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arxiv: 2205.10939 · v1 · submitted 2022-05-22 · 🌌 astro-ph.IM · astro-ph.CO

Recognition: no theorem link

Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument

B. Abareshi , J. Aguilar , S. Ahlen , Shadab Alam , David M. Alexander , R. Alfarsy , L. Allen , C. Allende Prieto
show 259 more authors
O. Alves J.Ameel E. Armengaud J. Asorey Alejandro Aviles S. Bailey A. Balaguera-Antol\'inez O. Ballester C. Baltay A. Bault S. F. Beltran B. Benavides S. BenZvi A. Berti R. Besuner Florian Beutler D. Bianchi C. Blake P. Blanc R. Blum A. Bolton S. Bose D. Bramall S. Brieden A. Brodzeller D. Brooks C. Brownewell E. Buckley-Geer R. N. Cahn Z. Cai R. Canning A. Carnero Rosell P. Carton R. Casas F.J. Castander J.L. Cervantes-Cota S. Chabanier E. Chaussidon C. Chuang C. Circosta S. Cole A.P. Cooper L. da Costa M.-C. Cousinou A. Cuceu T. M. Davis K. Dawson R. de la Cruz-Noriega A. de la Macorra A. de Mattia J. Della Costa P. Demmer M. Derwent A. Dey B. Dey G. Dhungana Z. Ding C. Dobson P. Doel J. Donald-McCann J. Donaldson K. Douglass Y. Duan P. Dunlop J. Edelstein S. Eftekharzadeh D. J. Eisenstein M. Enriquez-Vargas S. Escoffier M. Evatt P. Fagrelius X. Fan K. Fanning V. A. Fawcett S. Ferraro J. Ereza B. Flaugher A. Font-Ribera J. E. Forero-Romero C. S. Frenk S. Fromenteau B.T. G\"ansicke C. Garcia-Quintero L. Garrison E. Gazta\~naga F. Gerardi H. Gil-Mar\'in S. Gontcho A Gontcho Alma X. Gonzalez-Morales G. Gonzalez-de-Rivera V. Gonzalez-Perez C. Gordon O. Graur D. Green C. Grove D. Gruen G. Gutierrez J. Guy C. Hahn S. Harris D. Herrera Hiram K. Herrera-Alcantar K. Honscheid C. Howlett D. Huterer V. Ir\v{s}i\v{c} M. Ishak P. Jelinsky L. Jiang J. Jimenez Y.P. Jing R. Joyce E. Jullo S. Juneau N.G. Kara\c{c}ayl{\i} M. Karamanis A. Karcher T. Karim R. Kehoe S. Kent D. Kirkby T. Kisner F. Kitaura S. E. Koposov A. Kov\'acs A. Kremin Alex Krolewski B. L'Huillier O. Lahav A. Lambert C. Lamman Ting-Wen Lan M. Landriau S. Lane D. Lang J. U. Lange J. Lasker L. Le Guillou A. Leauthaud A. Le Van Suu Michael E. Levi T. S. Li C. Magneville M. Manera Christopher J. Manser B. Marshall W. McCollam P. McDonald Aaron M. Meisner J. Mena-Fern\'andez M. Mezcua T. Miller R. Miquel P. Montero-Camacho J. Moon J. Paul Martini J. Meneses-Rizo J. Moustakas E. Mueller Andrea Mu\~noz-Guti\'errez Adam D. Myers S. Nadathur J. Najita L. Napolitano E. Neilsen Jeffrey A. Newman J.D.Nie Y. Ning G. Niz P. Norberg Hern\'an E. Noriega T. O'Brien A. Obuljen N. Palanque-Delabrouille A. Palmese P. Zhiwei D. Pappalardo X. Peng W.J. Percival S. Perruchot R. Pogge C. Poppett A. Porredon F. Prada J. Prochaska R. Pucha A. P\'erez-Fern\'andez I. P\'erez-R\'afols D. Rabinowitz A. Raichoor S. Ramirez-Solano C\'esar Ram\'irez-P\'erez C. Ravoux K. Reil M. Rezaie A. Rocher C. Rockosi N.A. Roe A. Roodman A. J. Ross G. Rossi R. Ruggeri V. Ruhlmann-Kleider C. G. Sabiu S. Safonova K. Said A. Saintonge Javier Salas Catonga L. Samushia E. Sanchez C. Saulder E. Schaan E. Schlafly D. Schlegel J. Schmoll D. Scholte M. Schubnell A. Secroun H. Seo S. Serrano Ray M. Sharples Michael J. Sholl Joseph Harry Silber D. R. Silva M. Sirk M. Siudek A. Smith D. Sprayberry R. Staten B. Stupak T. Tan Gregory Tarl\'e Suk Sien Tie R. Tojeiro L. A. Ure\~na-L\'opez F. Valdes O. Valenzuela M. Valluri M. Vargas-Maga\~na L. Verde M. Walther B. Wang M. S. Wang B. A. Weaver C. Weaverdyck R. Wechsler Michael J. Wilson J. Yang Y. Yu S. Yuan Christophe Y\`eche H. Zhang K. Zhang Cheng Zhao Rongpu Zhou Zhimin Zhou H. Zou J. Zou S. Zou Y. Zu (DESI Collaboration)
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Pith reviewed 2026-05-17 07:02 UTC · model grok-4.3

classification 🌌 astro-ph.IM astro-ph.CO
keywords Dark Energy Spectroscopic InstrumentDESIfiber positionersspectrographsinstrumentationprime focus correctorMayall telescopedark energy survey
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The pith

DESI has installed and validated its wide-field corrector, 5020 robotic fiber positioners, and ten spectrographs, achieving all required performance metrics for the dark energy survey.

