Pith. sign in

REVIEW 3 major objections 6 minor 14 cited by

The Nineteenth Data Release of the Sloan Digital Sky Survey

T0 review · 3 major / 6 minor · reviewed 2026-08-06 · deepseek-v4-flash

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

Pith's one-line read The nineteenth data release of the Sloan Digital Sky Survey is the first to include data from all three SDSS-V mappers, delivering roughly two million new stellar spectra, a large multi-epoch quasar sample, and a first integral-field tile…

desk verdict A major, well-documented data release with one concrete counting error in the summary that should be corrected before publication. read the letter →

arxiv 2507.07093 v1 pith:H5AX5USF submitted 2025-07-09 astro-ph.GA astro-ph.COastro-ph.IMastro-ph.SR

SDSS Collaboration , Gautham Adamane Pallathadka , Mojgan Aghakhanloo , James Aird , Andrés Almeida , Singh Amrita , Friedrich Anders , Scott F. Anderson
show 204 more authors
Stefan Arseneau Consuelo González Avila Shir Aviram Catarina Aydar Carles Badenes Jorge K. Barrera-Ballesteros Franz E. Bauer Aida Behmard Michelle Berg F. Besser Christian Moni Bidin Dmitry Bizyaev Guillermo Blanc Michael R. Blanton Jo Bovy William Nielsen Brandt Joel R. Brownstein Johannes Buchner Esra Bulbul Joseph N. Burchett Leticia Carigi Joleen K. Carlberg Andrew R. Casey Priyanka Chakraborty Julio Chanamé Vedant Chandra Cristina Chiappini Igor Chilingarian Johan Comparat Kevin Covey Nicole Crumpler Katia Cunha Elena D'Onghia Xinyu Dai Jeremy Darling Megan Davis Nathan De Lee Niall Deacon José Eduardo Méndez Delgado Sebastian Demasi Mariia Demianenko Delvin Demke John Donor Niv Drory Monica Alejandra Villa Durango Tom Dwelly Oleg Egorov Evgeniya Egorova Kareem El-Badry Mike Eracleous Xiaohui Fan Emily Farr Douglas P. Finkbeiner Logan Fries Peter Frinchaboy Nicola Pietro Gentile Fusillo Luis Daniel Serrano Félix Boris Gaensicke Emma Galligan Pablo García Joseph Gelfand Katie Grabowski Eva Grebel Paul J Green Hannah Greve Catherine Grier Emily Griffith Paloma Guetzoyan Pramod Gupta Zoe Hackshaw Patrick B. Hall Keith Hawkins Viola Hegedűs Saskia Hekker T. M. Herbst J. J. Hermes Lorena Hernández-García Pranavi Hiremath David W Hogg Jon Holtzman Keith Horne Danny Horta Yang Huang Brian Hutchinson Maximilian Häberle Hector Javier Ibarra-Medel Alexander P. Ji Paula Jofre James W. Johnson Jennifer Johnson Evelyn J. Johnston Mary Kaldor Ivan Katkov Arman Khalatyan Sergey Khoperskov Ralf Klessen Matthias Kluge Anton M. Koekemoer Juna A. Kollmeier Marina Kounkel Kathryn Kreckel Dhanesh Krishnarao Mirko Krumpe Ivan Lacerna Chervin Laporte Sebastien Lepine Jing Li Fu-Heng Liang Guilherme Limberg Xin Liu Sarah Loebman Knox Long Yuxi Lu Madeline Lucey Alejandra Z. Lugo-Aranda Mary Loli Martínez Martinez-Aldama Kevin McKinnon Ilija Medan Andrea Merloni Sean Morrison Natalie Myers Szabolcs Mészáros Johanna Müller-Horn Samir Nepal Melissa Ness David Nidever Christian Nitschelm Audrey Oravetz Jonah Otto Kaike Pan Facundo Pérez Paolino Castalia Alenka Negrete Peñaloza Marc Pinsonneault Manuchehr Taghizadeh Popp Adrian Price-Whelan Nadiia Pulatova Anna Barbara Queiroz Jordan Raddick Amy Rankine Hans-Walter Rix Carlos Román-Zúñiga Daniela Fernández Rosso Jessie Runnoe Serat Mahmud Saad Mara Salvato Sebastian F. Sanchez Natascha Sattler Andrew Saydjari Conor Sayres Kevin Schlaufman Donald P. Schneider Axel Schwope Lucas M. Seaton Rhys Seeburger Javier Serna Sanjib Sharma Yue Shen Amaya Sinha Brian Sizemore Marzena Sniegowska Yingyi Song Diogo Souto Keivan Stassun Matthias Steinmetz Zachary Stone Alexander Stone-Martinez Guy S. Stringfellow Aurora Mata Sánchez José Sánchez-Gallego Jonathan Tan Jamie Tayar Riley Thai Ani Thakar Pierre Thibodeaux Yuan-Sen Ting Andrew Tkachenko Benny Trakhtenbrot Jose G. Fernandez Trincado Nicholas Troup Jonathan R. Trump Natalie Ulloa Roeland P. Van der Marel Pablo Vera Sandro Villanova Jaime Villaseñor Ji Wang Zachary Way Anne-Marie Weijmans Adam Wheeler John C. Wilson Aida Wofford Tony Wong Qiaoya Wu Dominika Wylezalek Xiang-Xiang Xue Renbin Yan Qian Yang Nadia Zakamska Eleonora Zari Gail Zasowski Grisha Zeltyn Zheng Zheng Catherine Zucker Rodolfo de J. Zermeño
This is my paper
classification astro-ph.GAastro-ph.COastro-ph.IMastro-ph.SR
keywords surveysastronomydatabasesdataacquisitionsoftwareSloanDigitalSkySurveySDSS-Vspectroscopyintegralfield
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

This paper is the official description of DR19, the nineteenth data release of the Sloan Digital Sky Survey and the first to contain data from all three SDSS-V science programs. The central claim is that DR19 delivers roughly 1.2 million APOGEE and 800,000 BOSS spectra of about 390,000 and 475,000 stars, about 380,000 BOSS spectra of roughly 120,000 extragalactic objects from the Black Hole Mapper, the first integral-field tile of the Helix Nebula from the Local Volume Mapper, and nine value-added catalogs, all publicly accessible. A sympathetic reader would care because this is the point where SDSS-V stops being a targeting exercise and becomes a working public data resource for Milky Way archaeology, black hole growth, and the ionized interstellar medium. The paper's load-bearing work is the documentation of the new reduction and analysis pipelines that turn raw exposures into these science-ready products.

What carries the argument

The carrying object is the release itself, but the argument for its scientific usefulness runs through four pipeline systems. The BOSS optical pipeline (idlspec2d, version v6_1_3) introduces a two-step exposure coadding scheme; the APOGEE near-infrared reduction pipeline (version 1.3) introduces a model point-spread function and daily wavelength solutions anchored by Fabry-Perot interferometer references; the Astra framework orchestrates stellar-parameter and abundance pipelines (ASPCAP, APOGEENet, AstroNN, ThePayne, and BOSS stellar classifiers) into one preferred-parameter summary file; and the Local Volume Mapper data reduction pipeline converts raw exposures into flux-calibrated, sky-subtracted row-stacked spectra. On the distribution side, the new Semaphore targeting flags, the sdss id cross-match identifier, and the Zora/Valis web framework are what make the data findable and reproducible.

What would settle it

For the stellar products, compare stellar parameters and abundances of the same stars reduced through both the DR17 legacy APOGEE pipeline and the DR19 version: systematic differences larger than the quoted uncertainties would show the new model PSF and wavelength solutions are not on the same scale as the legacy products. For the completeness claim, count the DR19 spectra that lack FERRE-based analysis results and test whether the missingness correlates with signal-to-noise, target type, or fiber position; if it is not random, the released sample is biased. For the Local Volume Mapper, compare fluxes of the cautioned lines (such as [O I] at 6300 Å and lines above 7000 Å) in the Helix tile against independent narrowband imaging to test whether the warned-about sky-subtraction contamination is actually present.

Watch

Extended reading notes

Core claim

DR19 is the second SDSS-V data release and, by the paper's accounting, the most substantial to date: it is the first release to include data from all three mappers. The Milky Way Mapper contributes about 1.2 million near-infrared APOGEE spectra and 800,000 optical BOSS spectra of roughly 390,000 and 475,000 unique stars, most of them run through the Astra stellar-parameter framework; the Black Hole Mapper contributes about 380,000 BOSS spectra of roughly 120,000 distinct quasars, AGN, X-ray sources, and cluster galaxies, including intense multi-epoch monitoring of reverberation-mapping fields; and the Local Volume Mapper contributes one reduced integral-field tile of the Helix Nebula as a preview of its data model. Nine value-added catalogs supplement the official pipeline products, and access is provided through the archive servers, SciServer, and a new Zora/Valis web framework. The paper argues that together these products make DR19 the first substantial public data delivery of the SDSS-V era.

