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arxiv: 2606.11587 · v1 · pith:EEAG6RJ2new · submitted 2026-06-10 · 🌌 astro-ph.IM · astro-ph.GA· astro-ph.SR

Recalibration of SDSS photometric zero-points based on the InfraRed Flux Method temperature scale

Zenghua Zhou , Luca Casagrande , Heran Xiong , Yanjun Guo , Jiajia Li , Zhanwen Han , Xuefei Chen This is my paper

Pith reviewed 2026-06-27 08:42 UTC · model grok-4.3

classification 🌌 astro-ph.IM astro-ph.GAastro-ph.SR
keywords SDSS photometryzero-point calibrationInfrared Flux Methodeffective temperatureFGK starsphotometric offsetsu-band red leakAB magnitude system
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The pith

Inverting the Infrared Flux Method on 6000 FGK stars reveals that SDSS u-band photometry needs a color-dependent zero-point offset while the r band is already on the nominal AB scale.

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

The paper establishes that photometric zero-points for the SDSS ugriz system can be recalibrated by using known effective temperatures of stars as an anchor and solving for the magnitude offsets that make the Infrared Flux Method reproduce those temperatures. A sympathetic reader would care because zero-point errors directly affect the conversion of observed magnitudes into physical fluxes, which matters for comparing observations to models and for combining data across different surveys. The method exploits the fact that the IRFM is sensitive to the absolute flux level in the optical bands. The largest effect appears in the u band and depends on whether the filter transmission includes a red leak. The work shows that samples of thousands of stars can serve as a practical calibration tool complementary to traditional spectrophotometric standards.

Core claim

Using benchmark effective temperatures for more than 6000 FGK-type stars, the authors invert the Infrared Flux Method to solve for the zero-point corrections that SDSS ugriz photometry must receive to recover the adopted temperature scale. The r band requires essentially no correction. The i and z bands show offsets of a few hundredths of a magnitude. A small offset appears in g. The u band exhibits the largest discrepancy, and the size of the correction changes markedly according to whether the original filter transmission curves or updated curves that include a red leak are adopted; the latter produces a color-dependent offset visible in late-type stars. Independent checks against CALSPEC

What carries the argument

Inversion of the Infrared Flux Method (IRFM) using benchmark effective temperatures to solve for SDSS ugriz zero-point corrections.

If this is right

  • The r-band zero-point can be treated as already correct for most applications.
  • i- and z-band magnitudes require adjustments of order 0.02-0.05 mag to align with the IRFM temperature scale.
  • u-band photometry carries a color-dependent systematic that is traceable to the choice of filter transmission curve.
  • Revised zero-points anchored to the IRFM scale can be applied directly to existing SDSS catalogs.
  • Large stellar samples offer a viable route to calibrate future wide-field surveys without relying solely on a small number of spectrophotometric standards.

Where Pith is reading between the lines

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

  • The same inversion technique could be tested on photometry from other surveys that overlap the SDSS footprint to check for consistent offsets.
  • If the u-band red-leak correction proves necessary, it may affect derived metallicities or temperatures for cool stars in any catalog that uses the original SDSS u transmission curves.
  • The method supplies an independent cross-check on Gaia XP spectra, which could be used to extend the calibration to fainter magnitudes.
  • Applying the recalibration to color-color diagrams of FGK stars should tighten the locus and reduce scatter in temperature-sensitive indices.

Load-bearing premise

The benchmark effective temperatures for the 6000 stars were determined independently of the SDSS ugriz photometry being recalibrated.

What would settle it

If new, fully independent effective-temperature determinations for the same stars (for example from high-resolution spectroscopy or interferometry) produce a different set of required zero-point offsets when fed into the same IRFM inversion, the derived SDSS corrections would be falsified.

Figures

Figures reproduced from arXiv: 2606.11587 by Heran Xiong, Jiajia Li, Luca Casagrande, Xuefei Chen, Yanjun Guo, Zenghua Zhou, Zhanwen Han.