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

The paper provides an overview of the instrumentation developed for the Dark Energy Spectroscopic Instrument survey. It explains the design of the prime focus corrector, the division of 5020 positioners into ten petals connected by fiber bundles to spectrographs covering 360-980 nm, and the facility upgrades at the Mayall telescope. The authors detail how the system was installed and commissioned, reporting that it meets or exceeds the science requirements with specific accuracy and sensitivity measurements. A sympathetic reader would care because this instrumentation is what makes possible the collection of spectra from tens of millions of galaxies to map the universe's expansion and structure growth. The description includes key successes and lessons from managing such a large project.

Core claim

The DESI instrument features a 3.2-degree wide-field prime-focus corrector that focuses light onto an 0.812 m aspheric focal surface populated with 5020 robotic fiber positioners arranged in ten wedge-shaped petals. Each petal connects via a 50 m fiber bundle to one of ten spectrographs, each splitting light into three channels for the 360-980 nm range with resolutions of 2000-5000. On-sky validation shows the positioners achieve RMS accuracy better than 0.1 arcsec, with signal-to-noise ratios meeting targets for high-redshift quasars and emission-line galaxies at z around 1.5. The survey, which began in May 2021, is now using this setup to measure redshifts for 40 million objects and probe暗

What carries the argument

The array of 5020 robotic fiber positioners on the aspheric focal surface, which precisely place fibers to capture light from targeted galaxies and quasars for multi-object spectroscopy.

If this is right

  • The system supports precise redshift measurements for 40 million galaxies and quasars over five years.
  • This allows mapping of baryon acoustic oscillations to measure cosmic distances up to redshift greater than 3.5.
  • Growth of structure measurements can test modifications to general relativity.
  • The successful commissioning confirms the instrument is ready for sustained survey operations starting in 2021.

Where Pith is reading between the lines

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

  • Performance at this scale could inform designs for even larger future spectroscopic facilities on similar telescopes.
  • The reported on-sky metrics set quantitative benchmarks that other multi-object spectrographs can be compared against directly.
  • If the fiber positioning and spectrograph stability hold, the survey will produce a dataset large enough to distinguish between competing dark energy models at the percent level.

Load-bearing premise

The performance metrics observed during commissioning will remain stable over the full five-year duration of the survey without degradation from factors like wear, temperature variations, or operational issues.

What would settle it

A follow-up observation campaign after two years of survey operations showing positioner accuracy worse than 0.1 arcsec RMS or SNR values below the reported thresholds for the specified targets.

read the original abstract

The Dark Energy Spectroscopic Instrument (DESI) has embarked on an ambitious five-year survey to explore the nature of dark energy with spectroscopy of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the Baryon Acoustic Oscillation method to measure distances from the nearby universe to z > 3.5, as well as measure the growth of structure and probe potential modifications to general relativity. In this paper we describe the significant instrumentation we developed for the DESI survey. The new instrumentation includes a wide-field, 3.2-deg diameter prime-focus corrector that focuses the light onto 5020 robotic fiber positioners on the 0.812 m diameter, aspheric focal surface. The positioners and their fibers are divided among ten wedge-shaped petals. Each petal is connected to one of ten spectrographs via a contiguous, high-efficiency, nearly 50 m fiber cable bundle. The ten spectrographs each use a pair of dichroics to split the light into three channels that together record the light from 360 - 980 nm with a resolution of 2000 to 5000. We describe the science requirements, technical requirements on the instrumentation, and management of the project. DESI was installed at the 4-m Mayall telescope at Kitt Peak, and we also describe the facility upgrades to prepare for DESI and the installation and functional verification process. DESI has achieved all of its performance goals, and the DESI survey began in May 2021. Some performance highlights include RMS positioner accuracy better than 0.1", SNR per \sqrt{\AA} > 0.5 for a z > 2 quasar with flux 0.28e-17 erg/s/cm^2/A at 380 nm in 4000s, and median SNR = 7 of the [OII] doublet at 8e-17 erg/s/cm^2 in a 1000s exposure for emission line galaxies at z = 1.4 - 1.6. We conclude with highlights from the on-sky validation and commissioning of the instrument, key successes, and lessons learned. (abridged)

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 2 minor

Summary. This manuscript provides an overview of the DESI instrumentation developed for a five-year spectroscopic survey of 40 million galaxies and quasars. It details the 3.2-deg prime-focus corrector, 5020 robotic fiber positioners on ten petals connected via fiber bundles to ten spectrographs (360-980 nm, R=2000-5000), facility upgrades at the Mayall 4-m telescope, installation, and functional verification. The central claim is that DESI has achieved all performance goals, evidenced by on-sky commissioning metrics: RMS positioner accuracy better than 0.1 arcsec, SNR per sqrt(Å) > 0.5 for a z>2 quasar with flux 0.28e-17 erg/s/cm²/Å at 380 nm in 4000 s, and median SNR=7 for the [OII] doublet at 8e-17 erg/s/cm² in 1000 s for ELGs at z=1.4-1.6. The survey began in May 2021.