Load-bearing premise

The release's scientific value rests on the accuracy of the newly upgraded reduction pipelines, and the paper itself cautions that the Local Volume Mapper reduction is still under active development, with sky subtraction and flux calibration that may still contaminate some lines, and that FERRE timeouts left a random subset of good spectra without analysis results.

Editorial extensions

If this is right

  • Astronomers can now build homogeneous samples of roughly 390,000 infrared and 475,000 optical stellar spectra with stellar parameters and abundances from the Astra framework, supporting Galactic archaeology and stellar physics at scales comparable to the full APOGEE-1 and -2 surveys.
  • The Black Hole Mapper data expand BHM spectroscopy by roughly an order of magnitude over DR18, enabling time-domain quasar studies (reverberation mapping, changing-look quasars, broad absorption line variability) and X-ray-selected AGN demographics from the SPIDERS program.
  • The single Local Volume Mapper tile of the Helix Nebula gives the community a first working example of the LVM data model and a resolved view of a planetary nebula at 0.03 pc resolution across a roughly 2 pc field.
  • The nine value-added catalogs extend the official products with M-dwarf elemental abundances, DA white dwarf physical parameters, stellar distances, masses and ages, cluster membership, quasar spectral properties, and component-separated APOGEE spectra.
  • The combination of daily, epoch, and allepoch coadds for BHM targets means time-domain claims can be checked against the choice of coadding scheme, and future releases are expected to extend the same products to southern-hemisphere data and a much larger LVM sample.

Reading between the lines

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

  • If the multi-epoch BHM spectra hold up under scrutiny, the daily-versus-allepoch coadd products effectively hand the community a built-in robustness test for every time-domain quasar claim made from DR19, something the paper documents but does not itself exploit.
  • The MADGICS component-separation catalog points toward a regime in which spectra are released as component posteriors rather than point estimates; if that regime becomes standard, stellar parameter and abundance pipelines will need to consume posterior distributions, a transition the paper's authors flag as needing pipeline maintainers' cooperation.
  • The sdss id cross-match layer is likely to become the standard way to join SDSS-V spectra to Gaia, TESS, and eROSITA catalogs; because it ties together cross-match versions, it also makes the survey's selection function reproducible, which is what statistical uses of SPIDERS and the quasar VAC will depend on.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. This paper describes SDSS DR19, the second data release of SDSS-V and the first to include data from all three mappers. The release contains new APOGEE and BOSS spectra from the Milky Way Mapper, BHM-led BOSS spectra of extragalactic targets, a single preview LVM integral-field tile of the Helix Nebula, nine value-added catalogs, a new targeting-flag system (Semaphore), the sdss id cross-match identifier, the Zora/Valis web framework, and a suite of Python tutorials. The paper describes the targeting database, the updated BOSS, APOGEE, Astra, and LVM reduction/analysis pipelines, and the access infrastructure (SAS, CAS, SciServer).

Significance. If the described data products are as characterized, DR19 is a major milestone: it is the first public release containing SDSS-V data from all three mappers, with roughly 1.2 million APOGEE and 800,000 BOSS spectra of several hundred thousand stars, about 380,000 BHM-led BOSS spectra, and the first LVM data. The paper's strengths include unusually complete documentation of targeting generations, cartons, pipeline versions, data models, and access paths; public code repositories for pipelines, Semaphore, and tutorials; and nine VACs with companion papers. Several limitations are honestly disclosed, notably the active development of the LVM pipeline and the FERRE timeout issue. However, the paper's central quantitative description of the release is undermined by an internal inconsistency between the summary count for BHM objects and the counts given in Section 5.2 and Table 6, which must be resolved before the release description can be trusted.

major comments (3)
  1. [Section 9, first bullet; Section 5.2; Table 6] The summary states that DR19 contains 'BOSS spectra of 318,123 galaxies and quasars/AGN,' but Section 5.2 reports approximately 380,000 BHM-led BOSS spectra for about 120,000 distinct objects, and the 'Unique targets' column of Table 6 sums to roughly 121,800 (with daily coadded spectra summing to roughly 378,600). The number 318,123 appears nowhere else in the paper, and it is unclear whether it is meant to count spectra or unique objects. Since the central claim of a data-release paper is an accurate quantitative description of the released data, this inconsistency must be fixed by deriving the headline count directly from the release database and by stating explicitly whether each count refers to spectra, unique objects, or unique SDSS IDs.
  2. [Section 5.1.1, Figure 4] The claim that DR19 achieves a minimum unbiased radial-velocity scatter of approximately 41 m/s is presented without an uncertainty or a sample size for the minimum bin. The figure shows median scatter per SNR bin, but the quoted minimum is not accompanied by a bootstrap or other uncertainty estimate, and the number of stars in the relevant SNR bin is not stated. Please provide the uncertainty on the 41 m/s value and the sample size, or rephrase the claim to match what Figure 4 actually demonstrates.
  3. [Section 4.3.2, item 5; Section 5.1] The FERRE timeout issue is disclosed, but its impact on the released products is not quantified. The text says 'a random subset of good spectra will sometimes have no results' and that some spectra were 'labelled problematic when they weren't,' yet Section 5.1 states that 'Almost all of these spectra have been run through Astra.' For users to know the completeness of the stellar-parameter products, the paper should state the fraction of released APOGEE spectra (and of BOSS spectra in MWM cartons) that lack ASPCAP or other Astra pipeline results, and how this fraction varies across the data set.
minor comments (6)
  1. [Section 5.1] The text gives '~390,00 and ~475,000 unique stars,' where '390,00' is missing a digit, and the second number differs slightly from the 479,081 quoted in the Section 9 summary; please harmonize these numbers.
  2. [Section 2.1, Planet Hosts paragraph] The phrase 'planets hosting starts' should be 'planet-hosting stars.'
  3. [Section 5.3] The word 'homogentized' should be 'homogenized,' and the sentence beginning 'The data reduction pipeline is still under active development' could be moved earlier in the paragraph so the caveat appears before the preview is described.
  4. [Figure 4 caption] The caption contains a doubled article: 'The The data is binned by logarithmic x-coordinate.'
  5. [Section 4.1] The phrase 'depreciated from the final spAll summary files' should likely read 'deprecated' (or 'removed'), and the Elodie fit parameters are said to remain in intermediate products, so please clarify their status.
  6. [Section 7.5] The StarHorse calibration equations are given with many significant digits but no stated uncertainties or derivation reference; please indicate the source of the fitted coefficients or provide a reference to where they are derived.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: DR19 is a data-release description whose claims are existence and accessibility of independently produced data products.

full rationale

This paper is a data-release description, not a derivation chain. Its central claims are that DR19 contains data from all three SDSS-V mappers, that specific numbers of spectra and targets are included, and that the data are publicly accessible through the described interfaces. None of these claims is derived from a fitted parameter, an assumed ansatz, or a uniqueness theorem. The reduction pipelines described in Section 4 are presented as processing the released data, but the release's existence and content do not depend on the pipelines being correct in any circular way; pipeline weaknesses are disclosed as limitations rather than used to justify the release. The many self-citations, including in-preparation pipeline papers and prior DR18 documentation, are bibliographical support for methods and targeting conventions, not load-bearing evidence that the data exist. The VAC summaries (Section 7) describe externally validated or independently constructed catalogs, and they are not used to justify the release itself. The reader's flagged inconsistency between the Section 9 summary count of 318,123 BHM galaxies/quasars and the Section 5.2/Table 6 figures (~380,000 spectra, ~120,000 objects) is a potential internal-consistency or correctness issue, not circularity, because no quantity is being defined in terms of another as a prediction. Similarly, the FERRE-timeout caveat and the LVM sky-subtraction cautions are honest limitations. No step reduces by construction to its own input, so the circularity score is 0.