Figure 1
Figure 1. Figure 1: Total system throughput of the SDSS ugriz photometric filters. Left: The original transmission curves from Fukugita et al. (1996, red dashed lines) and the updated curves from Doi et al. (2010, blue solid lines). Right: Red-leak contribution in the u-band reported in Doi et al. (2010), il￾lustrating residual sensitivity at λ > 760 nm. magnitude mζ,AB = −2.5 log R λf λi λ fλTζ dλ f 0 ν c R λf λi Tζ λ dλ , (… view at source ↗
Figure 2
Figure 2. Figure 2: Distribution of stellar parameters for our GALAH and APOGEE samples [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Left panel: ∆Teff = T ref eff − Teff,u(ϵu = 0) for stars in the GALAH (blue) and APOGEE (red) samples. Continuous lines show the best fits for the GALAH (blue), APOGEE (red) and combined (green) samples. Right panels: ∆χ 2 = χ 2 − χ 2 min curves, whereby values of 1, 2 and 3 define sigma confidence levels. Colours refer to the same samples shown in the left panel. The gray line corresponds to the combined … view at source ↗
Figure 4
Figure 4. Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 6
Figure 6. Figure 6 [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 5
Figure 5. Figure 5: Crosses show the difference between AB magnitudes computed from CALSPEC fluxes and observed SDSS magnitudes, ϵζ = mζ,AB − mζ,S DS S , as a function of observed g − r colour (green). Error bars are obtained by adding in quadrature the observational and CALSPEC uncer￾tainties. Dashed and dotted lines indicate the median and mean offsets, re￾spectively, reported in each panel together with their associated st… view at source ↗
read the original abstract

Accurate photometric zero-points are essential for translating observed magnitudes into physical fluxes, from comparing with models to ensuring consistency across surveys. We determine the zero-points needed to place the Sloan Digital Sky Survey (SDSS) $ugriz$ system on its nominal AB definition, by exploiting the sensitivity of the Infrared Flux Method (IRFM) to broadband flux calibration. Using benchmark effective temperatures for over 6,000 FGK-type stars, we invert the method to identify the zero-point corrections required for SDSS photometry to reproduce the adopted temperature scale. The $r$ band is found to be very well standardized, while the $i$ and $z$ bands show offsets of a few hundredths of a magnitude, consistent with previous studies. We also find a small offset in the $g$ band. The largest discrepancy occurs in the $u$ band, where the derived offset depends strongly on the adopted filter transmission curves, in particular whether one uses the original definition commonly adopted in the literature or the updated measurements that account for the presence of a red leak. This effect introduces a colour-dependent zero-point offset that becomes apparent when using a sample of late-type stars. Independent comparisons with CALSPEC spectrophotometric standards and Gaia XP spectra broadly support the offsets derived from the IRFM analysis. Our results provide a revised set of SDSS zero-points anchored to the IRFM temperature scale and demonstrate that large stellar samples can be used to constrain photometric calibration. The methodology presented here offers a complementary approach to traditional spectrophotometric calibration and may prove useful for future large-scale surveys.

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 / 0 minor

Summary. The manuscript claims to recalibrate SDSS ugriz zero-points by inverting the Infrared Flux Method (IRFM) on benchmark effective temperatures for over 6,000 FGK-type stars. It reports the r band as well standardized, small offsets in g/i/z, and a larger u-band offset that depends strongly on the choice of filter transmission curves (original vs. updated with red leak). Independent checks with CALSPEC standards and Gaia XP spectra are said to support the derived offsets.

