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Sloan Digital Sky Survey-V: Pioneering Panoptic Spectroscopy

T0 review · 1 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read SDSS-V claims to be the first all-sky, multi-epoch optical-to-infrared spectroscopic survey, pairing robotic multi-object spectroscopy on both hemispheres with ultra-wide-field integral field mapping of roughly a tenth of the sky.

desk verdict Worth knowing: this is the authoritative SDSS-V overview, and the central claim of a first all-sky multi-epoch optical-to-IR spectroscopic survey is credible; the real problem is the internally inconsistent LVM sky-area numbers, which should be fixed before acceptance. read the letter →

arxiv 2507.06989 v1 pith:K6F2LZVO submitted 2025-07-09 astro-ph.IM astro-ph.GAastro-ph.HEastro-ph.SR

Juna A. Kollmeier , Hans-Walter Rix , Conny Aerts , James Aird , Pablo Vera Alfaro , Andrés Almeida , Scott F. Anderson , Óscar Jiménez Arranz
show 212 more authors
Stefan M. Arseneau Roberto Assef Shir Aviram Catarina Aydar Carles Badenes Avrajit Bandyopadhyay Kat Barger Robert H. Barkhouser Franz E. Bauer Chad Bender Felipe Besser Binod Bhattarai Pavaman Bilgi Jonathan Bird Dmitry Bizyaev Guillermo A. Blanc Michael R. Blanton John Bochanski Jo Bovy Christopher Brandon William Nielsen Brandt Joel R. Brownstein Johannes Buchner Joseph N. Burchett Joleen Carlberg Andrew R. Casey Lesly Castaneda-Carlos Priyanka Chakraborty Julio Chanamé Vedant Chandra Brian Cherinka Igor Chilingarian Johan Comparat Maren Cosens Kevin Covey Jeffrey D. Crane Nicole R. Crumpler Katia Cunha Tim Cunningham Xinyu Dai Jeremy Darling James W. Davidson Jr. Megan C. Davis Nathan De Lee Niall Deacon José Eduardo Méndez Delgado Sebastian Demasi Mariia Demianenko Mark Derwent Elena D'Onghia Francesco Di Mille Bruno Dias John Donor Niv Drory Tom Dwelly Oleg Egorov Evgeniya Egorova Kareem El-Badry Mike Engelman Mike Eracleous Xiaohui Fan Emily Farr Logan Fries Peter Frinchaboy Cynthia S. Froning Boris T. Gänsicke Pablo García Joseph Gelfand Nicola Pietro Gentile Fusillo Simon Glover Katie Grabowski Eva K. Grebel Paul J Green Catherine Grier Pramod Gupta Aidan C. Gray Maximilian Häberle Patrick B. Hall Randolph P. Hammond Keith Hawkins Albert C. Harding Viola Hegedűs Tom Herbst J.J. Hermes Paola Rodríguez Hidalgo Thomas Hilder David W Hogg Jon A. Holtzman Danny Horta Yang Huang Hsiang-Chih Hwang Hector Javier Ibarra-Medel Julie Imig Keith Inight Arghajit Jana Alexander P. Ji Paula Jofre Matt Johns Jennifer Johnson James W. Johnson Evelyn J. Johnston Amy M Jones Ivan Katkov Anton M. Koekemoer Marina Kounkel Kathryn Kreckel Dhanesh Krishnarao Mirko Krumpe Nimisha Kumari Thomas Kupfer Ivan Lacerna Chervin Laporte Sebastien Lepine Jing Li Xin Liu Sarah Loebman Knox Long Alexandre Roman-Lopes Yuxi Lu Steven Raymond Majewski Dan Maoz Kevin A. McKinnon Ilija Medan Andrea Merloni Dante Minniti Sean Morrison Natalie Myers Szabolcs Mészáros Kirpal Nandra Prasanta K. Nayak Melissa K Ness David L. Nidever Thomas O'Brien Micah Oeur Audrey Oravetz Daniel Oravetz Jonah Otto Gautham Adamane Pallathadka Povilas Palunas Kaike Pan Daniel Pappalardo Rakesh Pandey Castalia Alenka Negrete Peñaloza Marc H. Pinsonneault Richard W. Pogge Manuchehr Taghizadeh Popp Adrian M. Price-Whelan Nadiia Pulatova Dan Qiu Solange Ramirez Amy Rankine Claudio Ricci Jessie C. Runnoe Sebastian Sanchez Mara Salvato Natascha Sattler Andrew K. Saydjari Conor Sayres Kevin C. Schlaufman Donald P. Schneider Matthias R. Schreiber Axel Schwope Javier Serna Yue Shen Cristóbal Sifón Amrita Singh Amaya Sinha Stephen Smee Ying-Yi Song Diogo Souto Keivan G. Stassun Matthias Steinmetz Alexander Stone-Martinez Guy Stringfellow Amelia Stutz José Sá nchez-Gallego Jonathan C. Tan Jamie Tayar Riley Thai Ani Thakar Yuan-Sen Ting Andrew Tkachenko Gagik Tovmasian Benny Trakhtenbrot José G. Fernández-Trincado Nicholas Troup Jonathan Trump Sarah Tuttle Roeland P. van der Marel Sandro Villanova Jaime Villaseñor Stefanie Wachter Zachary Way Anne-Marie Weijmans David Weinberg Adam Wheeler John Wilson Alessa I. Wiggins Tony Wong Qiaoya Wu Dominika Wylezalek Xiang-Xiang Xue Qian Yang Nadia Zakamska Eleonora Zari Gail Zasowski Grisha Zeltyn Catherine Zucker Carlos G. Román Zúñiga Rodolfo de J. Zermeño
This is my paper · ORCID
classification astro-ph.IMastro-ph.GAastro-ph.HEastro-ph.SR
keywords panopticspectroscopymulti-objectintegralfieldroboticfiberpositionersreverberationmappingMilkyWayMapperBlackHoleLocalVolume
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