Assumptions & free parameters 5 free parameters · 4 assumptions · 0 invented entities

The paper makes no physical derivation, so the ledger is small. The listed free parameters are calibration coefficients and a density threshold inside two value-added catalogs; they are not used to derive the central claim that the data are released. The axioms are domain assumptions inherited from the source catalogs and models the VACs rely on.

free parameters (5)
  • StarHorse Teff calibration slope = 0.86463363
    Applied as Teff(DR17-like) = raw_teff * 0.86463363 + 720.06160957 to bring DR19 APOGEE Teff onto the DR17 scale before the StarHorse run (Section 7.5).
  • StarHorse Teff calibration intercept = 720.06160957 K
    Same linear correction, Section 7.5.
  • StarHorse log g calibration slope = 0.82897254
    Applied as log g(DR17-like) = log g * 0.82897254 + 0.31209658, Section 7.5.
  • StarHorse log g calibration intercept = 0.31209658
    Same linear correction, Section 7.5.
  • StarFlow training-space density cut = 3 x 10^9
    Threshold used to define the main StarFlow catalog sample (Section 7.8).
assumptions (4)
  • domain assumption Binary wide companions are chemically homogeneous with their primaries
    Used in VAC 7.1 to transfer FGK ASPCAP abundances to M dwarf companions when training The Cannon (Section 7.1).
  • domain assumption PARSEC 1.2S stellar isochrones cover the parameter space of all fitted stars
    StarHorse posteriors are constrained to these isochrones (Section 7.5).
  • domain assumption Single-epoch virial relations and fixed bolometric corrections are valid for the quasar sample
    SMBH masses use Vestergaard & Peterson (2006); bolometric luminosities use Richards et al. (2006) corrections (Section 7.9).
  • domain assumption Dust maps (SFD, Green et al. 2015) and Fitzpatrick (1999) extinction curve describe the true extinction
    Used for BOSS spectra in the Galactic plane (Section 4.1) and for WD photometric fits (Section 7.6).

how reviews work

0 comments
Cite this review

Pith. "Pith review of The Nineteenth Data Release of the Sloan Digital Sky Survey." pith.science (2026). https://pith.science/paper/H5AX5USF

@misc{pith2026250707093,
  author       = {Pith},
  title        = {Pith review of: The Nineteenth Data Release of the Sloan Digital Sky Survey},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/H5AX5USF}},
  note         = {Machine review of arXiv:2507.07093}
}
read the original abstract

Mapping the local and distant Universe is key to our understanding of it. For decades, the Sloan Digital Sky Survey (SDSS) has made a concerted effort to map millions of celestial objects to constrain the physical processes that govern our Universe. The most recent and fifth generation of SDSS (SDSS-V) is organized into three scientific ``mappers". Milky Way Mapper (MWM) that aims to chart the various components of the Milky Way and constrain its formation and assembly, Black Hole Mapper (BHM), which focuses on understanding supermassive black holes in distant galaxies across the Universe, and Local Volume Mapper (LVM), which uses integral field spectroscopy to map the ionized interstellar medium in the local group. This paper describes and outlines the scope and content for the nineteenth data release (DR19) of SDSS and the most substantial to date in SDSS-V. DR19 is the first to contain data from all three mappers. Additionally, we also describe nine value added catalogs (VACs) that enhance the science that can be conducted with the SDSS-V data. Finally, we discuss how to access SDSS DR19 and provide illustrative examples and tutorials.

Figures

Figures reproduced from arXiv: 2507.07093 by the authors.

Figure 1
Figure 1. This flowchart contains the decision tree used to determine which pipeline and reported parameters Astra are preferred for an individual unique source (i.e., with a unique SDSS ID) [PITH_FULL_IMAGE:figures/full_fig_p022_1.png] view at source ↗
Figure 2
Figure 2. The right ascension (RA) and declination (DEC) for targets observed in DR19 MWM (red), DR19 BHM (blue) and legacy observations from SDSS-IV (gray). SDSS-V DR19 contains new spectra from the APO telescope in the Northern hemisphere [PITH_FULL_IMAGE:figures/full_fig_p025_2.png] view at source ↗
Figure 3
Figure 3. The ‘preferred’ log g as a function of Teff (Kiel di￾agram) for MWM spectra run through Astra. Lighter cells represent those which contain significantly more individual objects compared to cells which are darker. ‘Preferred’ Teff and log g are drawn from the astraMWMLite file, which uses the decision tree outlined in [PITH_FULL_IMAGE:figures/full_fig_p025_3.png] view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: The relationship between the median visit SNR versus the unbiased radial velocity scatter for stars with the following cuts: Teff < 6250 K, log g > 1.5, and unbiased RV scatter < 1.0 km/s. The underlying color map shows the number of stars in each logarithmic 2-dimensi…
Figure 5
Figure 5. Figure 5: Distribution (RA, Dec) on the sky of BHM (and related) optical spectra released in DR19. The color cod￾ing indicates the number (logarithmic scaling) of spectra per BHM object/target; many BHM spectra are multi-epoch. DR19 contains BOSS spectra for three BHM RM fields …
Figure 6
Figure 6. Figure 6: Density contours of X-ray sources in the observed X-ray (0.2−2.3 keV) luminosity vs. redshift plane. Blue con￾tours represent the sources from eRASS1 released in DR19 as part of the VAC catalog described in section 7.2; red con￾tours represent the sources in the eFEDS …
Figure 7
Figure 7. Figure 7: Composite red (R), green (G), blue (B) map of the Helix nebula constructed by using spectral windows that capture the three emission lines given in the title. Fibers with known issues have been removed. We include fibers that catch contaminating stars. in Section 6.2; …
Figure 8
Figure 8. Figure 8: SkyServer-Navigate application, fully redesigned. A major new feature for DR19 is the fully redesigned SkyServer Navigate App shown in [PITH_FULL_IMAGE:figures/full_fig_p030_8.png]
Figure 9
Figure 9. Figure 9: Zora target page, with interactive spectral display, and pipeline and metadata parameters [PITH_FULL_IMAGE:figures/full_fig_p033_9.png]
Figure 10
Figure 10. Figure 10: Zora on-sky explorer, with cone search overlay and results. SNR, class, best fit stellar template, and proper￾ties (spectral type, effective temperature, surface gravity, and Hα equivalent width from Astra). • From eROSITA: unique X-ray source identifier (DETUID), flu…
Figure 11
Figure 11. Figure 11: Zora dataview dashboard, with interactive catalog filtering and chart plotting [PITH_FULL_IMAGE:figures/full_fig_p034_11.png]

Discussion (0). Sign in to comment.

Forward citations

Cited by 14 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Detecting Solar-Like Oscillations in the Highest Mass TESS Giants

    astro-ph.SR 2026-07 conditional novelty 6.0 of 10

    Custom-aperture TESS photometry detects solar-like oscillations in 43 intermediate-mass giants (10 above 5 M⊙) and shows APOGEE DR19 log g is ~0.23 dex too high versus seismic values.

  2. The Twentieth Data Release of the Sloan Digital Sky Survey: First All-Sky BOSS Spectra, eROSITA-SDSS-V Mapper Coordinated Observations, and a Preview of the Local Volume Mapper

    astro-ph.GA 2026-07 accept novelty 6.0 of 10

    DR20 releases over three million BOSS spectra (first southern-hemisphere SDSS-V optical data), 169 LVM integral-field tiles over six targets, and eighteen value-added catalogs.

  3. BOSS-CLAM: Utilizing a Constrained Linear Absorption Model to Infer Stellar Parameters from BOSS Spectra

    astro-ph.SR 2026-07 conditional novelty 6.0 of 10

    A new generative pipeline, BOSS-CLAM, infers temperature, gravity, metallicity, and alpha-abundance for 1,708,214 SDSS-V BOSS spectra and releases a validated clean catalog of 915,514 stars.

  4. Payne4GAIN: NLTE Corrections for Red Giants in Milky Way Mapper using H-Band Neural Network Emulators

    astro-ph.SR 2026-07 conditional novelty 6.0 of 10

    Applying NLTE physics to APOGEE H-band spectra shifts red-giant abundances by ~0.1 dex for Al, Mn, and Ti; the paper provides a 360k-star correction catalog.

  5. A Probabilistic Framework for Population Studies of the Solar Neighborhood: Application to SDSS-V and Gaia

    astro-ph.SR 2026-07 conditional novelty 6.0 of 10

    A new probabilistic pipeline characterizes SDSS-V Solar Neighborhood Census selection effects against Gaia and infers subpopulation probabilities across the HR diagram from incomplete spectroscopy.

  6. SpecFANN: Spectral Fitting via Artificial Neural Networks I. A deep learning based fastwind emulator and fitting suite

    astro-ph.SR 2026-07 conditional novelty 6.0 of 10

    A neural-network emulator of FASTWIND reproduces OB-star line profiles to about 0.01–1% and fits stellar parameters roughly 360,000 times faster than direct FASTWIND calculations.

  7. VAR-PZnn: A machine-learning framework for AGN photometric redshifts using color and variability-based features

    astro-ph.GA 2026-07 conditional novelty 6.0 of 10

    VAR-PZnn combines ZTF g-band variability features with optical, MIR and NIR photometry in a mixture-density network to estimate AGN photometric redshifts with σ_NMAD=0.058 and an 8.2% outlier fraction on a 72,728-sour...

  8. COUGS-DESI: A Catalog of Unusual Galaxies with Polar Structures in the DESI Legacy Imaging Surveys

    astro-ph.GA 2026-01 conditional novelty 6.0 of 10

    A new visual catalog of ~3,000 polar-structure galaxy candidates in DESI Legacy imaging, ten times larger than previous samples, puts the local occurrence rate of polar structures at about 2.2% of non-dwarf galaxies.

  9. Double White Dwarf Binaries in SDSS-V DR19 : A catalog of DA white dwarf binaries and constraints on the binary population

    astro-ph.SR 2025-09 conditional novelty 6.0 of 10

    SDSS-V radial velocity monitoring yields 63 DA double white dwarf binary candidates (43 new), with fitted binary fraction f_bin,0.4 ≈ 9% and separation power-law index α ≈ -0.62.

