , G., Dai , M., et al

    Rose , B. M., Aldering , G., Dai , M., et al. 2021, title Synergies between Vera C. Rubin Observatory, Nancy Grace Roman Space Telescope, and Euclid Mission: Constraining Dark Energy with Type Ia Supernovae , arXiv e-prints, arXiv:2104.01199, 10.48550/arXiv.2104.01199

    2021 doi arXiv

  53. [61]

    2006, Evolution of Stars and Stellar Populations , 1st edn

    Salaris , M., & Cassisi , S. 2006, Evolution of Stars and Stellar Populations , 1st edn. ( Wiley )

    2006

  54. [62]

    C., Best , W

    Sanghi , A., Liu , M. C., Best , W. M., et al. 2023, title Ultracool Dwarf Absolute Magnitude versus Spectral Type Relations for JWST NIRCam Filters , Research Notes of the American Astronomical Society, 7, 194, 10.3847/2515-5172/acf864

    2023 doi

  55. [63]

    C., Dupuy , T

    Sanghi , A., Liu , M. C., Dupuy , T. J., et al. 2024, title Ultracool Dwarf Absolute Magnitude Versus Spectral Type Relations for Euclid and Roman Near-infrared Filters , Research Notes of the American Astronomical Society, 8, 137, 10.3847/2515-5172/ad4cec

    2024 doi

  56. [64]

    2017, title The brightness of the red giant branch tip

    Serenelli , A., Weiss , A., Cassisi , S., Salaris , M., & Pietrinferni , A. 2017, title The brightness of the red giant branch tip. Theoretical framework, a set of reference models, and predicted observables , , 606, A33, 10.1051/0004-6361/201731004

    2017 doi

  57. [65]

    M., Skowron , J., Udalski , A., et al

    Skowron , D. M., Skowron , J., Udalski , A., et al. 2021, title OGLE-ing the Magellanic System: Optical Reddening Maps of the Large and Small Magellanic Clouds from Red Clump Stars , , 252, 23, 10.3847/1538-4365/abcb81

    2021 doi

  58. [66]

    1998, title Synthetic Photometry Experiments in the Vicinity of the Paschen Jump , Baltic Astronomy, 7, 571, 10.1515/astro-1998-0404

    Straizys , V. 1998, title Synthetic Photometry Experiments in the Vicinity of the Paschen Jump , Baltic Astronomy, 7, 571, 10.1515/astro-1998-0404

    1998 doi

  59. [67]

    2018, title synphot: Synthetic photometry using Astropy , 1811.001

    STScI Development Team . 2018, title synphot: Synthetic photometry using Astropy , 1811.001

    2018

  60. [68]

    2020, title stsynphot: synphot for HST and JWST , 2010.003

    STScI Development Team . 2020, title stsynphot: synphot for HST and JWST , 2010.003

    2020

  61. [69]

    Taylor , B. J. 1986, title Transformation Equations and Other Aids for VRI Photometry , , 60, 577, 10.1086/191098

    1986 doi

  62. [70]

    2016, title GPyOpt: A Bayesian Optimization framework in Python, , http://github.com/SheffieldML/GPyOpt

    The GPyOpt authors . 2016, title GPyOpt: A Bayesian Optimization framework in Python, , http://github.com/SheffieldML/GPyOpt

    2016

  63. [71]

    A., Bohlin , R

    Turnshek , D. A., Bohlin , R. C., Williamson , R. L., I., et al. 1990, title An Atlas of Hubble Space Telescope Photometric, Spectrophotometric, and Polarimetric Calibration Objects , , 99, 1243, 10.1086/115413

    1990 doi

  64. [72]

    K., & Szyma \'n ski , G

    Udalski , A., Szyma \'n ski , M. K., & Szyma \'n ski , G. 2015, title OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment , , 65, 1, 10.48550/arXiv.1504.05966

    2015 doi arXiv

  65. [73]

    R., & Origlia , L

    Valenti , E., Ferraro , F. R., & Origlia , L. 2004, title Red giant branch in near-infrared colour-magnitude diagrams - II. The luminosity of the bump and the tip , , 354, 815, 10.1111/j.1365-2966.2004.08249.x

    2004

  66. [74]

    C., & Varoquaux, G

    van der Walt , S., Colbert, S. C., & Varoquaux, G. 2011, title The NumPy Array : A Structure for Efficient Numerical Computation , Computing in Science & Engineering, 13, 22, 10.1109/MCSE.2011.37

    2011 doi

  67. [75]

    L., Lallement , R., & Cox , N

    Vergely , J. L., Lallement , R., & Cox , N. L. J. 2022, title Three-dimensional extinction maps: Inverting inter-calibrated extinction catalogues , , 664, A174, 10.1051/0004-6361/202243319

    2022 doi

  68. [76]

    C., Peletier , R

    Verro , K., Trager , S. C., Peletier , R. F., et al. 2022 a , title The X-shooter Spectral Library (XSL): Data Release 3 , , 660, A34, 10.1051/0004-6361/202142388

    2022 doi

  69. [77]

    C., Peletier , R

    Verro , K., Trager , S. C., Peletier , R. F., et al. 2022 b , title Modelling simple stellar populations in the near-ultraviolet to near-infrared with the X-shooter Spectral Library (XSL) , , 661, A50, 10.1051/0004-6361/202142387

    2022 doi

  70. [78]

    2017, title The Extended IRTF Spectral Library: Expanded Coverage in Metallicity, Temperature, and Surface Gravity , , 230, 23, 10.3847/1538-4365/aa72ed

    Villaume , A., Conroy , C., Johnson , B., et al. 2017, title The Extended IRTF Spectral Library: Expanded Coverage in Metallicity, Temperature, and Surface Gravity , , 230, 23, 10.3847/1538-4365/aa72ed

    2017 doi

  71. [79]

    E., et al

    Virtanen , P., Gommers , R., Oliphant , T. E., et al. 2020, title SciPy 1.0: fundamental algorithms for scientific computing in Python , Nature Methods, 17, 261, 10.1038/s41592-019-0686-2

    2020 doi

  72. [80]

    2021, title seaborn: statistical data visualization , The Journal of Open Source Software, 6, 3021, 10.21105/joss.03021

    Waskom , M. 2021, title seaborn: statistical data visualization , The Journal of Open Source Software, 6, 3021, 10.21105/joss.03021

    2021 doi

  73. [81]

    2000, title The SIMBAD astronomical database

    Wenger , M., Ochsenbein , F., Egret , D., et al. 2000, title The SIMBAD astronomical database. The CDS reference database for astronomical objects , , 143, 9, 10.1051/aas:2000332

    2000 doi

  74. [82]

    B., Rizzi , L., et al

    Wu , P.-F., Tully , R. B., Rizzi , L., et al. 2014, title Infrared Tip of the Red Giant Branch and Distances to the Maffei/IC 342 Group , , 148, 7, 10.1088/0004-6256/148/1/7

    2014 doi

  75. [83]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.stat...

  76. [84]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.d...

  77. [85]

    E e'UXb8r9;Wf^̙ 4=8( _zde @ 3> z 6o]Fr: ru X ?xi+c g R!8! 8 zԋ^?mp Ef<W + [ZB_ ]v81 4ؼN R Vk =`jwMS y x8<X= - 7 䱊 c/ 49

    thebibliography [1] 20pt to REFERENCES 6pt =0pt \@twocolumntrue 12pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty...

    2017

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.