SDSS-V aims to establish that a ground-based spectroscopic survey can match the all-sky, time-domain scope of modern space missions. It claims to be the first all-sky, multi-epoch optical-to-infrared spectroscopic survey, using robots on two hemispheres to reposition 500 fibers in minutes instead of swapping pre-drilled plates. It also claims the first ultra-wide-field optical integral field unit, LVM-I, which maps about 4,000 square degrees, roughly a tenth of the celestial sphere, with 37-arcsecond spaxels. If these claims hold, astronomers get millions of repeated stellar and quasar spectra plus contiguous spectral maps of the Milky Way and nearby galaxies, turning spectroscopy into a panoptic time-domain tool.

What carries the argument

The load-bearing mechanism is the robotic Focal Plane System (FPS): 500 zonal fiber positioners per telescope that reconfigure in under three minutes, allowing more than 30 fields per night and reducing target lead time from months to minutes. Positional feedback from a fiber-viewing camera brings blind-move errors from roughly 50 microns to about 20 microns RMS, and the kaiju path-planning code achieves better than 99.99% collision-free reconfiguration efficiency. For the integral field side, LVM-I pairs a 16-cm siderostat telescope with a 1,801-fiber lenslet IFU, a 35.3-arcsecond spaxel scale, and three $R\sim4000$ spectrographs covering 3600--9800 Å; this combination is what makes contiguous spectral mapping of a tenth of the sky affordable.

What would settle it

Track the fiber-view-camera metrology logs and kaiju reconfiguration records over a continuous year of operations at both survey sites: a sustained rise in RMS positioning error above the roughly 18--20 micron target, or a drop in reconfiguration success below the claimed 99.99%, would falsify the survey's ability to deliver its planned panoptic coverage. A simpler check is comparing the number of unique targets and epochs in the first public data releases against the target counts in Tables 2--4 of the paper.

Watch

Extended reading notes

Core claim

The paper's central claim is that SDSS-V has realized "panoptic spectroscopy": the first all-sky, multi-epoch spectroscopic survey covering optical and near-infrared wavelengths. The dual-hemisphere multi-object system obtains spectra for roughly six million objects, with about a million observed at multiple epochs through 15-minute exposure quanta. A separate new facility, LVM-I, feeds 1,801 lenslet-coupled fibers arranged in a 0.5-degree hexagon to three medium-resolution spectrographs, providing integral field spectroscopy over about 4,300 square degrees with sub-parsec to 10-parsec resolution in the Milky Way and Magellanic Clouds. The survey is organized into three mappers: Milky Way Mapper for stellar chemo-dynamics and stellar physics, Black Hole Mapper for supermassive black hole growth via reverberation mapping and X-ray source follow-up, and Local Volume Mapper for the interstellar medium and feedback.

Load-bearing premise

The all-sky, multi-epoch claim depends on the robotic fiber positioners at both sites keeping their current measured performance (about 20 microns RMS positioning and greater than 99.99% reconfiguration success) for the full survey duration; if either degrades, the planned cadence and sky completeness will not be reached.

Editorial extensions

If this is right

  • More than seven million unique stars will get high-resolution near-IR or optical spectra, and over 700,000 X-ray-selected active galactic nuclei will get identification spectra, with many objects observed across multiple epochs.
  • Reverberation mapping of roughly 1,000--1,500 quasars at about 100 epochs each will grow the sample of directly measured black hole masses by about an order of magnitude.
  • The Local Volume Mapper will take more than 55 million spectra over about 4,300 square degrees, including 0.1--1 pc sampling of Milky Way nebulae and 10 pc sampling of the Magellanic Clouds.
  • Robotic reconfiguration reduces the time to point at a transient from months to minutes, making spectroscopic follow-up of newly discovered sources a routine part of survey operations.
  • Matching SDSS-V spectra to all-sky imaging from space missions multiplies the scientific return of those missions with ground-based radial velocities, abundances, and spectral classifications.