  10. Current and future constraints on the expansion history of the GREA model

    astro-ph.CO 2026-03 conditional novelty 5.0 of 10

    GREA is disfavored by current data when CMB information is included, and forecasts show gravitational-wave standard sirens will strongly discriminate between GREA and ΛCDM.

  11. Searching for Electromagnetic Counterpart Candidates to GW231123

    astro-ph.HE 2025-11 conditional novelty 5.0 of 10

    A crossmatch of GW231123's localization with ZTF AGN-flare catalogs yields six unconfirmed optical flare candidates, with association claims driven largely by the event's high primary mass.

  12. The Milky Way - Large Magellanic Cloud Interaction with Simulation Based Inference

    astro-ph.GA 2025-10 conditional novelty 5.0 of 10

    Simulation-based inference on outer-halo star velocities gives a Milky Way reflex speed of 26.4 km/s and an LMC enclosed mass of 9.2×10^10 solar masses within 50 kpc.

  13. A Test of FeH Line Parameters using DR19 APOGEE spectra of Benchmark M Dwarfs

    astro-ph.SR 2026-07 conditional novelty 4.0 of 10

    No adjustment to Hargreaves et al. (2010) FeH gf-values is needed: binary, cluster, and interferometric M-dwarf benchmarks give consistent Fe I/FeH metallicities and Teff within uncertainties.

  14. The Open Cluster Chemical Abundances and Mapping Survey: IX. Measuring the Effects of Stellar Diffusion in the Open Clusters NGC 752 and Ruprecht 147 using APOGEE

    astro-ph.SR 2026-07 conditional novelty 4.0 of 10

    Atomic diffusion depletes surface Fe, C, Ca, and other elements in ~1.2–1.35 solar-mass stars of NGC 752 and Ruprecht 147, consistent with MIST models and affecting derived ages.

Reference graph

Works this paper leans on

192 extracted references · 14 canonical work pages · cited by 14 Pith papers

  1. [1]

    , " * 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.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    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.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    ?iCCPICC ProfileHW XS [R! RBoRBhw Q IPb ; 6tUD E,/ u`Wޤ 93 \8 OT gMNa h 2`;./_̊ /nD^ui M q:? AJXRQƛO) 0@[ x g*p +^M|, VȪ\ ːg 2Z N

    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 `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key o...

    arXiv 2017

  4. [4]

    2022, , 259, 35, 10.3847/1538-4365/ac4414

    Abdurro'uf , Accetta , K., Aerts , C., et al. 2022, , 259, 35, 10.3847/1538-4365/ac4414

    doi:10.3847/1538-4365/ac4414 2022

  5. [5]

    A., Almeida , A., et al

    Ahumada , R., Prieto , C. A., Almeida , A., et al. 2020, , 249, 3, 10.3847/1538-4365/ab929e

    doi:10.3847/1538-4365/ab929e 2020

  6. [6]

    L., Georgakakis , A., et al

    Aird , J., Coil , A. L., Georgakakis , A., et al. 2015, , 451, 1892, 10.1093/mnras/stv1062

    doi:10.1093/mnras/stv1062 2015

  7. [7]

    D., Prieto, C

    Alam, S., Albareti, F. D., Prieto, C. A., et al. 2015, The Astrophysical Journal Supplement Series, 219, 12, 10.1088/0067-0049/219/1/12

    doi:10.1088/0067-0049/219/1/12 2015

  8. [8]

    D., Allende Prieto , C., Almeida , A., et al

    Albareti , F. D., Allende Prieto , C., Almeida , A., et al. 2017, , 233, 25, 10.3847/1538-4365/aa8992

    doi:10.3847/1538-4365/aa8992 2017

Show all 192 references
  1. [9]

    F., Argudo-Fern \'a ndez , M., et al

    Almeida , A., Anderson , S. F., Argudo-Fern \'a ndez , M., et al. 2023, , 267, 44, 10.3847/1538-4365/acda98

    2023 doi

  2. [10]

    Anders , F., Khalatyan , A., Queiroz , A. B. A., et al. 2022, , 658, A91, 10.1051/0004-6361/202142369

    2022 doi

  3. [11]

    2017, , 469, 2102, 10.1093/mnras/stx796

    Anguiano , B., Rebassa-Mansergas , A., Garc \' a-Berro , E., et al. 2017, , 469, 2102, 10.1093/mnras/stx796

    2017 doi

  4. [12]

    2025, , 698, 30, https://doi.org/10.1051/0004-6361/202554372

    Aydar , C., Merloni , A., Dwelly , T., et al. 2025, , 698, 30, https://doi.org/10.1051/0004-6361/202554372

    2025 doi

  5. [13]

    Bailer-Jones , C. A. L., Rybizki , J., Fouesneau , M., Demleitner , M., & Andrae , R. 2021, , 161, 147, 10.3847/1538-3881/abd806

    2021 doi

  6. [14]

    2025, Aladin Lite, 3.6.5, Zenodo, 10.5281/zenodo.15181455

    Baumann, M., Boch, T., & Marchand, M. 2025, Aladin Lite, 3.6.5, Zenodo, 10.5281/zenodo.15181455

    2025 doi

  7. [15]

    2022, in Astronomical Society of the Pacific Conference Series, Vol

    Baumann , M., Boch , T., Pineau , F.-X., et al. 2022, in Astronomical Society of the Pacific Conference Series, Vol. 532, Astronomical Data Analysis Software and Systems XXX, ed. J. E. Ruiz , F. Pierfedereci , & P. Teuben , 7

    2022

  8. [16]

    K., Casey , A

    Behmard , A., Ness , M. K., Casey , A. R., et al. 2025, , 982, 13, 10.3847/1538-4357/adaf1f

    2025 doi

  9. [17]

    2014, , 354, 103, 10.1007/s10509-014-1935-6

    Bianchi , L. 2014, , 354, 103, 10.1007/s10509-014-1935-6

    2014 doi

  10. [18]

    2017, , 230, 24, 10.3847/1538-4365/aa7053

    Bianchi , L., Shiao , B., & Thilker , D. 2017, , 230, 24, 10.3847/1538-4365/aa7053

    2017 doi

  11. [19]

    A., Morales , F., Besser , F., et al

    Blanc , G. A., Morales , F., Besser , F., et al. 2024, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 13094, Ground-based and Airborne Telescopes X, ed. H. K. Marshall , J. Spyromilio , & T. Usuda , 1309403, 10.1117/12.3018767

    2024 doi

  12. [20]

    R., Bershady , M

    Blanton , M. R., Bershady , M. A., Abolfathi , B., et al. 2017, , 154, 28, 10.3847/1538-3881/aa7567

    2017 doi

  13. [21]

    R., Carlberg , J

    Blanton , M. R., Carlberg , J. K., Dwelly , T., et al. 2025, arXiv e-prints, arXiv:2505.21328, 10.48550/arXiv.2505.21328

    2025 doi

  14. [22]

    S., Schlegel , D

    Bolton , A. S., Schlegel , D. J., Aubourg , \'E ., et al. 2012, , 144, 144, 10.1088/0004-6256/144/5/144

    2012 doi

  15. [23]

    A., & Green , R

    Boroson , T. A., & Green , R. F. 1992, , 80, 109, 10.1086/191661

    1992 doi

  16. [24]

    F., Hogg , D

    Bovy , J., Hennawi , J. F., Hogg , D. W., et al. 2011, , 729, 141, 10.1088/0004-637X/729/2/141

    2011 doi

  17. [25]

    2022, , 661, A1, 10.1051/0004-6361/202141266

    Brunner , H., Liu , T., Lamer , G., et al. 2022, , 661, A1, 10.1051/0004-6361/202141266

    2022 doi

  18. [26]

    Budavari , T., Dobos , L., & Szalay , A. S. 2013, Computing in Science and Engineering, 15, 12, 10.1109/MCSE.2013.41

    2013 doi

  19. [27]

    A., Law, D

    Bundy, K., Bershady, M. A., Law, D. R., et al. 2015, The Astrophysical Journal, 798, 7

    2015

  20. [28]

    A., Law , D

    Bundy , K., Bershady , M. A., Law , D. R., et al. 2015, , 798, 7, 10.1088/0004-637X/798/1/7

    2015 doi

  21. [29]

    2018, , 618, A93, 10.1051/0004-6361/201833476

    Cantat-Gaudin , T., Jordi , C., Vallenari , A., et al. 2018, , 618, A93, 10.1051/0004-6361/201833476

    2018 doi

  22. [30]

    J., Noriega-Crespo , A., Mizuno , D

    Carey , S. J., Noriega-Crespo , A., Mizuno , D. R., et al. 2009, , 121, 76, 10.1086/596581