Significance. If the reported commissioning metrics hold, this represents a major instrumentation achievement enabling precise BAO and growth-of-structure measurements for dark energy studies. The quantitative performance metrics and description of technical requirements, verification, and lessons learned provide valuable documentation for the field and future large-scale projects.

major comments (1)
  1. [On-sky validation and commissioning] On-sky validation and commissioning section: The performance metrics (RMS accuracy <0.1 arcsec, quasar SNR >0.5, ELG [OII] SNR=7) are presented as evidence that all goals are met. However, these derive from initial commissioning snapshots; the manuscript provides no repeated measurements, degradation rates, or models for fiber stress, positioner motor wear, or thermal cycling effects over the planned five-year operations at Kitt Peak. This leaves the transition from commissioning achievement to sustained survey performance as an untested assumption.
minor comments (2)
  1. [Abstract] Abstract: The performance highlights lack associated uncertainties or error analysis details; these should be expanded in the main text for full traceability to the quantitative claims.
  2. [Requirements and verification sections] Requirements and verification sections: Adding explicit cross-references between each stated technical requirement and the corresponding verification result or table would improve clarity and auditability.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their positive assessment of the manuscript and for the constructive comment on long-term performance. We address the point below and clarify the intended scope of this instrumentation overview paper.

read point-by-point responses

  1. Referee: [On-sky validation and commissioning] On-sky validation and commissioning section: The performance metrics (RMS accuracy <0.1 arcsec, quasar SNR >0.5, ELG [OII] SNR=7) are presented as evidence that all goals are met. However, these derive from initial commissioning snapshots; the manuscript provides no repeated measurements, degradation rates, or models for fiber stress, positioner motor wear, or thermal cycling effects over the planned five-year operations at Kitt Peak. This leaves the transition from commissioning achievement to sustained survey performance as an untested assumption.

    Authors: We agree that sustained performance over five years is essential for the survey's success. This manuscript is an overview of the DESI instrumentation, its technical requirements, design, installation at the Mayall telescope, and the results of initial on-sky commissioning and functional verification. The quoted metrics demonstrate that the instrument met all performance goals at the conclusion of commissioning, enabling the survey to begin in May 2021. Repeated measurements, degradation monitoring, and models for fiber stress, motor wear, or thermal effects require multi-year operational data that were not yet available when the paper was prepared. Such analyses are part of ongoing survey operations and will appear in future publications. The instrument design includes provisions for regular maintenance and monitoring to address these effects, and early survey data have shown stable performance consistent with commissioning results. We will add a brief clarifying sentence in the commissioning section to explicitly note the distinction between initial verification and long-term monitoring. revision: partial

Circularity Check

0 steps flagged

No circularity; claims rest on direct engineering measurements and commissioning reports

full rationale

The paper is an instrumentation overview describing hardware design, facility upgrades, installation, and on-sky validation for DESI. Performance claims (RMS positioner accuracy <0.1 arcsec, specific SNR thresholds for quasars and ELGs) are presented as empirical results from commissioning tests and functional verification, not as outputs of equations, models, or derivations that reduce to the inputs by construction. No self-definitional steps, fitted parameters called predictions, or load-bearing self-citation chains appear in the reported chain from requirements to achieved metrics. The central assertions are externally falsifiable via the cited on-sky data and do not rely on renaming or smuggling ansatzes. This is a standard self-contained technical report.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The central claims rest on standard assumptions from astronomical instrumentation engineering and project management; no free parameters, invented entities, or ad-hoc axioms are introduced beyond established practices for telescope systems.

pith-pipeline@v0.9.0 · 7179 in / 1165 out tokens · 58541 ms · 2026-05-17T07:02:53.749422+00:00 · methodology

discussion (0)

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Forward citations

Cited by 18 Pith papers

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

  1. Measurement of the galaxy-velocity power spectrum of DESI tracers with the kinematic Sunyaev-Zeldovich effect using DESI DR2 and ACT DR6

    astro-ph.CO 2026-04 unverdicted novelty 7.0

    DESI DR2 and ACT DR6 data yield 17σ LRG-velocity, 8.3σ ELG-velocity, and 6.8σ QSO-velocity detections plus a 3.1σ velocity-velocity signal, producing f_NL^loc = 15.9_{-34.4}^{+34.6} from the velocity field.

  2. Cosmological analysis of the DESI DR1 Lyman alpha 1D power spectrum

    astro-ph.CO 2026-01 unverdicted novelty 7.0

    DESI DR1 Lyman-alpha data yields Δ²★=0.379±0.032 and n★=-2.309±0.019 at k★=0.009 km⁻¹s and z=3, sharpening N_eff, α_s, and β_s constraints by factors of 1.18-1.90 when combined with other probes.

  3. DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints

    astro-ph.CO 2025-03 accept novelty 7.0

    DESI DR2 BAO data exhibits 2.3 sigma tension with CMB in Lambda-CDM but prefers evolving dark energy (w0 > -1, wa < 0) at 3.1 sigma with CMB and 2.8-4.2 sigma when including supernovae.

  4. DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations

    astro-ph.CO 2024-04 accept novelty 7.0

    First-year DESI BAO data are consistent with flat LambdaCDM and, when combined with CMB, show a 2.5-3.9 sigma preference for evolving dark energy (w0 > -1, wa < 0) that strengthens with certain supernova datasets.

  5. DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars

    astro-ph.CO 2024-04 accept novelty 7.0

    DESI measures BAO scales in six redshift bins with 0.52% combined precision using 5.7 million objects, detecting the signal at up to 9.1 sigma and finding larger scales than Planck LCDM at z<0.8.