Reading between the lines

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

  • The 15-minute epoch quanta make spectroscopy itself a time-domain survey rather than a one-pass census; the same design pattern could be adopted by other wide-field fiber spectrographs to create multi-epoch surveys without dedicated target lists.
  • If LVM-I reaches its planned 4,300 square degrees, the jump from 0.001% to roughly 10% of the celestial sphere with contiguous optical IFU coverage suggests that all-sky IFU mapping is an engineering scaling problem, not a conceptual impossibility.
  • The combination of rapid reconfiguration and fiber-view-camera metrology sets quantitative benchmarks (about 20 microns RMS positioning, >99.99% path efficiency) that future robotic positioner arrays could be designed against.
  • An obvious testable extension is to check DR19 and DR20 delivered spectra against the planned target counts and cadences; discrepancies would isolate whether the bottleneck is scheduling, positioning, or weather.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

1 major / 4 minor

Summary. This paper is a status report for SDSS-V, describing the survey's three science programs (Black Hole Mapper, Milky Way Mapper, Local Volume Mapper), the dual-hemisphere MOS instrumentation (robotic Focal Plane Systems feeding BOSS and APOGEE spectrographs), the new LVM-I integral field facility, survey planning and scheduling software, data reduction and analysis pipelines, and data management/archiving infrastructure. The central claim is that SDSS-V is pioneering panoptic spectroscopy: the first all-sky, multi-epoch, optical-to-infrared spectroscopic survey, and the first ultra-wide-field optical IFU program covering about 1/10th of the celestial sphere. The paper reports that MOS robotic operations began in 2021 and LVM-I IFS observations began in 2023, with detailed performance numbers for fiber positioning and path planning.

Significance. If the survey delivers as described, this is a historically significant program: it combines all-sky multi-epoch optical and near-infrared MOS spectroscopy with contiguous IFU spectroscopy over thousands of square degrees, and it is explicitly designed to be a public, community resource. The paper's credibility is strengthened by concrete software products that are open source and named in the text (robostrategy, kaiju, coordio, cherno, hal, Astra), by the 'publish all the bits' data-release philosophy, and by the quantitative operational metrics reported in Section 5.5 (kaiju path-planning efficiency above 99.99%, fiber positioning accuracy around 20 microns RMS). The main load-bearing weakness is the internally inconsistent LVM sky-area figures, which conflict across the abstract, introduction, Sections 2.3.1, 2.3.3, 4, and Table 4; because the 'about 1/10th of the celestial sphere' claim is a headline statement, this inconsistency must be resolved. Many detailed design and performance claims are also deferred to 'in prep' references, which is acceptable for a status report but limits independent verification.

major comments (1)
  1. [Abstract; Section 1] The abstract's claim that SDSS-V is "the first all-sky, multi-epoch, optical-to-infrared spectroscopic survey" needs qualification in light of the paper's own footnote 1, which acknowledges that Gaia already provides all-sky optical spectroscopy, albeit at R≲100 (BP/RP) and with narrow wavelength coverage (RVS). As written, the abstract can be read as claiming precedence over Gaia's spectroscopic data, which is not accurate. Please rephrase to specify the intended claim, e.g., "the first all-sky, multi-epoch survey providing high-resolution (R≳1000) optical and near-infrared spectroscopy," or otherwise explicitly compare with Gaia's spectral capabilities. Similarly, given that operations began in 2021 and are still underway, the wording should distinguish between the survey as designed/operating and the survey as completed, or the claim should be tied to the survey's planned scope.
minor comments (4)
  1. [Section 3.1; Section 3.2; Abstract; Figure 1] The APOGEE fiber count is inconsistently reported as 300 fibers in the abstract and in several places in Section 3, but as 298 fibers in Section 3.1 and as "298 robots that have active APOGEE fibers" in Section 3.2, before the text again refers to "300 APOGEE fibers" in the focal-plane layout description. Please state clearly whether the design value is 300 with 298 currently active, or whether the instrument has 298 total, and use consistent numbers throughout.
  2. [Section 2.1.3] The text contains a typo, "BMH in SDSS-V", in the paragraph listing early Black Hole Mapper science publications; it should read "BHM". Similar minor typos elsewhere include "comissioning" (Section 3.2), "ressources" (Section 3.1.2), "reache" (Figure 2 caption), and "Smee et al. (2025, in prep.." (Section 3.3).
  3. [Table 3] In the Milky Way Mapper targeting summary, the row "mwm tessob APOGEE 20 8" appears to have an incomplete target count; please clarify whether "20" is a placeholder or the intended number.
  4. [Throughout] The paper relies heavily on "in prep" references for key details such as robostrategy, the LVM reduction pipeline, and upcoming data-release papers. This is acceptable for a status report, but the headline numbers and central claims would be easier to verify if the manuscript either gave the essential numbers in the text or cited published papers for them.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: SDSS-V is a descriptive survey overview with no derivation that reduces to its inputs.

full rationale

This paper is an instrumental and survey description rather than a derivation or prediction paper. Its central claims, such as being the first all-sky, multi-epoch, optical-to-infrared MOS survey and providing the first ultra-wide-field optical IFU coverage of roughly one-tenth of the celestial sphere, are empirical and descriptive statements about survey design, hardware, and operations. There is no fitted parameter later relabeled as a prediction, and no equation in the paper defines a claimed output in terms of an input. The differing LVM area figures (Abstract approximately 4000 deg^2; Section 2.3.1 approximately 3,300 deg^2; Section 2.3.3 approximately 4,300 deg^2; Section 4 over 3500 square degrees; Table 4 components summing higher) present an internal consistency concern, not circularity. Self-citations such as Kollmeier et al. (2017) and Drory et al. (2024) provide project background and engineering references; none is invoked as an unverified theorem to forbid alternatives or as the sole support for a quantitative result. The 'first' claims are falsifiable against external survey history and are not implied by any definition in the paper. Therefore no circular step can be exhibited with quoted text; the honest finding is a score of 0.