    2009 doi

  23. [31]

    A., Conroy , C., Johnson , B

    Cargile , P. A., Conroy , C., Johnson , B. D., et al. 2020, ApJ, 900, 28, 10.3847/1538-4357/aba43b

    2020 doi

  24. [32]

    R., Hogg , D

    Casey , A. R., Hogg , D. W., Ness , M., et al. 2016, arXiv e-prints, arXiv:1603.03040, 10.48550/arXiv.1603.03040

    2016 doi arXiv

  25. [33]

    2023, corv: Compact Object Radial Velocities (version 1)

    Chandra , V., Arseneau , S., Crumpler , N., & Inight , K. 2023, corv: Compact Object Radial Velocities (version 1). Zenodo. https://doi.org/10.5281/zenodo.10211598

    2023 doi

  26. [34]

    L., & Budav \'a ri , T

    Chandra , V., Hwang , H.-C., Zakamska , N. L., & Budav \'a ri , T. 2020, , 497, 2688, 10.1093/mnras/staa2165

    2020 doi

  27. [35]

    K., et al

    Chiti , A., Frebel , A., Mardini , M. K., et al. 2021, , 254, 31, 10.3847/1538-4365/abf73d

    2021 doi

  28. [36]

    L., Meade , M

    Churchwell , E., Babler , B. L., Meade , M. R., et al. 2009, , 121, 213, 10.1086/597811

    2009 doi

  29. [37]

    2023, arXiv e-prints, arXiv:2301.01388

    Comparat , J., Luo , W., Merloni , A., et al. 2023, arXiv e-prints, arXiv:2301.01388. 2301.01388

    2023 arXiv

  30. [38]

    R., Meyer , M

    Cottaar , M., Covey , K. R., Meyer , M. R., et al. 2014, , 794, 125, 10.1088/0004-637X/794/2/125

    2014 doi

  31. [39]

    Crumpler , N. R. 2025,

    2025

  32. [40]

    R., Chandra , V., Zakamska , N

    Crumpler , N. R., Chandra , V., Zakamska , N. L., et al. 2024, , 977, 237, 10.3847/1538-4357/ad8ddc

    2024 doi

  33. [41]

    M., Wright , E

    Cutri , R. M., Wright , E. L., Conrow , T., et al. 2013, Explanatory Supplement to the AllWISE Data Release Products , Tech. rep

    2013

  34. [42]

    S., Bessell , M

    da Costa , G. S., Bessell , M. S., Mackey , A. D., et al. 2023, VizieR Online Data Catalog: Extremely metal-poor stars in SkyMapper DR1.1 (Da+, 2019) , VizieR On-line Data Catalog: J/MNRAS/489/5900. Originally published in: 2019MNRAS.489.5900D

    2023

  35. [43]

    S., Schlegel , D

    Dawson , K. S., Schlegel , D. J., Ahn , C. P., et al. 2013, , 145, 10, 10.1088/0004-6256/145/1/10

    2013 doi

  36. [44]

    S., Kneib , J.-P., Percival , W

    Dawson , K. S., Kneib , J.-P., Percival , W. J., et al. 2016, , 151, 44, 10.3847/0004-6256/151/2/44

    2016 doi

  37. [45]

    G., Scuderi , S., et al

    Desidera , S., Gratton , R. G., Scuderi , S., et al. 2004, , 420, 683, 10.1051/0004-6361:20041242

    2004 doi

  38. [46]

    2025, Jdaviz , v4.2.1, Zenodo, 10.5281/zenodo.5513927

    Developers , J., Averbukh , J., Bradley , L., et al. 2025, Jdaviz , v4.2.1, Zenodo, 10.5281/zenodo.5513927

    2025 doi

  39. [47]

    J., Lang , D., et al

    Dey , A., Schlegel , D. J., Lang , D., et al. 2019, , 157, 168, 10.3847/1538-3881/ab089d

    2019 doi

  40. [48]

    R., Covey , K., et al

    Donor , J., Blanton , M. R., Covey , K., et al. 2024, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 13101, Software and Cyberinfrastructure for Astronomy VIII, ed. J. Ibsen & G. Chiozzi , 1310146, 10.1117/12.3020292

    2024 doi

  41. [49]

    M., Cunha , K., et al

    Donor , J., Frinchaboy , P. M., Cunha , K., et al. 2018, , 156, 142, 10.3847/1538-3881/aad635

    2018 doi

  42. [50]

    2020, , 159, 199, 10.3847/1538-3881/ab77bc

    ---. 2020, , 159, 199, 10.3847/1538-3881/ab77bc

    2020 doi

  43. [51]

    P., Norberg , P., Baldry , I

    Driver , S. P., Norberg , P., Baldry , I. K., et al. 2009, Astronomy and Geophysics, 50, 5.12, 10.1111/j.1468-4004.2009.50512.x

    2009

  44. [52]

    A., Kreckel , K., et al

    Drory , N., Blanc , G. A., Kreckel , K., et al. 2024, , 168, 198, 10.3847/1538-3881/ad6de9

    2024 doi

  45. [53]

    2024, astropy/specutils: v1.19.0 , v1.19.0, Zenodo, 10.5281/zenodo.14042033

    Earl , N., Tollerud , E., O'Steen , R., et al. 2024, astropy/specutils: v1.19.0 , v1.19.0, Zenodo, 10.5281/zenodo.14042033

    2024 doi

  46. [54]

    2024, , 685, A82, 10.1051/0004-6361/202347628

    Edenhofer , G., Zucker , C., Frank , P., et al. 2024, , 685, A82, 10.1051/0004-6361/202347628

    2024 doi

  47. [55]

    J., Liebert , J., Harris , H

    Eisenstein , D. J., Liebert , J., Harris , H. C., et al. 2006, , 167, 40, 10.1086/507110

    2006 doi

  48. [56]

    J., Weinberg , D

    Eisenstein , D. J., Weinberg , D. H., Agol , E., et al. 2011, , 142, 72, 10.1088/0004-6256/142/3/72

    2011 doi

  49. [57]

    N., Evans, J

    Evans, I. N., Evans, J. D., Martínez-Galarza, J. R., et al. 2024, The Astrophysical Journal Supplement Series, 274, 22, 10.3847/1538-4365/ad6319

    2024 doi

  50. [58]

    E., Winget , D

    Falcon , R. E., Winget , D. E., Montgomery , M. H., & Williams , K. A. 2010, , 712, 585, 10.1088/0004-637X/712/1/585

    2010 doi

  51. [59]

    G., Boch , T., et al

    Fernique , P., Allen , M. G., Boch , T., et al. 2015, , 578, A114, 10.1051/0004-6361/201526075

    2015 doi

  52. [60]

    Fitzpatrick , E. L. 1999, , 111, 63, 10.1086/316293

    1999 doi

  53. [61]

    A., Magnier , E

    Flewelling , H. A., Magnier , E. A., Chambers , K. C., et al. 2020, , 251, 7, 10.3847/1538-4365/abb82d

    2020 doi

  54. [62]

    C., & Schmitt , J

    Freund , S., Czesla , S., Robrade , J., Schneider , P. C., & Schmitt , J. H. M. M. 2022, , 664, A105, 10.1051/0004-6361/202142573

    2022 doi

  55. [63]

    2024, , 684, A121, 10.1051/0004-6361/202348278

    Freund , S., Czesla , S., Predehl , P., et al. 2024, , 684, A121, 10.1051/0004-6361/202348278

    2024 doi

  56. [64]

    A., Bassett , B., Becker , A., et al

    Frieman , J. A., Bassett , B., Becker , A., et al. 2008, , 135, 338, 10.1088/0004-6256/135/1/338

    2008 doi

  57. [65]

    B., Trump , J

    Fries , L. B., Trump , J. R., Davis , M. C., et al. 2023, , 948, 5, 10.3847/1538-4357/acbfb7

    2023 doi

  58. [66]

    B., Trump , J

    Fries , L. B., Trump , J. R., Horne , K., et al. 2024, , 975, 239, 10.3847/1538-4357/ad7c42

    2024 doi

  59. [67]

    Gaia Collaboration , Prusti , T., de Bruijne , J. H. J., et al. 2016, , 595, A1, 10.1051/0004-6361/201629272

    2016 doi

  60. [68]

    Gaia Collaboration , Brown, A. G. A. , Vallenari, A. , et al. 2018, A&A, 616, A1, 10.1051/0004-6361/201833051

    2018 doi

  61. [69]

    Gaia Collaboration , Brown , A. G. A., Vallenari , A., et al. 2021, , 649, A1, 10.1051/0004-6361/202039657

    2021 doi

  62. [70]

    2023, , 674, A40, 10.1051/0004-6361/202243283

    Gaia Collaboration , Schultheis , M., Zhao , H., et al. 2023, , 674, A40, 10.1051/0004-6361/202243283

    2023 doi

  63. [71]