Significance. If the benchmark Teff values are fully independent of SDSS photometry, the work supplies a useful large-sample, IRFM-anchored complement to spectrophotometric calibration. The reported consistency with CALSPEC and Gaia XP adds external support, and the approach may be applicable to future surveys.

major comments (1)
  1. [Benchmark sample description (abstract and methods)] The inversion's validity rests on the benchmark Teff being determined entirely independently of SDSS ugriz photometry or any correlated system. The abstract asserts the temperatures are 'benchmark' but supplies no explicit cross-check, provenance table, or discussion of the input catalogue's construction; this is load-bearing for all reported offsets and requires a dedicated verification section or appendix.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their review and for highlighting the importance of clearly establishing the independence of the benchmark temperatures. We address the single major comment below.

read point-by-point responses

  1. Referee: [Benchmark sample description (abstract and methods)] The inversion's validity rests on the benchmark Teff being determined entirely independently of SDSS ugriz photometry or any correlated system. The abstract asserts the temperatures are 'benchmark' but supplies no explicit cross-check, provenance table, or discussion of the input catalogue's construction; this is load-bearing for all reported offsets and requires a dedicated verification section or appendix.

    Authors: We agree that the current manuscript does not provide sufficient detail on the provenance and independence of the benchmark Teff values. The temperatures are taken from an external compilation based on high-resolution spectroscopy and other non-photometric methods that predate and do not incorporate SDSS ugriz data. In the revised manuscript we will add a dedicated subsection (and supporting appendix table) that (i) cites the original catalogue sources, (ii) summarises the construction and selection criteria, and (iii) explicitly verifies that no SDSS photometry entered the Teff determinations. This addition will make the independence of the temperature scale transparent and address the referee's concern directly. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation anchored to external benchmarks and cross-validated

full rationale

The paper inverts the IRFM using benchmark Teff values for >6000 stars (presented as an adopted external temperature scale) to solve for SDSS ugriz zero-point offsets needed to recover those Teff. It then reports consistency with independent CALSPEC spectrophotometric standards and Gaia XP spectra. No equations or steps reduce the derived offsets to the input photometry by construction, no fitted parameters are relabeled as predictions, and no load-bearing self-citation chain is invoked to justify the central result. The methodology is self-contained against external benchmarks, satisfying the default expectation of no circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the accuracy and independence of the benchmark temperatures and on the assumption that the IRFM can be inverted without introducing systematics from filter definitions or stellar parameters.

axioms (1)
  • domain assumption Benchmark effective temperatures for the 6000 FGK stars are accurate and independent of SDSS photometry
    The inversion procedure is designed to reproduce these temperatures, so any error or shared systematic in the benchmarks directly affects the derived zero-points.

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discussion (0)

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Works this paper leans on

70 extracted references · 62 canonical work pages · 28 internal anchors

  1. [1]

    The u'g'r'i'z' Standard Star Network

    The u'g'r'i'z' Standard-Star System. , keywords =. doi:10.1086/339311 , archivePrefix =. astro-ph/0201143 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/339311

  2. [2]

    Preliminary flux tables for the calibration of Gaia DR2 and (E)DR3

    The Gaia spectrophotometric standard stars survey - V. Preliminary flux tables for the calibration of Gaia DR2 and (E)DR3. , keywords =. doi:10.1093/mnras/stab766 , archivePrefix =. 2103.07154 , primaryClass =

    work page doi:10.1093/mnras/stab766

  3. [3]

    , author =

    M dwarfs: effective temperatures, radii and metallicities. , keywords =. doi:10.1111/j.1365-2966.2008.13573.x , archivePrefix =. 0806.2471 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.13573.x 2008

  4. [4]

    Astrometry and Photometry for Cool Dwarfs and Brown Dwarfs

    Astrometry and Photometry for Cool Dwarfs and Brown Dwarfs. , keywords =. doi:10.1086/341646 , archivePrefix =. astro-ph/0205050 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/341646

  5. [5]

    Maps of Dust IR Emission for Use in Estimation of Reddening and CMBR Foregrounds

    Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds. , keywords =. doi:10.1086/305772 , archivePrefix =. astro-ph/9710327 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/305772

  6. [6]

    , 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 =

    work page doi:10.3847/1538-4365/ac4414

  7. [7]

    , keywords =

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

    work page doi:10.1093/mnras/stab1242 2011

  8. [8]