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

The paper introduces no new theoretical entities or free parameters. It relies on assumptions about instrument performance and survey continuity, which are design goals rather than derived quantities.

assumptions (3)
  • domain assumption The two robotic Focal Plane Systems will maintain their measured positioning accuracy and reconfiguration efficiency for the duration of the survey.
    The all-sky, multi-epoch claim depends on sustained performance; Section 5.5 reports current measured values.
  • domain assumption The Local Volume Mapper IFU will reach the stated 5-sigma H-alpha sensitivity of 6e-18 erg/s/cm2/arcsec2 in 15-minute exposures.
    The LVM survey's ability to map the diffuse ISM depends on this sensitivity; stated as a design goal in Section 6.2, not yet demonstrated across the full footprint.
  • domain assumption The survey will receive the planned observing time and survive the duration.
    The paper's claimed scope (millions of targets, multiple epochs) depends on multi-year operations.

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Cite this review

Pith. "Pith review of Sloan Digital Sky Survey-V: Pioneering Panoptic Spectroscopy." pith.science (2026). https://pith.science/paper/K6F2LZVO

@misc{pith2026250706989,
  author       = {Pith},
  title        = {Pith review of: Sloan Digital Sky Survey-V: Pioneering Panoptic Spectroscopy},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/K6F2LZVO}},
  note         = {Machine review of arXiv:2507.06989}
}
abstract

The Sloan Digital Sky Survey-V (SDSS-V) is pioneering panoptic spectroscopy: it is the first all-sky, multi-epoch, optical-to-infrared spectroscopic survey. SDSS-V is mapping the sky with multi-object spectroscopy (MOS) at telescopes in both hemispheres (the 2.5-m Sloan Foundation Telescope at Apache Point Observatory and the 100-inch du Pont Telescope at Las Campanas Observatory), where 500 zonal robotic fiber positioners feed light from a wide-field focal plane to an optical (R$\sim 2000$, 500 fibers) and a near-infrared (R$\sim 22,000$, 300 fibers) spectrograph. In addition to these MOS capabilities, the survey is pioneering ultra wide-field ($\sim$ 4000~deg$^2$) integral field spectroscopy enabled by a new dedicated facility (LVM-I) at Las Campanas Observatory, where an integral field spectrograph (IFS) with 1801 lenslet-coupled fibers arranged in a 0.5 degree diameter hexagon feeds multiple R$\sim$4000 optical spectrographs that cover 3600-9800 angstroms. SDSS-V's hardware and multi-year survey strategy are designed to decode the chemo-dynamical history of the Milky Way Galaxy and tackle fundamental open issues in stellar physics in its Milky Way Mapper program, trace the growth physics of supermassive black holes in its Black Hole Mapper program, and understand the self-regulation mechanisms and the chemical enrichment of galactic ecosystems at the energy-injection scale in its Local Volume Mapper program. The survey is well-timed to multiply the scientific output from major all-sky space missions. The SDSS-V MOS programs began robotic operations in 2021; IFS observations began in 2023 with the completion of the LVM-I facility. SDSS-V builds upon decades of heritage of SDSS's pioneering advances in data analysis, collaboration spirit, infrastructure, and product deliverables in astronomy.

Figures

Figures reproduced from arXiv: 2507.06989 by the authors.