    E., Allende Prieto , C., Holtzman , J

    Garc \' a P \'e rez , A. E., Allende Prieto , C., Holtzman , J. A., et al. 2016, , 151, 144, 10.3847/0004-6256/151/6/144

    2016 doi

  64. [72]

    2008, in Astronomical Society of the Pacific Conference Series, Vol

    Ge , J., Mahadevan , S., Lee , B., et al. 2008, in Astronomical Society of the Pacific Conference Series, Vol. 398, Extreme Solar Systems, ed. D. Fischer , F. A. Rasio , S. E. Thorsett , & A. Wolszczan , 449

    2008

  65. [73]

    P., Tremblay , P.-E., G \"a nsicke , B

    Gentile Fusillo , N. P., Tremblay , P.-E., G \"a nsicke , B. T., et al. 2019, , 482, 4570, 10.1093/mnras/sty3016

    2019 doi

  66. [74]

    P., Tremblay , P

    Gentile Fusillo , N. P., Tremblay , P. E., Cukanovaite , E., et al. 2021, , 508, 3877, 10.1093/mnras/stab2672

    2021 doi

  67. [75]

    E., & Pérez, F

    Granger, B. E., & Pérez, F. 2021, Computing in Science & Engineering, 23, 7, 10.1109/MCSE.2021.3059263

    2021

  68. [76]

    A., & Szalay , A

    Gray , J., Nieto-Santisteban , M. A., & Szalay , A. S. 2007, arXiv e-prints, cs/0701171, 10.48550/arXiv.cs/0701171

    2007 doi arXiv

  69. [78]

    2018 b , The Journal of Open Source Software, 3, 695, 10.21105/joss.00695

    ---. 2018 b , The Journal of Open Source Software, 3, 695, 10.21105/joss.00695

    2018 doi

  70. [79]

    M., Schlafly , E

    Green , G. M., Schlafly , E. F., Finkbeiner , D. P., et al. 2015, , 810, 25, 10.1088/0004-637X/810/1/25

    2015 doi

  71. [80]

    2018, PyQSOFit: Python code to fit the spectrum of quasars , Astrophysics Source Code Library, record ascl:1809.008

    Guo , H., Shen , Y., & Wang , S. 2018, PyQSOFit: Python code to fit the spectrum of quasars , Astrophysics Source Code Library, record ascl:1809.008. 1809.008

    2018

  72. [81]

    C., MacGillivray , H

    Hambly , N. C., MacGillivray , H. T., Read , M. A., et al. 2001, , 326, 1279, 10.1111/j.1365-2966.2001.04660.x

    2001

  73. [82]

    2020, , 492, 1164, 10.1093/mnras/stz3132

    Hawkins , K., Lucey , M., Ting , Y.-S., et al. 2020, , 492, 1164, 10.1093/mnras/stz3132

    2020 doi

  74. [83]

    Henry , R. B. C., Kwitter , K. B., & Dufour , R. J. 1999, , 517, 782, 10.1086/307215

    1999 doi

  75. [84]

    M., Bilgi , P., Bizenberger , P., et al

    Herbst , T. M., Bilgi , P., Bizenberger , P., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11445, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 114450J, 10.1117/12.2561419

    2020 doi

  76. [85]

    M., Bizenberger , P., Blanc , G

    Herbst , T. M., Bizenberger , P., Blanc , G. A., et al. 2024, , 168, 267, 10.3847/1538-3881/ad7948

    2024 doi

  77. [86]

    V., et al

    H g , E., Fabricius , C., Makarov , V. V., et al. 2000, , 355, L27

    2000

  78. [87]

    A., Hasselquist , S., Shetrone , M., et al

    Holtzman , J. A., Hasselquist , S., Shetrone , M., et al. 2018, , 156, 125, 10.3847/1538-3881/aad4f9

    2018 doi

  79. [88]

    Holtzman, W. H. 1950, The American Journal of Psychology, 63, 615. http://www.jstor.org/stable/1418879

    1950

  80. [89]

    2020, , 499, 4768, 10.1093/mnras/staa3044

    Ider Chitham , J., Comparat , J., Finoguenov , A., et al. 2020, , 499, 4768, 10.1093/mnras/staa3044

    2020 doi

  81. [90]

    Z., et al

    Inno , L., Rix , H.-W., Stanek , K. Z., et al. 2021, , 914, 127, 10.3847/1538-4357/abf940

    2021 doi

  82. [91]

    O., Pelisoli , I., Koester , D., et al

    Kepler , S. O., Pelisoli , I., Koester , D., et al. 2015, , 446, 4078, 10.1093/mnras/stu2388

    2015 doi

  83. [92]

    2016, , 455, 3413, 10.1093/mnras/stv2526

    ---. 2016, , 455, 3413, 10.1093/mnras/stv2526

    2016 doi

  84. [93]

    2019, , 486, 2169, 10.1093/mnras/stz960

    ---. 2019, , 486, 2169, 10.1093/mnras/stz960

    2019 doi

  85. [94]

    2018, , 616, L2, 10.1051/0004-6361/201833647

    Kimeswenger , S., & Barr \' a , D. 2018, , 616, L2, 10.1051/0004-6361/201833647

    2018 doi

  86. [95]

    J., et al

    Klein , M., Oguri , M., Mohr , J. J., et al. 2022, , 661, A4, 10.1051/0004-6361/202141123

    2022 doi

  87. [96]

    J., Harris , H

    Kleinman , S. J., Harris , H. C., Eisenstein , D. J., et al. 2004, , 607, 426, 10.1086/383464

    2004 doi

  88. [97]

    J., Kepler , S

    Kleinman , S. J., Kepler , S. O., Koester , D., et al. 2013, , 204, 5, 10.1088/0067-0049/204/1/5

    2013 doi

  89. [98]

    2009, , 505, 441, 10.1051/0004-6361/200912531

    Koester , D., Voss , B., Napiwotzki , R., et al. 2009, , 505, 441, 10.1051/0004-6361/200912531

    2009 doi

  90. [99]

    A., Zasowski , G., Rix , H.-W., et al

    Kollmeier , J. A., Zasowski , G., Rix , H.-W., et al. 2017, ArXiv e-prints. 1711.03234

    2017 arXiv

  91. [100]

    P., Herbst , T., Froning , C., et al

    Konidaris , N. P., Herbst , T., Froning , C., et al. 2024, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 13096, Ground-based and Airborne Instrumentation for Astronomy X, ed. J. J. Bryant , K. Motohara , & J. R. D. Vernet , 130961Z, 10.11...

    2024 doi

  92. [101]

    2022, PyXCSAO, 0.2, Zenodo, 10.5281/zenodo.6998993

    Kounkel, M. 2022, PyXCSAO, 0.2, Zenodo, 10.5281/zenodo.6998993

    2022 doi

  93. [102]

    2019, , 158, 122, 10.3847/1538-3881/ab339a

    Kounkel , M., & Covey , K. 2019, , 158, 122, 10.3847/1538-3881/ab339a

    2019 doi

  94. [104]

    2016 b , , 152, 83, 10.3847/0004-6256/152/4/83

    ---. 2016 b , , 152, 83, 10.3847/0004-6256/152/4/83

    2016 doi

  95. [105]

    R., Westfall , K

    Law , D. R., Westfall , K. B., Bershady , M. A., et al. 2021, , 161, 52, 10.3847/1538-3881/abcaa2

    2021 doi

  96. [106]

    W., & Bovy , J

    Leung , H. W., & Bovy , J. 2019, , 483, 3255, 10.1093/mnras/sty3217

    2019 doi

  97. [107]

    W., Bovy , J., Mackereth , J

    Leung , H. W., Bovy , J., Mackereth , J. T., & Miglio , A. 2023, , 522, 4577, 10.1093/mnras/stad1272

    2023 doi

  98. [108]

    W., Higley , A

    Lyke , B. W., Higley , A. N., McLane , J. N., et al. 2020, , 250, 8, 10.3847/1538-4365/aba623

    2020 doi

  99. [109]

    T., Bovy , J., Leung , H

    Mackereth , J. T., Bovy , J., Leung , H. W., et al. 2019, , 489, 176, 10.1093/mnras/stz1521

    2019 doi

  100. [110]

    A., Chambers , K

    Magnier , E. A., Chambers , K. C., Flewelling , H. A., et al. 2020, , 251, 3, 10.3847/1538-4365/abb829

    2020 doi

  101. [111]

    R., Schiavon , R

    Majewski , S. R., Schiavon , R. P., Frinchaboy , P. M., et al. 2017, , 154, 94, 10.3847/1538-3881/aa784d

    2017 doi

  102. [112]

    Marocco , F., Eisenhardt , P. R. M., Fowler , J. W., et al. 2021, , 253, 8, 10.3847/1538-4365/abd805

    2021 doi

  103. [113]

    2021, , 162, 282, 10.3847/1538-3881/ac2432

    McBride , A., Lingg , R., Kounkel , M., Covey , K., & Hutchinson , B. 2021, , 162, 282, 10.3847/1538-3881/ac2432