  6. Precision Kinematic Sunyaev--Zel'dovich Measurements Across Halo Mass and Redshift with DESI DR2 and ACT DR6: Part I. Luminous Red Galaxies

    astro-ph.CO 2026-04 unverdicted novelty 6.0

    High-significance kSZ measurements around LRGs show gas is redistributed beyond gravitational collapse and imply more efficient feedback in group-scale halos than in standard hydrodynamical models.

  7. Into the Gompverse: A robust Gompertzian reionization model for CMB analyses

    astro-ph.CO 2026-04 unverdicted novelty 6.0

    A Gompertzian reionization model with three nuisance parameters demotes optical depth to a derived quantity, reducing its uncertainty by a factor of three and revealing potential neutrino mass tension in CMB analyses.

  8. DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements

    astro-ph.CO 2024-11 accept novelty 6.0

    DESI DR1 full-shape clustering yields Ω_m = 0.2962 ± 0.0095 and σ_8 = 0.842 ± 0.034 in flat ΛCDM, tightening to H_0 = 68.40 ± 0.27 km/s/Mpc with CMB and DESY3, while favoring w_0 > -1, w_a < 0 and limiting neutrino ma...

  9. DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars

    astro-ph.CO 2024-11 accept novelty 6.0

    DESI DR1 full-shape galaxy clustering constrains Omega_m = 0.296 ± 0.010, H0 = 68.63 ± 0.79 km/s/Mpc, and sigma_8 = 0.841 ± 0.034, consistent with LambdaCDM and Planck.

  10. FolpsD: combining EFT and phenomenological approaches for joint power spectrum and bispectrum analyses

    astro-ph.CO 2026-04 conditional novelty 5.0

    FolpsD combines EFT power spectrum and tree-level bispectrum with damping to enable joint analyses that improve cosmological constraints from DESI-like galaxy mocks by up to 30% on As and omega_cdm while extending the...

  11. Local primordial non-Gaussianity using cross-correlations of DESI tracers

    astro-ph.CO 2026-04 conditional novelty 5.0

    Cross-correlating LRG and QSO samples in DESI DR1 yields f_NL^loc = 2.1 with 68% uncertainties of +8.8 and -8.3, an incremental improvement over auto-correlations alone.

  12. Constraints on Neutrino Physics from DESI DR2 BAO and DR1 Full Shape

    astro-ph.CO 2025-03 conditional novelty 5.0

    DESI DR2 BAO and full-shape data plus CMB yield ∑m_ν < 0.0642 eV (95% CL) under ΛCDM, in 3σ tension with oscillation lower limits, relaxed to <0.163 eV in w0waCDM.

  13. From Large Telescopes to the MUltiplexed Survey Telescope (MUST)

    astro-ph.IM 2026-05 unverdicted novelty 4.0

    MUST is a new 6.5 m telescope designed to deliver simultaneous optical spectra for over 20,000 targets across a 5 deg² field, enabling the largest 3D spectroscopic map of the Universe with redshifts for more than 100 ...

  14. Testing Scale-Dependent Modified Gravity with DESI DR1

    astro-ph.CO 2026-04 accept novelty 4.0

    DESI DR1 constrains the modified gravity parameter to log10 |f_R0| < -4.59 at 95% CL, implying no detectable fifth force on scales below about 18 Mpc.

  15. Cosmic Shear constraints from HSC Year 3 with clustering calibration of the tomographic redshift distributions from DESI

    astro-ph.CO 2025-11 unverdicted novelty 4.0

    Reanalysis of HSC Y3 cosmic shear with DESI clustering redshift calibration yields S8 = 0.805 ± 0.018, a 1.8× error reduction and upward shift toward Planck cosmology.

  16. Extended Dark Energy analysis using DESI DR2 BAO measurements

    astro-ph.CO 2025-03 conditional novelty 4.0

    Extended analysis of DESI DR2 data confirms robust evidence for dynamical dark energy with phantom crossing preference, stable under parametric and non-parametric modeling.

  17. DESI DR2 Results I: Baryon Acoustic Oscillations from the Lyman Alpha Forest

    astro-ph.CO 2025-03 accept novelty 4.0

    DESI DR2 delivers 0.65% precision BAO measurements from the LyA forest at z_eff=2.33, with D_H/r_d = 8.632 ± 0.098 ± 0.026 and D_M/r_d = 38.99 ± 0.52 ± 0.12.

  18. Machine Learning Techniques for Astrophysics and Cosmology: Photometric Redshifts

    astro-ph.IM 2026-05 unverdicted novelty 3.0

    AI techniques for photometric redshift estimation have converged and are now limited by the size, systematics, and selection effects in spectroscopic training samples rather than by methodology.