    The Second Data Release of the Sloan Digital Sky Survey

    The Second Data Release of the Sloan Digital Sky Survey. , keywords =. doi:10.1086/421365 , archivePrefix =. astro-ph/0403325 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/421365

  9. [9]

    Application to Arcturus and other stars; with effective temperatures

    Stellar angular diameters from infrared photometry. Application to Arcturus and other stars; with effective temperatures. , keywords =. doi:10.1093/mnras/180.2.177 , adsurl =

    work page doi:10.1093/mnras/180.2.177

  10. [10]

    , keywords =

    Determination of temperatures and angular diameters of 114 F-M stars using the infrared flux method (IRFM). , keywords =

  11. [11]

    and Li, Nolan , journal=

    Thakar, Ani R. and Li, Nolan , journal=. 2008 , volume=. doi:10.1109/MCSE.2008.6 , url =

    work page doi:10.1109/mcse.2008.6 2008

  12. [12]

    , keywords =

    The infrared flux method for determining stellar angular diameters and effective temperatures. , keywords =. doi:10.1093/mnras/188.4.847 , adsurl =

    work page doi:10.1093/mnras/188.4.847

  13. [13]

    , keywords =

    Use of the infra-red flux method for determining stellar effective temperatures and angular diameters; the stellar temperature scale. , keywords =

  14. [14]

    , keywords =

    Determination of effective temperatures for an extended sample of dwarfs and subdwarfs (F0-K5). , keywords =

  15. [15]

    , 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 =

    work page doi:10.1093/mnras/stab2304 2011

  16. [16]

    The Effective Temperature Scale of FGK Stars. II. T _ eff :Color:[Fe/H] Calibrations. , keywords =. doi:10.1086/430102 , archivePrefix =. astro-ph/0503110 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/430102

  17. [17]

    A new implementation of the infrared flux method using the 2MASS catalogue

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200810904

  18. [18]

    An absolutely calibrated effective temperature scale from the InfraRed Flux Method

    An absolutely calibrated T _ eff scale from the infrared flux method. Dwarfs and subgiants. , keywords =. doi:10.1051/0004-6361/200913204 , archivePrefix =. 1001.3142 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200913204

  19. [19]

    , keywords =

    The Sloan Digital Sky Survey Photometric System. , keywords =. doi:10.1086/117915 , adsurl =

    work page doi:10.1086/117915

  20. [20]

    Photometric Response Functions of the SDSS Imager

    Photometric Response Functions of the Sloan Digital Sky Survey Imager. , keywords =. doi:10.1088/0004-6256/139/4/1628 , archivePrefix =. 1002.3701 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/139/4/1628

  21. [21]

    SkyMapper stellar parameters for Galactic Archaeology on a grand-scale

    SkyMapper stellar parameters for Galactic Archaeology on a grand-scale. , keywords =. doi:10.1093/mnras/sty2878 , archivePrefix =. 1810.09581 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2878

  22. [22]

    The Sloan Digital Sky Survey: Technical Summary

    The Sloan Digital Sky Survey: Technical Summary. , keywords =. doi:10.1086/301513 , archivePrefix =. astro-ph/0006396 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/301513

  23. [23]

    A Modified Magnitude System that Produces Well-Behaved Magnitudes, Colors, and Errors Even for Low Signal-to-Noise Ratio Measurements

    A Modified Magnitude System that Produces Well-Behaved Magnitudes, Colors, and Errors Even for Low Signal-to-Noise Ratio Measurements. , keywords =. doi:10.1086/301004 , archivePrefix =. astro-ph/9903081 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/301004

  24. [24]

    Astronomical Data Analysis Software and Systems XIV , year = 2005, editor =

    TOPCAT & STIL: Starlink Table/VOTable Processing Software. Astronomical Data Analysis Software and Systems XIV , year = 2005, editor =

    2005

  25. [25]