Figure 1
Figure 1. A schematic representation of SDSS-V: an all-sky, multi-epoch spectroscopic facility and its science programs. Dual-hemisphere survey operations are undertaken at Apache Point Observatory (APO) and Las Campanas Observatory (LCO). Multi-object fiber spectroscopy is being carried out with two 2.5 m telescopes, each feeding an near-IR APOGEE spectrograph (300 fibers, R ∼ 22, 000) and an optical BOSS spectrograph (500 f… view at source ↗
Figure 2
Figure 2. Target density of SDSS-V’s two MOS mappers: The MOS target densities (MWM and BHM) across the sky are illustrated in a logarithmic color scale, ranging from 30 to 15,000 targets / deg2 . While the target density is not uniform across the entire sky, the reache of the program is clear. The LVM survey footprint is overlaid in grey. objects across the sky; and to carry out ultra-wide-field IFS mapping across more than … view at source ↗
Figure 3
Figure 3. Ratio of MWM to BHM targets across the sky in Galactic coordinates. This ratio highlights where each mapper is driving the survey implementation. The primary LVM footprint (excluding the high-latitude and nearby galaxy survey) is overlaid in white. At the core of “Sloan Surveys” (York et al. 2000a; Eisenstein et al. 2011; Blanton et al. 2017), has been the existence of clear and focused core science objectives that … view at source ↗
Figures from the paper (20 more)
Figure 4
Figure 4. Figure 4: Schematic of the innermost regions around a quasar’s central supermassive black hole (BH): the X-ray corona, accretion disk, and broad-line region (BLR). SDSS-V explores the physics of supermassive BH accretion and dynamics with three parallel approaches: reverberation…
Figure 5
Figure 5. Figure 5: Sky distribution of all BHM (and Galactic X-ray emitting) targets. Top left panel: QSO targets for BHM time-domain repeat BOSS optical spectroscopy. The gray background depicts the sky-density of bright (ipsf < 19.1) QSOs taken from the SDSS DR16 QSO catalog (Lyke et a…
Figure 6
Figure 6. Figure 6: Representative luminosity and redshift coverage of core BHM time-domain (left) and X-ray selected (right) surveys of AGN: Left panel: The distribution of absolute magnitude vs. redshift for BHM core time-domain spectra of SDSS quasars (here, highlighting a subset of ab…
Figure 7
Figure 7. Figure 7: MWM on-sky target density. These plots show the on-sky distribution of targets expected to be observed for MWM for a representative survey simulation. The Galactic Genesis survey (left) dominates the total number of stars observed under MWM, particularly in the Galacti…
Figure 8
Figure 8. Figure 8: Evolution of SDSS in-plane Galactic target density: Target surface density of the APOGEE DR17 data release (left) and MWM’s Galactic Genesis Survey (GG; right) for stars within 500 parsec of the Galactic midplane. The maps show a face-on schematic of the Milky Way (cre…
Figure 9
Figure 9. Figure 9: Stellar astrophysical targets in the MWM: The Gaia (Bp−Rp) color and absolute Gaia G magnitude of MWM targets within 1 kpc, color coded by number density. The left panel includes all stars observed with either APOGEE or BOSS that will be included in the DR 19 data rele…
Figure 10
Figure 10. Figure 10: Color-magnitude (CMD) and color-color diagrams of [PITH_FULL_IMAGE:figures/full_fig_p023_10.png]
Figure 11
Figure 11. Figure 11: SDSS-V’s stellar companion mass sensitivity. The 3σ detection limit as a function of semi-major axis and secondary mass. The detection limit assumes a 1 solar mass primary and circular orbits. For the RV limits, sin i = 1. The SDSS-V APOGEE instrument has an RV precis…
Figure 12
Figure 12. Figure 12: SDSS-V’s MWM planned epochs shown on the H-R diagram. Each of the three panels show targets drawn from Milky Way Mapper (MWM) cartons in the Theta-1 version of robostrategy survey simulation that received at least 3 epochs. Left: All targets that receive 3 or more obs…
Figure 13
Figure 13. Figure 13: Resolving nebular ISM structures with LVM. Optical (V-band) and narrow band ([O III], Hα, [S II]) imaging of the LMC reveal a wealth of nebular structures that are only apparent at the ∼10 pc resolution that LVM will achieve in the LMC/SMC and ∼pc resolution in the Mi…
Figure 14
Figure 14. Figure 14: The LVM footprint. Overlaid on a low-resolution all sky Hα map (Finkbeiner 2003), the LVM will cover a ±9 degree band along the Milky Way plane, a large area across the Orion and Gum Nebulas, and the full disk of the LMC and SMC. Higher priority zones are colored in p…
Figure 15
Figure 15. Figure 15: FPS focal plane configuration. Left: Sloan FPS unit, with yellow dust caps installed on the fiber positioners; Right: layout showing fiber positioner patrol fields (colored +s and annuli), fiber- illuminated fiducials (blue and white circles), and guide/focus/acquisit…
Figure 16
Figure 16. Figure 16: SDSS-V Wide-Field Corrector for the 2.5m at APO. [PITH_FULL_IMAGE:figures/full_fig_p035_16.png]
Figure 17
Figure 17. Figure 17: Overview of the LVM Instrument. Each of the four telescopes uses a siderostat in alt-alt configuration feeding components on an optical table. The IFUs in the focal plane convey the light to an environmentally-controlled spectrograph chamber containing a “sorting hat”…
Figure 18
Figure 18. Figure 18: Architecture of the LVM telescopes. Note that the Science and two Sky telescopes contain K-mirror de-rotators as shown, while the fourth, Spectrophotometric telescope does not. It hosts a rotating fiber selector mask in its focal plane for isolating the flux of indivi…
Figure 19
Figure 19. Figure 19: The LVM Fiber System. The four fiber bundles coming from the IFU’s (right) enter the “Sorting Hat”, where almost 2000 fiber splices redistribute them to the fiber bundles leading to the entrance slits of the spectrographs (left). The inset photos show a back illuminat…
Figure 20
Figure 20. Figure 20: IFU layout showing the allocation to each of the three spectrographs. [PITH_FULL_IMAGE:figures/full_fig_p039_20.png]
Figure 21
Figure 21. Figure 21: Three-dimensional rendering of the opto-mechanics of one spectrograph (left) and [PITH_FULL_IMAGE:figures/full_fig_p039_21.png]
Figure 22
Figure 22. Figure 22: LVM-I software subsystem architecture. See Section 6.3 for details. of IDLSPEC2D build on the final (v5 13 2) SDSS-IV/eBOSS version of the pipeline.24 These updates are outlined in Almeida et al. (2023), with a general description below. Data from BOSS are processed t…
Figure 23
Figure 23. Figure 23: SDSS-V’s Organizational Structure. The shaded colored boxes show the SDSS-V Management Committee. In cases where individuals have served out their terms, both the original and current individual are shown with individuals whose terms concluded are denoted by the aster…