Reference graph

Works this paper leans on

81 extracted references · 81 canonical work pages · cited by 18 Pith papers · 5 internal anchors

  1. [1]

    2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Abareshi, B., Williams, D., & Marshall, R. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10707, Software and Cyberinfrastructure for Astronomy V, ed. J. C. Guzman & J. Ibsen, 107071J, doi: 10.1117/12.2313194

    work page doi:10.1117/12.2313194 2018

  2. [2]

    2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Abareshi, B., Marshall, R., Gott, S., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9913, Software and Cyberinfrastructure for Astronomy IV, ed. G. Chiozzi & J. C. Guzman, 99131O, doi: 10.1117/12.2233087

    work page doi:10.1117/12.2233087 2016

  3. [3]

    2020, ApJS, 249, 3, doi: 10.3847/1538-4365/ab929e

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

    work page doi:10.3847/1538-4365/ab929e 2020

  4. [4]

    2017, MNRAS, 470, 2617, doi: 10.1093/mnras/stx721

    Alam, S., Ata, M., Bailey, S., et al. 2017, MNRAS, 470, 2617, doi: 10.1093/mnras/stx721

    work page doi:10.1093/mnras/stx721 2017

  5. [5]

    2021, PhRvD, 103, 083533, doi: 10.1103/PhysRevD.103.083533

    Alam, S., Aubert, M., Avila, S., et al. 2021, PhRvD, 103, 083533, doi: 10.1103/PhysRevD.103.083533

    work page doi:10.1103/physrevd.103.083533 2021

  6. [6]

    Report of the Dark Energy Task Force

    Albrecht, A., Bernstein, G., Cahn, R., et al. 2006, arXiv e-prints, astro. https://arxiv.org/abs/astro-ph/0609591 Allende Prieto, C., Cooper, A. P., Dey, A., et al. 2020, Research Notes of the American Astronomical Society, 4, 188, doi: 10.3847/2515-5172/abc1dc

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2515-5172/abc1dc 2006

  7. [7]

    2019, PASP, 131, 065001, doi: 10.1088/1538-3873/ab15c2

    Baltay, C., Rabinowitz, D., Besuner, R., et al. 2019, PASP, 131, 065001, doi: 10.1088/1538-3873/ab15c2

    work page doi:10.1088/1538-3873/ab15c2 2019

  8. [8]

    E., Busca, N

    Bautista, J. E., Busca, N. G., Guy, J., et al. 2017, A&A, 603, A12, doi: 10.1051/0004-6361/201730533

    work page doi:10.1051/0004-6361/201730533 2017

  9. [9]

    J., Emes, J

    Bebek, C. J., Emes, J. H., Groom, D. E., et al. 2015, Journal of Instrumentation, 10, C05026, doi: 10.1088/1748-0221/10/05/C05026 76 DESI Collaboration

    work page doi:10.1088/1748-0221/10/05/c05026 2015

  10. [10]

    2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Besuner, R., Allen, L., Baltay, C., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11447, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 1144710, doi: 10.1117/12.2561507

    work page doi:10.1117/12.2561507 2020

  11. [11]

    2011, , 414, 264, 10.1111/j.1365-2966.2011.18402.x

    Blake, C., Kazin, E. A., Beutler, F., et al. 2011, MNRAS, 418, 1707, doi: 10.1111/j.1365-2966.2011.19592.x

    work page doi:10.1111/j.1365-2966.2011.19592.x 2011

  12. [12]

    S., & Schlegel, D

    Bolton, A. S., & Schlegel, D. J. 2010, PASP, 122, 248, doi: 10.1086/651008

    work page doi:10.1086/651008 2010

  13. [13]

    R., & Efstathiou, G

    Bond, J. R., & Efstathiou, G. 1984, ApJL, 285, L45, doi: 10.1086/184362

    work page doi:10.1086/184362 1984

  14. [14]

    T., Pappalardo, D., Pogge, R., et al

    Coker, C. T., Pappalardo, D., Pogge, R., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Ground-based and Airborne Instrumentation for Astronomy VI, ed. C. J

    work page 2016

  15. [15]

    Simard, & H

    Evans, L. Simard, & H. Takami, 99087P, doi: 10.1117/12.2231117

    work page doi:10.1117/12.2231117

  16. [16]

    2006, , 366, 101, 10.1111/j.1365-2966.2005.09782.x

    Cole, S., Percival, W. J., Peacock, J. A., et al. 2005, MNRAS, 362, 505, doi: 10.1111/j.1365-2966.2005.09318.x

    work page doi:10.1111/j.1365-2966.2005.09318.x 2005

  17. [17]

    A., Brooks, D., Derwent, M., et al

    Coles, R. A., Brooks, D., Derwent, M., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10706, Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III, 107061L, doi: 10.1117/12.2312592

    work page doi:10.1117/12.2312592 2018

  18. [18]

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

    Dawson, K. S., Kneib, J.-P., Percival, W. J., et al. 2016, AJ, 151, 44, doi: 10.3847/0004-6256/151/2/44 de Mattia, A., Ruhlmann-Kleider, V., Raichoor, A., et al. 2020, arXiv e-prints, arXiv:2007.09008. https://arxiv.org/abs/2007.09008

    work page doi:10.3847/0004-6256/151/2/44 2016

  19. [19]

    The DESI Experiment Part I: Science,Targeting, and Survey Design

    Derwent, M. A., O’Brien, T. P., Pappalardo, D. P., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Ground-based and Airborne Instrumentation for Astronomy VI, 99087T, doi: 10.1117/12.2231483 DESI Collaboration, Aghamousa, A., Aguilar, J., et al. 2016a, arXiv e-prints, arXiv:1611.00036. https://arxiv....