    Black-Body Stars

    Blackbody Stars. , keywords =. doi:10.3847/1538-3881/aac88b , archivePrefix =. 1711.01122 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aac88b

  26. [26]

    , keywords =

    Secondary standard stars for absolute spectrophotometry. , keywords =. doi:10.1086/160817 , adsurl =

    work page doi:10.1086/160817

  27. [27]

    , year = 2005, month = sep, volume =

    Standard Photometric Systems. , year = 2005, month = sep, volume =. doi:10.1146/annurev.astro.41.082801.100251 , adsurl =

    work page doi:10.1146/annurev.astro.41.082801.100251 2005

  28. [28]

    The Thirteenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-IV Survey MApping Nearby Galaxies at Apache Point Observatory

    The 13th Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-IV Survey Mapping Nearby Galaxies at Apache Point Observatory. , keywords =. doi:10.3847/1538-4365/aa8992 , archivePrefix =. 1608.02013 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aa8992

  29. [29]

    , keywords =

    Model atmospheres for Vega. , keywords =

  30. [30]

    SDSS-III: Massive Spectroscopic Surveys of the Distant Universe, the Milky Way Galaxy, and Extra-Solar Planetary Systems

    SDSS-III: Massive Spectroscopic Surveys of the Distant Universe, the Milky Way, and Extra-Solar Planetary Systems. , keywords =. doi:10.1088/0004-6256/142/3/72 , archivePrefix =. 1101.1529 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/142/3/72

  31. [31]

    New Grids of ATLAS9 Model Atmospheres

    New Grids of ATLAS9 Model Atmospheres. Modelling of Stellar Atmospheres , year = 2003, editor =. doi:10.48550/arXiv.astro-ph/0405087 , archivePrefix =. astro-ph/0405087 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0405087 2003

  32. [32]

    Synthetic Stellar Photometry - I. General considerations and new transformations for broad-band systems

    Synthetic stellar photometry - I. General considerations and new transformations for broad-band systems. , keywords =. doi:10.1093/mnras/stu1476 , archivePrefix =. 1407.6095 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu1476

  33. [33]

    A Catalog of Spectroscopically Confirmed White Dwarfs from the Sloan Digital Sky Survey Data Release 4

    A Catalog of Spectroscopically Confirmed White Dwarfs from the Sloan Digital Sky Survey Data Release 4. , keywords =. doi:10.1086/507110 , archivePrefix =. astro-ph/0606700 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/507110

  34. [34]

    Use of a self-consistent calibration

    Effect of improved H- opacity on the infrared flux method temperature scale and derived angular diameters. Use of a self-consistent calibration. , keywords =

  35. [35]

    , keywords =

    Accurate fundamental parameters for lower main-sequence stars. , keywords =. doi:10.1111/j.1365-2966.2006.10999.x , archivePrefix =. astro-ph/0608504 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.10999.x 2006

  36. [36]

    , keywords =

    Hubble Space Telescope CALSPEC Flux Standards: Sirius (and Vega). , keywords =. doi:10.1088/0004-6256/147/6/127 , adsurl =

    work page doi:10.1088/0004-6256/147/6/127

  37. [37]

    , keywords =

    Spectrophotometric Standards from the Far-Ultraviolet to the Near-Infrared: STIS and NICMOS Fluxes. , keywords =. doi:10.1086/323137 , adsurl =

    work page doi:10.1086/323137

  38. [38]

    Update of the STIS CTE Correction Formula for Stellar Spectra

  39. [39]

    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 =

    work page doi:10.1051/0004-6361/202243709

  40. [40]

    2023 , pages =

    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

  41. [41]

    , keywords =

    Calibration of Synthetic Photometry Using DA White Dwarfs. , keywords =. doi:10.1086/505938 , adsurl =

    work page doi:10.1086/505938

  42. [42]

    , keywords =

    Stellar effective temperatures and angular diameters determined by the infrared flux method (IRFM) : revisions using improved Kurucz LTE stellar atmospheres. , keywords =

  43. [43]