    2021 doi

  104. [114]

    G., Banerji , M., Gonzalez , E., et al

    McMahon , R. G., Banerji , M., Gonzalez , E., et al. 2013, The Messenger, 154, 35

    2013

  105. [115]

    M., Lang , D., Schlafly , E

    Meisner , A. M., Lang , D., Schlafly , E. F., & Schlegel , D. J. 2019, , 131, 124504, 10.1088/1538-3873/ab3df4

    2019 doi

  106. [116]

    2012, arXiv e-prints, arXiv:1209.3114

    Merloni , A., Predehl , P., Becker , W., et al. 2012, arXiv e-prints, arXiv:1209.3114. 1209.3114

    2012 arXiv

  107. [117]

    2024, , 682, A34, 10.1051/0004-6361/202347165

    Merloni , A., Lamer , G., Liu , T., et al. 2024, , 682, A34, 10.1051/0004-6361/202347165

    2024 doi

  108. [118]

    A., et al

    M \'e sz \'a ros , S., Jofr \'e , P., Johnson , J. A., et al. 2025, arXiv e-prints, arXiv:2506.07845, 10.48550/arXiv.2506.07845

    2025 doi arXiv

  109. [119]

    2022, , 164, 85, 10.3847/1538-3881/ac7ce5

    Myers , N., Donor , J., Spoo , T., et al. 2022, , 164, 85, 10.3847/1538-3881/ac7ce5

    2022 doi

  110. [120]

    Nandra , K., Waddell , S. G. H., Liu , T., et al. 2025, , 693, A212, 10.1051/0004-6361/202449416

    2025 doi

  111. [121]

    2021, , 921, 118, 10.3847/1538-4357/ac14be

    Nelson , T., Ting , Y.-S., Hawkins , K., et al. 2021, , 921, 118, 10.3847/1538-4357/ac14be

    2021 doi

  112. [122]

    W., Rix , H

    Ness , M., Hogg , D. W., Rix , H. W., Ho , A. Y. Q., & Zasowski , G. 2015, , 808, 16, 10.1088/0004-637X/808/1/16

    2015 doi

  113. [123]

    W., Hogg , D

    Ness , M., Rix , H. W., Hogg , D. W., et al. 2018, , 853, 198, 10.3847/1538-4357/aa9d8e

    2018 doi

  114. [124]

    2021, dnidever/doppler: Cannon and Payne models , v1.1.0, Zenodo, 10.5281/zenodo.4906681

    Nidever , D. 2021, dnidever/doppler: Cannon and Payne models , v1.1.0, Zenodo, 10.5281/zenodo.4906681

    2021 doi

  115. [125]

    L., Holtzman , J

    Nidever , D. L., Holtzman , J. A., Allende Prieto , C., et al. 2015, , 150, 173, 10.1088/0004-6256/150/6/173

    2015 doi

  116. [126]

    O'Dell , C. R. 1998, , 116, 1346, 10.1086/300506

    1998 doi

  117. [127]

    2020, , 159, 182, 10.3847/1538-3881/ab7a97

    Olney , R., Kounkel , M., Schillinger , C., et al. 2020, , 159, 182, 10.3847/1538-3881/ab7a97

    2020 doi

  118. [128]

    A., Wolf , C., Bessell , M

    Onken , C. A., Wolf , C., Bessell , M. S., et al. 2019, , 36, e033, 10.1017/pasa.2019.27

    2019 doi

  119. [129]

    J., Brindle , C., Talavera , A., et al

    Page , M. J., Brindle , C., Talavera , A., et al. 2012, , 426, 903, 10.1111/j.1365-2966.2012.21706.x

    2012

  120. [130]

    W., Derwent , M

    Pogge , R. W., Derwent , M. A., O'Brien , T. P., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11447, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 1144781, 10.1117/12.2561113

    2020 doi

  121. [131]

    2021, , 647, A1, 10.1051/0004-6361/202039313

    Predehl , P., Andritschke , R., Arefiev , V., et al. 2021, , 647, A1, 10.1051/0004-6361/202039313

    2021 doi

  122. [132]

    2001, , 369, 1048, 10.1051/0004-6361:20010163

    Prugniel , P., & Soubiran , C. 2001, , 369, 1048, 10.1051/0004-6361:20010163

    2001 doi

  123. [133]

    Queiroz , A. B. A., Anders , F., Santiago , B. X., et al. 2018, , 476, 2556, 10.1093/mnras/sty330

    2018 doi

  124. [134]

    Queiroz , A. B. A., Anders , F., Chiappini , C., et al. 2020, , 638, A76, 10.1051/0004-6361/201937364

    2020 doi

  125. [135]

    2023, , 673, A155, 10.1051/0004-6361/202245399

    ---. 2023, , 673, A155, 10.1051/0004-6361/202245399

    2023 doi

  126. [136]

    2022, , 658, A22, 10.1051/0004-6361/202141837

    Raddi , R., Torres , S., Rebassa-Mansergas , A., et al. 2022, , 658, A22, 10.1051/0004-6361/202141837

    2022 doi

  127. [137]

    2024, , 974, 153, 10.3847/1538-4357/ad6e76

    Ren , W., Guo , H., Shen , Y., et al. 2024, , 974, 153, 10.3847/1538-4357/ad6e76

    2024 doi

  128. [138]

    T., Lacy , M., Storrie-Lombardi , L

    Richards , G. T., Lacy , M., Storrie-Lombardi , L. J., et al. 2006, , 166, 470, 10.1086/506525

    2006 doi

  129. [139]

    R., Winn , J., & Vanderspek , R

    Ricker , G. R., Winn , J., & Vanderspek , R. 2022, in Bulletin of the American Astronomical Society, Vol. 54, 406.02

    2022

  130. [140]

    M., Lee , Y

    Rockosi , C. M., Lee , Y. S., Morrison , H. L., et al. 2022, , 259, 60, 10.3847/1538-4365/ac5323

    2022 doi

  131. [141]

    2024, , 692, A260, 10.1051/0004-6361/202452361

    Roster , W., Salvato , M., Krippendorf , S., et al. 2024, , 692, A260, 10.1051/0004-6361/202452361

    2024 doi

  132. [142]

    S., Rozo , E., Busha , M

    Rykoff , E. S., Rozo , E., Busha , M. T., et al. 2014, , 785, 104, 10.1088/0004-637X/785/2/104

    2014 doi

  133. [143]

    2024, , 167, 125, 10.3847/1538-3881/ad2001

    Saad , S., Lane , K., Kounkel , M., et al. 2024, , 167, 125, 10.3847/1538-3881/ad2001

    2024 doi

  134. [144]

    2022, , 661, A3, 10.1051/0004-6361/202141631

    Salvato , M., Wolf , J., Dwelly , T., et al. 2022, , 661, A3, 10.1051/0004-6361/202141631

    2022 doi

  135. [145]

    F., Mej \' a-Narv \'a ez , A., Egorov , O

    S \'a nchez , S. F., Mej \' a-Narv \'a ez , A., Egorov , O. V., et al. 2025, , 169, 52, 10.3847/1538-3881/ad93bb

    2025 doi

  136. [146]

    2024, , 690, A365, 10.1051/0004-6361/202450886

    Saxena , A., Salvato , M., Roster , W., et al. 2024, , 690, A365, 10.1051/0004-6361/202450886

    2024 doi

  137. [147]

    K., Uzsoy , A

    Saydjari , A. K., Uzsoy , A. S. M., Zucker , C., Peek , J. E. G., & Finkbeiner , D. P. 2023, , 954, 141, 10.3847/1538-4357/acd454

    2023 doi

  138. [148]

    K., Finkbeiner , D

    Saydjari , A. K., Finkbeiner , D. P., Wheeler , A. J., et al. 2025, , 169, 167, 10.3847/1538-3881/adb02d

    2025 doi

  139. [149]

    F., & Finkbeiner , D

    Schlafly , E. F., & Finkbeiner , D. P. 2011, , 737, 103, 10.1088/0004-637X/737/2/103

    2011 doi

  140. [150]

    F., Meisner, A

    Schlafly, E. F., Meisner, A. M., & Green, G. M. 2019, The Astrophysical Journal Supplement Series, 240, 30, 10.3847/1538-4365/aafbea

    2019 doi

  141. [151]

    C., & Casey , A

    Schlaufman , K. C., & Casey , A. R. 2014, , 797, 13, 10.1088/0004-637X/797/1/13

    2014 doi

  142. [152]

    J., Finkbeiner , D

    Schlegel , D. J., Finkbeiner , D. P., & Davis , M. 1998, , 500, 525, 10.1086/305772

    1998 doi

  143. [153]

    P., Richards , G

    Schneider , D. P., Richards , G. T., Hall , P. B., et al. 2010, , 139, 2360, 10.1088/0004-6256/139/6/2360