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1117/12.2231483 2016

  20. [20]

    2014, PASP, 126, 296, doi: 10.1086/675808

    Dey, A., & Valdes, F. 2014, PASP, 126, 296, doi: 10.1086/675808

    work page doi:10.1086/675808 2014

  21. [21]

    2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Dey, A., Rabinowitz, D., Karcher, A., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Ground-based and Airborne Instrumentation for Astronomy VI, ed. C. J. Evans, L. Simard, & H. Takami, 99082C, doi: 10.1117/12.2231488

    work page doi:10.1117/12.2231488 2016

  22. [22]

    J., Lang, D., et al

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

    work page doi:10.3847/1538-3881/ab089d 2019

  23. [23]

    T., & Dark Energy Survey Collaboration

    Diehl, H. T., & Dark Energy Survey Collaboration. 2015, in APS Meeting Abstracts, Vol. 2015, APS April Meeting

    work page 2015

  24. [24]

    2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Doel, P., Besuner, R., Brooks, D., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Ground-based and Airborne Instrumentation for Astronomy VI, ed. C. J. Evans, L. Simard, & H. Takami, 99088D, doi: 10.1117/12.2232493 du Mas des Bourboux, H., Le Goff, J.-M., Blomqvist, M., et al. 2017, A&A, 608, A130, d...

    work page doi:10.1117/12.2232493 2016

  25. [25]

    H., Claybaugh, T

    Duan, Y., Silber, J. H., Claybaugh, T. M., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10706, Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III, ed. R. Navarro & R. Geyl, 1070643, doi: 10.1117/12.2309875

    work page doi:10.1117/12.2309875 2018

  26. [26]

    2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Edelstein, J., Jelinsky, P., Levi, M., Tarle, G., & Brooks, D. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10702, Proc. SPIE, 107027G, doi: 10.1117/12.2311821

    work page doi:10.1117/12.2311821 2018

  27. [27]

    J., Zehavi, I., Hogg, D

    Eisenstein, D. J., Zehavi, I., Hogg, D. W., et al. 2005, ApJ, 633, 560, doi: 10.1086/466512

    work page doi:10.1086/466512 2005

  28. [28]

    2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Fagrelius, P., Poppett, C., & Edelstein, J. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Proc. SPIE, 99087Q, doi: 10.1117/12.2231331

    work page doi:10.1117/12.2231331 2016

  29. [29]

    2018, PASP, 130, 025005, doi: 10.1088/1538-3873/aaa225

    Fagrelius, P., Abareshi, B., Allen, L., et al. 2018, PASP, 130, 025005, doi: 10.1088/1538-3873/aaa225

    work page doi:10.1088/1538-3873/aaa225 2018

  30. [30]

    2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Fagrelius, P., Duan, Y., Fanning, K., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11447, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 114478K, doi: 10.1117/12.2561631

    work page doi:10.1117/12.2561631 2020

  31. [31]

    T., Honscheid, K., et al

    Flaugher, B., Diehl, H. T., Honscheid, K., et al. 2015, AJ, 150, 150, doi: 10.1088/0004-6256/150/5/150 Gaia Collaboration, Prusti, T., de Bruijne, J. H. J., et al. 2016, A&A, 595, A1, doi: 10.1051/0004-6361/201629272 Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2018, A&A, 616, A1, doi: 10.1051/0004-6361/201833051

    work page doi:10.1088/0004-6256/150/5/150 2015

  32. [32]

    E., Siegmund , W

    Gunn, J. E., Siegmund, W. A., Mannery, E. J., et al. 2006, AJ, 131, 2332, doi: 10.1086/500975

    work page doi:10.1086/500975 2006

  33. [33]

    H., Sloane, N

    Hardin, R. H., Sloane, N. J. A., & Smith, W. D. 2001, Tables of spherical codes with icosahedral symmetry. http://NeilSloane.com/icosahedral.codes/

    work page 2001

  34. [34]

    2013, ApJS, 208, 19, doi: 10.1088/0067-0049/208/2/19

    Hinshaw, G., Larson, D., Komatsu, E., et al. 2013, ApJS, 208, 19, doi: 10.1088/0067-0049/208/2/19

    work page internal anchor Pith review doi:10.1088/0067-0049/208/2/19 2013

  35. [35]

    R., Kazin, E., Davis, T

    Hinton, S. R., Kazin, E., Davis, T. M., et al. 2017, MNRAS, 464, 4807, doi: 10.1093/mnras/stw2725 DESI Instrument Overview 77

    work page doi:10.1093/mnras/stw2725 2017

  36. [36]

    E., Bebek, C

    Holland, S. E., Bebek, C. J., Dion, F., et al. 2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9154, High Energy, Optical, and Infrared Detectors for Astronomy VI, ed. A. D. Holland & J. Beletic, 91541E, doi: 10.1117/12.2057219

    work page doi:10.1117/12.2057219 2014

  37. [37]

    2012, Proc

    Honscheid, K., Elliott, A., Annis, J., et al. 2012, Proc. SPIE, 8451, 845112, doi: 10.1117/12.925717

    work page doi:10.1117/12.925717 2012

  38. [38]

    2014, Proc

    Honscheid, K., Elliott, A., Bonati, M., et al. 2014, Proc. SPIE, 9152, 91520G, doi: 10.1117/12.2057073

    work page doi:10.1117/12.2057073 2014

  39. [39]

    E., Beaufore, L., et al

    Honscheid, K., Elliott, A. E., Beaufore, L., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9913, Software and Cyberinfrastructure for Astronomy IV, ed. G. Chiozzi & J. C. Guzman, 99130P, doi: 10.1117/12.2229835

    work page doi:10.1117/12.2229835 2016

  40. [40]