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Works this paper leans on

166 extracted references · 20 canonical work pages · cited by 11 Pith papers

  1. [1]

    P., Abbott, R., Abbott, T

    Abbott, B. P., Abbott, R., Abbott, T. D., et al. 2017, Phys. Rev. Lett., 119, 161101, doi: 10.1103/PhysRevLett.119.161101 Abdurro’uf, Accetta, K., Aerts, C., et al. 2022, ApJS, 259, 35, doi: 10.3847/1538-4365/ac4414

    doi:10.1103/physrevlett.119.161101 2017

  2. [2]

    2021, Reviews of Modern Physics, 93, 015001, doi: 10.1103/RevModPhys.93.015001

    Aerts, C. 2021, Reviews of Modern Physics, 93, 015001, doi: 10.1103/RevModPhys.93.015001

    doi:10.1103/revmodphys.93.015001 2021

  3. [3]

    Aerts, C., Mathis, S., & Rogers, T. M. 2019, ARA&A, 57, 35, doi: 10.1146/annurev-astro-091918-104359

    doi:10.1146/annurev-astro-091918-104359 2019

  4. [4]

    2023, arXiv e-prints, arXiv:2311.08453, doi: 10.48550/arXiv.2311.08453

    Aerts, C., & Tkachenko, A. 2023, arXiv e-prints, arXiv:2311.08453, doi: 10.48550/arXiv.2311.08453

    arXiv doi:10.48550/arxiv.2311.08453 2023

  5. [5]

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

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

    doi:10.3847/1538-4365/aa8992 2017

  6. [6]

    F., Argudo-Fern´ andez, M., et al

    Almeida, A., Anderson, S. F., Argudo-Fern´ andez, M., et al. 2023, arXiv e-prints, arXiv:2301.07688, doi: 10.48550/arXiv.2301.07688

    arXiv doi:10.48550/arxiv.2301.07688 2023

  7. [7]

    A., Sana, H., Taylor, W., et al

    Almeida, L. A., Sana, H., Taylor, W., et al. 2017, A&A, 598, A84, doi: 10.1051/0004-6361/201629844

    doi:10.1051/0004-6361/201629844 2017

  8. [8]

    2023, ApJS, 267, 8, doi: 10.3847/1538-4365/acd53e

    Andrae, R., Rix, H.-W., & Chandra, V. 2023, ApJS, 267, 8, doi: 10.3847/1538-4365/acd53e

    doi:10.3847/1538-4365/acd53e 2023

Show all 166 references
  1. [9]

    Althouse, W. t. 2009, ApJ, 697, 1071, doi: 10.1088/0004-637X/697/2/1071

    2009 doi

  2. [10]

    2021a, AJ, 161, 147, doi: 10.3847/1538-3881/abd806 —

    Demleitner, M., & Andrae, R. 2021a, AJ, 161, 147, doi: 10.3847/1538-3881/abd806 —. 2021b, AJ, 161, 147, doi: 10.3847/1538-3881/abd806

    doi

  3. [11]

    2012, PASP, 124, 1015, doi: 10.1086/668105 —

    Bailey, S. 2012, PASP, 124, 1015, doi: 10.1086/668105 —. 2016, Weighted EMPCA: Weighted Expectation Maximization Principal Component Analysis, Astrophysics Source Code Library, record ascl:1609.007. http://ascl.net/1609.007

    2012 doi

  4. [12]

    2022, A&A, 658, A69, doi: 10.1051/0004-6361/202141037

    Banyard, G., Sana, H., Mahy, L., et al. 2022, A&A, 658, A69, doi: 10.1051/0004-6361/202141037

    2022 doi

  5. [13]

    H., Smee, S

    Barkhouser, R. H., Smee, S. A., Hammond, R. P., et al. 2022, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference

    2022

  6. [14]

    12182, Ground-based and Airborne Telescopes IX, ed

    Series, Vol. 12182, Ground-based and Airborne Telescopes IX, ed. H. K. Marshall, J. Spyromilio, & T. Usuda, 121823O, doi: 10.1117/12.2630655

    doi

  7. [15]

    2020, Frontiers in Astronomy and Space Sciences, 7, 44, doi: 10.3389/fspas.2020.00044

    Basu, S., & Hekker, S. 2020, Frontiers in Astronomy and Space Sciences, 7, 44, doi: 10.3389/fspas.2020.00044