    , keywords =

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

    work page doi:10.1086/498708

  44. [44]

    , keywords =

    Faint White Dwarf Flux Standards: Data and Models. , keywords =. doi:10.3847/1538-3881/ad93d8 , archivePrefix =. 2411.09049 , primaryClass =

    work page doi:10.3847/1538-3881/ad93d8

  45. [45]

    LSST: from Science Drivers to Reference Design and Anticipated Data Products

    LSST: From Science Drivers to Reference Design and Anticipated Data Products. , keywords =. doi:10.3847/1538-4357/ab042c , archivePrefix =. 0805.2366 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab042c

  46. [46]

    A catalogue of the Chandra Deep Field South with multi-colour classification and photometric redshifts from COMBO-17

    A catalogue of the Chandra Deep Field South with multi-colour classification and photometric redshifts from COMBO-17. , keywords =. doi:10.1051/0004-6361:20040525 , archivePrefix =. astro-ph/0403666 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20040525

  47. [47]

    Morphological Classification of Galaxies using Photometric Parameters: the Concentration index versus the Coarseness parameter

    Morphological Classification of Galaxies Using Photometric Parameters: The Concentration Index versus the Coarseness Parameter. , keywords =. doi:10.1086/444416 , archivePrefix =. astro-ph/0507060 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/444416

  48. [48]

    The Photometric Classification Server for Pan-STARRS1

    The Photometric Classification Server for Pan-STARRS1. , keywords =. doi:10.1088/0004-637X/746/2/128 , archivePrefix =. 1109.5080 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/746/2/128

  49. [49]

    , keywords =

    A novel optimal transport-based approach for interpolating spectral time series: Paving the way for photometric classification of supernovae. , keywords =. doi:10.1051/0004-6361/202449170 , archivePrefix =. 2409.10701 , primaryClass =

    work page doi:10.1051/0004-6361/202449170

  50. [50]

    , keywords =

    Machine learning-based photometric classification of galaxies, quasars, emission-line galaxies, and stars. , keywords =. doi:10.1093/mnras/stad3436 , archivePrefix =. 2311.02951 , primaryClass =

    work page doi:10.1093/mnras/stad3436

  51. [51]

    A 3D Dust Map Based on Gaia, Pan-STARRS 1 and 2MASS

    A 3D Dust Map Based on Gaia, Pan-STARRS 1, and 2MASS. , keywords =. doi:10.3847/1538-4357/ab5362 , archivePrefix =. 1905.02734 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab5362 1905

  52. [52]

    The GALAH Survey: Scientific Motivation

    The GALAH survey: scientific motivation. , keywords =. doi:10.1093/mnras/stv327 , archivePrefix =. 1502.04767 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv327

  53. [53]

    APOGEE: The Apache Point Observatory Galactic Evolution Experiment

    APOGEE: The Apache Point Observatory Galactic Evolution Experiment. Astronomische Nachrichten , keywords =. doi:10.1002/asna.200811080 , archivePrefix =. 0809.2362 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1002/asna.200811080

  54. [54]

    doi:10.5281/zenodo.6563093 , version =

    gaia-dpci/GaiaXPy: Release 1.0.0. doi:10.5281/zenodo.6563093 , version =

    work page doi:10.5281/zenodo.6563093

  55. [55]

    The Wide Field Infrared Survey Telescope: 100 Hubbles for the 2020s

    The Wide Field Infrared Survey Telescope: 100 Hubbles for the 2020s. arXiv e-prints , keywords =. doi:10.48550/arXiv.1902.05569 , archivePrefix =. 1902.05569 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1902.05569 1902

  56. [56]

    Scientia Sinica Physica, Mechanica & Astronomica , year = 2011, month = jan, volume =

    Consideration for a large-scale multi-color imaging and slitless spectroscopy survey on the Chinese space station and its application in dark energy research. Scientia Sinica Physica, Mechanica & Astronomica , year = 2011, month = jan, volume =. doi:10.1360/132011-961 , adsurl =

    work page doi:10.1360/132011-961 2011

  57. [57]