    2010 doi

  144. [154]

    2024, , 686, A110, 10.1051/0004-6361/202348426

    Schwope , A., Kurpas , J., Baecke , P., et al. 2024, , 686, A110, 10.1051/0004-6361/202348426

    2024 doi

  145. [155]

    T., Strauss , M

    Shen , Y., Richards , G. T., Strauss , M. A., et al. 2011, , 194, 45, 10.1088/0067-0049/194/2/45

    2011 doi

  146. [156]

    N., Dawson , K

    Shen , Y., Brandt , W. N., Dawson , K. S., et al. 2015, , 216, 4, 10.1088/0067-0049/216/1/4

    2015 doi

  147. [157]

    N., Richards , G

    Shen , Y., Brandt , W. N., Richards , G. T., et al. 2016, , 831, 7, 10.3847/0004-637X/831/1/7

    2016 doi

  148. [158]

    B., Horne , K., et al

    Shen , Y., Hall , P. B., Horne , K., et al. 2019, , 241, 34, 10.3847/1538-4365/ab074f

    2019 doi

  149. [159]

    J., Horne , K., et al

    Shen , Y., Grier , C. J., Horne , K., et al. 2024, , 272, 26, 10.3847/1538-4365/ad3936

    2024 doi

  150. [160]

    E., Evans , N

    Shu , Y., Koposov , S. E., Evans , N. W., et al. 2019, , 489, 4741, 10.1093/mnras/stz2487

    2019 doi

  151. [161]

    2024, , 167, 173, 10.3847/1538-3881/ad291d

    Sizemore , L., Llanes , D., Kounkel , M., et al. 2024, , 167, 173, 10.3847/1538-3881/ad291d

    2024 doi

  152. [162]

    F., Cutri, R

    Skrutskie, M. F., Cutri, R. M., Stiening, R., et al. 2006, The Astronomical Journal, 131, 1163, 10.1086/498708

    2006 doi

  153. [164]

    2013 b , , 146, 32, 10.1088/0004-6256/146/2/32

    ---. 2013 b , , 146, 32, 10.1088/0004-6256/146/2/32

    2013 doi

  154. [165]

    2021, Nature Astronomy, 5, 1163, 10.1038/s41550-021-01451-8

    Spina , L., Sharma , P., Mel \'e ndez , J., et al. 2021, Nature Astronomy, 5, 1163, 10.1038/s41550-021-01451-8

    2021 doi

  155. [166]

    2022, , 163, 152, 10.3847/1538-3881/ac4de7

    Sprague , D., Culhane , C., Kounkel , M., et al. 2022, , 163, 152, 10.3847/1538-3881/ac4de7

    2022 doi

  156. [167]

    G., Oelkers , R

    Stassun , K. G., Oelkers , R. J., Paegert , M., et al. 2019, , 158, 138, 10.3847/1538-3881/ab3467

    2019 doi

  157. [168]

    F., et al

    Stone , Z., Shen , Y., Anderson , S. F., et al. 2024, arXiv e-prints, arXiv:2408.04789, 10.48550/arXiv.2408.04789

    2024 doi arXiv

  158. [169]

    A., Imig , J., et al

    Stone-Martinez , A., Holtzman , J. A., Imig , J., et al. 2024, , 167, 73, 10.3847/1538-3881/ad12a6

    2024 doi

  159. [170]

    A., Yuxi , et al

    Stone-Martinez , A., Holtzman , J. A., Yuxi , et al. 2025, arXiv e-prints, arXiv:2503.03138, 10.48550/arXiv.2503.03138

    2025 doi arXiv

  160. [171]

    2021, , 656, A132, 10.1051/0004-6361/202141179

    Sunyaev , R., Arefiev , V., Babyshkin , V., et al. 2021, , 656, A132, 10.1051/0004-6361/202141179

    2021 doi

  161. [172]

    2025, 10.5281/zenodo.15304237

    Taghizadeh-Popp, M. 2025, 10.5281/zenodo.15304237

    2025 doi

  162. [173]

    2023, SQLxMatch: In-Database Spatial Cross-Match of Astronomical Catalogs, v1.2.0, Zenodo, 10.5281/zenodo.10160988

    Taghizadeh-Popp, M., & Dobos, L. 2023, SQLxMatch: In-Database Spatial Cross-Match of Astronomical Catalogs, v1.2.0, Zenodo, 10.5281/zenodo.10160988

    2023 doi

  163. [174]

    W., Lemson , G., et al

    Taghizadeh-Popp , M., Kim , J. W., Lemson , G., et al. 2020, Astronomy and Computing, 33, 100412, 10.1016/j.ascom.2020.100412

    2020

  164. [175]

    2019, , 879, 69, 10.3847/1538-4357/ab2331

    Ting , Y.-S., Conroy , C., Rix , H.-W., & Cargile , P. 2019, , 879, 69, 10.3847/1538-4357/ab2331

    2019 doi

  165. [176]

    E., Ludwig , H

    Tremblay , P. E., Ludwig , H. G., Steffen , M., & Freytag , B. 2013, , 559, A104, 10.1051/0004-6361/201322318

    2013 doi

  166. [177]

    Uzsoy , A. S. M., Saydjari , A. K., Dey , A., et al. 2025, arXiv e-prints, arXiv:2504.06870, 10.48550/arXiv.2504.06870

    2025 doi

  167. [178]

    van Dokkum , P. G. 2001, , 113, 1420, 10.1086/323894

    2001 doi

  168. [179]

    Vestergaard , M., & Peterson , B. M. 2006, , 641, 689, 10.1086/500572

    2006 doi

  169. [180]

    Waddell , S. G. H., Nandra , K., Buchner , J., et al. 2024, , 690, A132, 10.1051/0004-6361/202245572

    2024 doi

  170. [181]

    L., Henden , A

    Watson , C. L., Henden , A. A., & Price , A. 2006, Society for Astronomical Sciences Annual Symposium, 25, 47

    2006

  171. [183]

    2019 b , , 158, 231, 10.3847/1538-3881/ab44a2

    ---. 2019 b , , 158, 231, 10.3847/1538-3881/ab44a2

    2019 doi

  172. [184]

    J., Hall , P

    Wheatley , R., Grier , C. J., Hall , P. B., et al. 2024, , 968, 49, 10.3847/1538-4357/ad429e

    2024 doi

  173. [185]

    C., Hearty , F

    Wilson , J. C., Hearty , F. R., Skrutskie , M. F., et al. 2019, , 131, 055001, 10.1088/1538-3873/ab0075

    2019 doi

  174. [186]

    2022, , 263, 42, 10.3847/1538-4365/ac9ead

    Wu , Q., & Shen , Y. 2022, , 263, 42, 10.3847/1538-4365/ac9ead

    2022 doi

  175. [187]

    2019, , 883, 175, 10.3847/1538-4357/ab3ebc

    Yan , R., Chen , Y., Lazarz , D., et al. 2019, , 883, 175, 10.3847/1538-4357/ab3ebc

    2019 doi

  176. [188]

    2022, arXiv e-prints, arXiv:2206.08989

    Yang , Q., & Shen , Y. 2022, arXiv e-prints, arXiv:2206.08989. 2206.08989

    2022 arXiv

  177. [189]

    2023, The Astrophysical Journal Supplement Series, 264, 9, 10.3847/1538-4365/ac9ea8

    Yang, Q., & Shen, Y. 2023, The Astrophysical Journal Supplement Series, 264, 9, 10.3847/1538-4365/ac9ea8

    2023 doi

  178. [190]

    J., et al

    Yanny , B., Rockosi , C., Newberg , H. J., et al. 2009, , 137, 4377, 10.1088/0004-6256/137/5/4377

    2009 doi

  179. [191]

    Yershov , V. N. 2014, , 354, 97, 10.1007/s10509-014-1944-5

    2014 doi

  180. [193]

    2000 b , , 120, 1579, 10.1086/301513

    ---. 2000 b , , 120, 1579, 10.1086/301513

    2000 doi

  181. [194]

    Zari , E., Hashemi , H., Brown , A. G. A., Jardine , K., & de Zeeuw , P. T. 2018, , 620, A172, 10.1051/0004-6361/201834150

    2018 doi

  182. [195]

    E., Chojnowski, S

    Zasowski, G., Cohen, R. E., Chojnowski, S. D., et al. 2017, AJ, 154, 198. http://stacks.iop.org/1538-3881/154/i=5/a=198

    2017

  183. [196]

    2022, , 939, L16, 10.3847/2041-8213/ac9a47

    Zeltyn , G., Trakhtenbrot , B., Eracleous , M., et al. 2022, , 939, L16, 10.3847/2041-8213/ac9a47

    2022 doi

  184. [197]

    2024, , 966, 85, 10.3847/1538-4357/ad2f30

    ---. 2024, , 966, 85, 10.3847/1538-4357/ad2f30

    2024 doi

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.