    2020

  8. [16]

    2024, cds-astro/aladin-lite: 3.5.1-beta, 3.5.1-beta, Zenodo, doi: 10.5281/zenodo.7638833

    Baumann, M., Boch, T., Marchand, M., et al. 2024, cds-astro/aladin-lite: 3.5.1-beta, 3.5.1-beta, Zenodo, doi: 10.5281/zenodo.7638833

    2024 doi

  9. [17]

    2022, in Software and Cyberinfrastructure for Astronomy VII, ed

    Beard, S., Willemse, B., Watson, S., et al. 2022, in Software and Cyberinfrastructure for Astronomy VII, ed. J. Ibsen & G. Chiozzi, Vol. 12189, International Society for Optics and Photonics (SPIE), 121890V, doi: 10.1117/12.2629239 B´ edard, A. 2024, Ap&SS, 369, 43, doi: 10.10...

    2022 doi

  10. [18]

    L., Halpern, M., Hinshaw, G., et al

    Bennett, C. L., Halpern, M., Hinshaw, G., et al. 2003, The Astrophysical Journal Supplement Series, 148, 1, doi: 10.1086/377253

    2003 doi

  11. [19]

    2016, ARA&A, 54, 529, doi: 10.1146/annurev-astro-081915-023441

    Bland-Hawthorn, J., & Gerhard, O. 2016, ARA&A, 54, 529, doi: 10.1146/annurev-astro-081915-023441

    2016 doi

  12. [20]

    D., & McKee, C

    Blandford, R. D., & McKee, C. F. 1982, ApJ, 255, 419, doi: 10.1086/159843

    1982 doi

  13. [21]

    R., Bershady, M

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

    2017 doi

  14. [22]

    2021, A&A, 652, A70, doi: 10.1051/0004-6361/202140507 72

    Bodensteiner, J., Sana, H., Wang, C., et al. 2021, A&A, 652, A70, doi: 10.1051/0004-6361/202140507 72

    2021 doi

  15. [23]

    S., Schlegel, D

    Bolton, A. S., Schlegel, D. J., Aubourg, ´E., et al. 2012, AJ, 144, 144, doi: 10.1088/0004-6256/144/5/144

    2012 doi

  16. [24]

    J., Koch, D., Basri, G., et al

    Borucki, W. J., Koch, D., Basri, G., et al. 2010, Science, 327, 977, doi: 10.1126/science.1185402

    2010 doi

  17. [25]

    S., & Vaughan, Jr., A

    Bowen, I. S., & Vaughan, Jr., A. H. 1973, ApOpt, 12, 1430, doi: 10.1364/AO.12.001430

    1973 doi

  18. [26]

    M., & Fischer, D

    Brewer, J. M., & Fischer, D. A. 2018, ApJS, 237, 38, doi: 10.3847/1538-4365/aad501

    2018 doi

  19. [27]

    2022, A&A, 661, A1, doi: 10.1051/0004-6361/202141266

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

    2022 doi

  20. [28]

    A., Law, D

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

    2015

  21. [29]

    H., S´ anchez-Gallego, J., et al

    Cherinka, B., Andrews, B. H., S´ anchez-Gallego, J., et al. 2019, AJ, 158, 74, doi: 10.3847/1538-3881/ab2634

    2019 doi

  22. [30]

    Collaboration, P., Ade, P. A. R., Aghanim, N., et al. 2016, A&A, 594, A13, doi: 10.1051/0004-6361/201525830

    2016 doi

  23. [31]

    2023, A&A, 673, A122, doi: 10.1051/0004-6361/202245726

    Comparat, J., Luo, W., Merloni, A., et al. 2023, A&A, 673, A122, doi: 10.1051/0004-6361/202245726

    2023 doi

  24. [32]

    P., Koposov, S

    Cooper, A. P., Koposov, S. E., Allende Prieto, C., et al. 2023, ApJ, 947, 37, doi: 10.3847/1538-4357/acb3c0

    2023 doi

  25. [34]

    2012, Research in Astronomy and Astrophysics, 12, 1197, doi: 10.1088/1674-4527/12/9/003

    Cui, X.-Q., Zhao, Y.-H., Chu, Y.-Q., et al. 2012, Research in Astronomy and Astrophysics, 12, 1197, doi: 10.1088/1674-4527/12/9/003

    2012 doi

  26. [35]

    2019, MNRAS, 488, 2503, doi: 10.1093/mnras/stz1759

    Ludwig, H.-G., & Koester, D. 2019, MNRAS, 488, 2503, doi: 10.1093/mnras/stz1759

    2019 doi

  27. [36]

    S., Schlegel, D

    Dawson, K. S., Schlegel, D. J., Ahn, C. P., et al. 2013, AJ, 145, 10, doi: 10.1088/0004-6256/145/1/10 De Silva, G. M., Freeman, K. C.,

    2013 doi

  28. [37]

    2015, MNRAS, 449, 2604, doi: 10.1093/mnras/stv327

    Bland-Hawthorn, J., et al. 2015, MNRAS, 449, 2604, doi: 10.1093/mnras/stv327

    2015 doi

  29. [38]