    E., Buckley-Geer, E., et al

    Honscheid, K., Elliott, A. E., Buckley-Geer, E., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10707, Proc. SPIE, 107071D, doi: 10.1117/12.2311927

    work page doi:10.1117/12.2311927 2018

  41. [41]

    2015, MNRAS, 449, 848, doi: 10.1093/mnras/stu2693

    Manera, M. 2015, MNRAS, 449, 848, doi: 10.1093/mnras/stu2693

    work page doi:10.1093/mnras/stu2693 2015

  42. [42]

    M., Edelstein, J., et al

    Ishikawa, Y., Sirk, M. M., Edelstein, J., et al. 2018, ApJ, 869, 24, doi: 10.3847/1538-4357/aaebfb

    work page doi:10.3847/1538-4357/aaebfb 2018

  43. [43]

    E., Lacey , C

    Jones, D. H., Read, M. A., Saunders, W., et al. 2009, MNRAS, 399, 683, doi: 10.1111/j.1365-2966.2009.15338.x

    work page doi:10.1111/j.1365-2966.2009.15338.x 2009

  44. [44]

    1987, MNRAS, 227, 1, doi: 10.1093/mnras/227.1.1

    Kaiser, N. 1987, MNRAS, 227, 1, doi: 10.1093/mnras/227.1.1

    work page doi:10.1093/mnras/227.1.1 1987

  45. [45]

    A., Koda, J., Blake, C., et al

    Kazin, E. A., Koda, J., Blake, C., et al. 2014, MNRAS, 441, 3524, doi: 10.1093/mnras/stu778

    work page doi:10.1093/mnras/stu778 2014

  46. [46]

    2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Kennemore, C., Archer, D., Barbaria, R., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10706, Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III, 107061S, doi: 10.1117/12.2313006

    work page doi:10.1117/12.2313006 2018

  47. [47]

    P., et al

    Kent, S., Lampton, M., Doel, A. P., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Ground-based and Airborne Instrumentation for Astronomy VI, ed. C. J. Evans, L. Simard, & H. Takami, 99088F, doi: 10.1117/12.2232689

    work page doi:10.1117/12.2232689 2016

  48. [48]

    Kent, S. M. 2018, PASP, 130, 044501, doi: 10.1088/1538-3873/aaa6b8

    work page doi:10.1088/1538-3873/aaa6b8 2018

  49. [49]

    2020, in IEEE/ACM HPC for Urgent Decision Making, UrgentHPC@SC 2020, Atlanta, GA, USA, November 13, 2020 (IEEE), 1–9, doi: 10.1109/UrgentHPC51945.2020.00006

    Kremin, A., Bailey, S., Guy, J., Kisner, T., & Zhang, K. 2020, in IEEE/ACM HPC for Urgent Decision Making, UrgentHPC@SC 2020, Atlanta, GA, USA, November 13, 2020 (IEEE), 1–9, doi: 10.1109/UrgentHPC51945.2020.00006

    work page doi:10.1109/urgenthpc51945.2020.00006 2020

  50. [50]

    2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Leitner, D., Aguilar, J., Ameel, J., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10706, Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III, 1070669, doi: 10.1117/12.2312228

    work page doi:10.1117/12.2312228 2018

  51. [51]

    The DESI Experiment, a whitepaper for Snowmass 2013

    Levi, M., Bebek, C., Beers, T., et al. 2013, arXiv e-prints, arXiv:1308.0847. https://arxiv.org/abs/1308.0847

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  52. [52]

    2021, in Proceedings of the 20th Python in Science Conference, ed

    Margala, D., Stephey, L., Thomas, R., & Bailey, S. 2021, in Proceedings of the 20th Python in Science Conference, ed. Meghann Agarwal, Chris Calloway, Dillon Niederhut, & David Shupe, 33 – 39, doi: 10.25080/majora-1b6fd038-004

    work page doi:10.25080/majora-1b6fd038-004 2021

  53. [53]

    2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Martini, P., Elias, J., Points, S., et al. 2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9147, Ground-based and Airborne Instrumentation for Astronomy V, 91470Z, doi: 10.1117/12.2056834

    work page doi:10.1117/12.2056834 2014

  54. [54]

    M., Abareshi, B., Dey, A., et al

    Meisner, A. M., Abareshi, B., Dey, A., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11447, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 1144794, doi: 10.1117/12.2574776

    work page doi:10.1117/12.2574776 2020

  55. [55]

    N., Besuner, R

    Miller, T. N., Besuner, R. W., Levi, M. E., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10706, Proc. SPIE, 107060X, doi: 10.1117/12.2312949 O’Brien, T. P., Derwent, M., Martini, P., & Poczulp, G. 2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9151, Advances i...

    work page doi:10.1117/12.2312949 2018

  56. [56]

    Peebles, P. J. E., & Yu, J. T. 1970, ApJ, 162, 815, doi: 10.1086/150713

    work page doi:10.1086/150713 1970

  57. [57]

    2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Perruchot, S., Blanc, P.-´E., Guy, J., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11447, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 1144786, doi: 10.1117/12.2561275 Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2016, A&A, 594, A13, doi: 10.1051/0004-6361/201525830

    work page doi:10.1117/12.2561275 2020

  58. [58]

    2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Bramall, D. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10702, Proc. SPIE, 107027O, doi: 10.1117/12.2312176

    work page doi:10.1117/12.2312176 2018

  59. [59]

    2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Poppett, C., Jelinsky, P., Guy, J., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11447, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 1144711, doi: 10.1117/12.2562565 78 DESI Collaboration

    work page doi:10.1117/12.2562565 2020

  60. [60]