    Testing photometric redshift measurements with filter definition of the Chinese Space Station Optical Survey (CSS-OS)

    Testing photometric redshift measurements with filter definition of the Chinese Space Station Optical Survey (CSS-OS). , keywords =. doi:10.1093/mnras/sty1980 , archivePrefix =. 1706.09586 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1980

  58. [58]

    , keywords =

    Cosmology from the Chinese Space Station Optical Survey (CSS-OS). , keywords =. doi:10.3847/1538-4357/ab391e , archivePrefix =. 1901.04634 , primaryClass =

    work page doi:10.3847/1538-4357/ab391e 1901

  59. [59]

    , keywords =

    Combined APOGEE-GALAH stellar catalogues using the Cannon. , keywords =. doi:10.1093/mnras/stac873 , archivePrefix =. 2011.02783 , primaryClass =

    work page doi:10.1093/mnras/stac873 2011

  60. [60]

    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

  61. [61]

    , keywords =

    Internal calibration of Gaia BP/RP low-resolution spectra. , keywords =. doi:10.1051/0004-6361/202141249 , archivePrefix =. 2106.01752 , primaryClass =

    work page doi:10.1051/0004-6361/202141249

  62. [62]

    Processing and validation of BP/RP low-resolution spectral data

    Gaia Data Release 3. Processing and validation of BP/RP low-resolution spectral data. , keywords =. doi:10.1051/0004-6361/202243680 , archivePrefix =. 2206.06143 , primaryClass =

    work page doi:10.1051/0004-6361/202243680

  63. [63]

    External calibration of BP/RP low-resolution spectroscopic data

    Gaia Data Release 3. External calibration of BP/RP low-resolution spectroscopic data. , keywords =. doi:10.1051/0004-6361/202243880 , archivePrefix =. 2206.06205 , primaryClass =

    work page doi:10.1051/0004-6361/202243880

  64. [64]

    , keywords =

    The Early-type Stars from the LAMOST Survey: Atmospheric Parameters. , keywords =. doi:10.3847/1538-4365/ac2ded , archivePrefix =. 2110.06246 , primaryClass =

    work page doi:10.3847/1538-4365/ac2ded

  65. [65]

    , keywords =

    Deriving the Stellar Labels of LAMOST Spectra with the Stellar LAbel Machine (SLAM). , keywords =. doi:10.3847/1538-4365/ab55ef , archivePrefix =. 1908.08677 , primaryClass =

    work page doi:10.3847/1538-4365/ab55ef 1908

  66. [66]

    , keywords =

    Estimating the Atmospheric Parameters of Early-type Stars from the Chinese Space Station Telescope (CSST) Slitless Spectra Survey. , keywords =. doi:10.3847/1538-3881/ad4463 , archivePrefix =. 2408.10803 , primaryClass =

    work page doi:10.3847/1538-3881/ad4463

  67. [67]

    , keywords =

    Empirical effective temperatures and bolometric corrections for early-type stars. , keywords =. doi:10.1086/154093 , adsurl =

    work page doi:10.1086/154093

  68. [68]

    Fundamental stellar parameters of benchmark stars from CHARA interferometry. I. Metal-poor stars. , keywords =. doi:10.1051/0004-6361/202037590 , archivePrefix =. 2006.05411 , primaryClass =

    work page doi:10.1051/0004-6361/202037590 2006

  69. [69]

    Sulphur and zinc abundances in Galactic halo stars revisited

    Sulphur and zinc abundances in Galactic halo stars revisited. , keywords =. doi:10.1051/0004-6361:20077344 , archivePrefix =. astro-ph/0702689 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20077344

  70. [70]

    , keywords =

    Nearby stars of the Galactic disc and halo - IV. , keywords =. doi:10.1111/j.1365-2966.2007.12671.x , adsurl =

    work page doi:10.1111/j.1365-2966.2007.12671.x 2007