    J., Karim, T., et al

    Raichoor, A., Eisenstein, D. J., Karim, T., et al. 2020, Research Notes of the American Astronomical Society, 4, 180, doi: 10.3847/2515-5172/abc078

    work page doi:10.3847/2515-5172/abc078 2020

  61. [61]

    2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Roodman, A., Reil, K., & Davis, C. 2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9145, Ground-based and Airborne Telescopes V, 914516, doi: 10.1117/12.2056904

    work page doi:10.1117/12.2056904 2014

  62. [62]

    J., Martini, P., Coles, R., et al

    Ross, A. J., Martini, P., Coles, R., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10702, Proc. SPIE, 1070280, doi: 10.1117/12.2312885

    work page doi:10.1117/12.2312885 2018

  63. [63]

    2020, Research Notes of the American Astronomical Society, 4, 187, doi: 10.3847/2515-5172/abc25a

    Ruiz-Macias, O., Zarrouk, P., Cole, S., et al. 2020, Research Notes of the American Astronomical Society, 4, 187, doi: 10.3847/2515-5172/abc25a

    work page doi:10.3847/2515-5172/abc25a 2020

  64. [64]

    2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Schweiker, H. 2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 7735, Ground-based and Airborne Instrumentation for Astronomy III, ed. I. S. McLean, S. K. Ramsay, & H. Takami, 77353A, doi: 10.1117/12.857619

    work page doi:10.1117/12.857619 2010

  65. [65]

    2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Schmoll, J., Besuner, R., Bramall, D., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10702, Ground-based and Airborne Instrumentation for Astronomy VII, ed. C. J

    work page 2018

  66. [66]

    Simard, & H

    Evans, L. Simard, & H. Takami, 107027N, doi: 10.1117/12.2312140

    work page doi:10.1117/12.2312140

  67. [67]

    W., et al

    Schubnell, M., Ameel, J., Besuner, R. W., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Ground-based and Airborne Instrumentation for Astronomy VI, 990892, doi: 10.1117/12.2233370

    work page doi:10.1117/12.2233370 2016

  68. [68]

    J., Ackerman, M

    Sholl, M. J., Ackerman, M. R., Bebek, C., et al. 2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 8446, Ground-based and Airborne Instrumentation for Astronomy IV, ed. I. S

    work page 2012

  69. [69]

    McLean, S. K. Ramsay, & H. Takami, 844667, doi: 10.1117/12.926179

    work page doi:10.1117/12.926179

  70. [70]

    2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Shourt, W., Besuner, R., Silber, J., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11445, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 114456J, doi: 10.1117/12.2562687

    work page doi:10.1117/12.2562687 2020

  71. [71]

    A., Gunn, J

    Smee, S. A., Gunn, J. E., Uomoto, A., et al. 2013, AJ, 146, 32, doi: 10.1088/0004-6256/146/2/32

    work page doi:10.1088/0004-6256/146/2/32 2013

  72. [72]

    2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Sprayberry, D., Goble, W., Allen, L., et al. 2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9145, Ground-based and Airborne Telescopes V, 91453Y, doi: 10.1117/12.2055625

    work page doi:10.1117/12.2055625 2014

  73. [73]

    2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Sprayberry, D., Dunlop, P., Evatt, M., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9906, Ground-based and Airborne Telescopes VI, 990608, doi: 10.1117/12.2233177

    work page doi:10.1117/12.2233177 2016

  74. [74]

    A., & Zeldovich, Y

    Sunyaev, R. A., & Zeldovich, Y. B. 1970, Ap&SS, 7, 3, doi: 10.1007/BF00653471

    work page doi:10.1007/bf00653471 1970

  75. [75]

    2020, MNRAS, 499, 5527, doi: 10.1093/mnras/staa3050

    Tamone, A., Raichoor, A., Zhao, C., et al. 2020, MNRAS, 499, 5527, doi: 10.1093/mnras/staa3050

    work page doi:10.1093/mnras/staa3050 2020

  76. [76]

    S., Kirkby, D., Martini, P., et al

    Tie, S. S., Kirkby, D., Martini, 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, 1144785, doi: 10.1117/12.2561436

    work page doi:10.1117/12.2561436 2020

  77. [77]

    2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Tyas, L., Besuner, R., Bramall, D., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10702, Ground-based and Airborne Instrumentation for Astronomy VII, ed. C. J

    work page 2018

  78. [78]

    Simard, & H

    Evans, L. Simard, & H. Takami, 107027L, doi: 10.1117/12.2312034

    work page doi:10.1117/12.2312034

  79. [79]

    2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Warner, M., Cantarutti, R., Schumacher, G., et al. 2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 8451, Software and Cyberinfrastructure for Astronomy II, 84510U, doi: 10.1117/12.926193

    work page doi:10.1117/12.926193 2012

  80. [80]

    L., Eisenhardt, P

    Wright, E. L., Eisenhardt, P. R. M., Mainzer, A. K., et al. 2010, AJ, 140, 1868, doi: 10.1088/0004-6256/140/6/1868 Y` eche, C., Palanque-Delabrouille, N., Claveau, C.-A., et al. 2020, Research Notes of the American Astronomical Society, 4, 179, doi: 10.3847/2515-5172/abc01a

    work page internal anchor Pith review doi:10.1088/0004-6256/140/6/1868 2010

Showing first 80 references.