    2024, Jdaviz, v4.0.0, Zenodo, doi: 10.5281/zenodo.5513927

    Developers, J., Averbukh, J., Bradley, L., et al. 2024, Jdaviz, v4.0.0, Zenodo, doi: 10.5281/zenodo.5513927

    2024 doi

  30. [39]

    J., Lang, D., et al

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

    2019 doi

  31. [41]

    A., Kreckel, K., et al

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

    2024 doi

  32. [42]

    2024, astropy/specutils: v1.18.0, v1.18.0, Zenodo, doi: 10.5281/zenodo.1421356

    Earl, N., Tollerud, E., O’Steen, R., et al. 2024, astropy/specutils: v1.18.0, v1.18.0, Zenodo, doi: 10.5281/zenodo.1421356

    2024 doi

  33. [43]

    J., Weinberg, D

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

    2011 doi

  34. [44]

    2022, A&A, 659, A191, doi: 10.1051/0004-6361/202141727

    Emsellem, E., Schinnerer, E., Santoro, F., et al. 2022, A&A, 659, A191, doi: 10.1051/0004-6361/202141727

    2022 doi

  35. [45]

    Finkbeiner, D. P. 2003, ApJS, 146, 407, doi: 10.1086/374411

    2003 doi

  36. [46]

    B., Trump, J

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

    2023 doi

  37. [47]

    B., Trump, J

    Fries, L. B., Trump, J. R., Horne, K., et al. 2024, ApJ, 975, 239, doi: 10.3847/1538-4357/ad7c42 Gaia Collaboration, Vallenari, A., Brown, A. G. A., et al. 2022, arXiv e-prints, arXiv:2208.00211. https://arxiv.org/abs/2208.00211 Gaia Collaboration, Creevey, O. L., Sarro, L. M....

    2024 arXiv

  38. [48]

    GaiaCollaboration, Prusti, T., de Bruijne, J. H. J., et al. 2016, A&A, 595, A1, doi: 10.1051/0004-6361/201629272

    2016 doi

  39. [49]

    1610, Sidereus nuncius magna, longeque admirabilia spectacula pandens lunae facie, fixis innumeris, lacteo circulo, stellis nebulosis,

    Galilei, G. 1610, Sidereus nuncius magna, longeque admirabilia spectacula pandens lunae facie, fixis innumeris, lacteo circulo, stellis nebulosis, ... Galileo Galileo : nuper a se reperti beneficio sunt observata in apprime vero in quatuor planetis circa Iovis stellam disparib...

    doi

  40. [50]

    2022, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference

    Gilles, M., Cammarata, C., Ducollet, H., et al. 2022, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference

    2022

  41. [51]

    12188, Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation, 121880M, doi: 10.1117/12.2627242

    Series, Vol. 12188, Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation, 121880M, doi: 10.1117/12.2627242

    doi

  42. [52]

    2012, The Messenger, 147, 25 GRA VITY Collaboration, Amorim, A.,

    Gilmore, G., Randich, S., Asplund, M., et al. 2012, The Messenger, 147, 25 GRA VITY Collaboration, Amorim, A.,

    2012

  43. [53]

    2024, A&A, 684, A167, doi: 10.1051/0004-6361/202348167 73

    Bourdarot, G., et al. 2024, A&A, 684, A167, doi: 10.1051/0004-6361/202348167 73

    2024 doi

  44. [54]

    C., Barkhouser, R

    Gray, A. C., Barkhouser, R. H., Smee, S. A., et al. 2022, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference

    2022

  45. [55]

    Evans, J. J. Bryant, & K. Motohara, 1218462, doi: 10.1117/12.2630539

    doi

  46. [56]

    M., Schlafly, E

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

    2015 doi

  47. [57]

    Grether, D., & Lineweaver, C. H. 2006, ApJ, 640, 1051, doi: 10.1086/500161

    2006 doi

  48. [58]

    E., Siegmund, W

    Gunn, J. E., Siegmund, W. A., Mannery, E. J., et al. 2006, AJ, 131, 2332, doi: 10.1086/500975 H¨ aring, N., & Rix, H.-W. 2004, ApJL, 604, L89, doi: 10.1086/383567

    2006 doi

  49. [59]

    2017, A&A Rv, 25, 1, doi: 10.1007/s00159-017-0101-x

    Hekker, S., & Christensen-Dalsgaard, J. 2017, A&A Rv, 25, 1, doi: 10.1007/s00159-017-0101-x

    2017 doi

  50. [60]

    M., Bizenberger, P., Blanc, G

    Herbst, T. M., Bizenberger, P., Blanc, G. A., et al. 2024, AJ, 168, 267, doi: 10.3847/1538-3881/ ad794810.1134/S1063772908070044

    2024

  51. [61]

    Hill, J. M. 1988, in Astronomical Society of the Pacific Conference Series, Vol. 3, Fiber Optics in Astronomy, ed. S. C. Barden, 77

    1988

  52. [62]

    1986, PASP, 98, 609, doi: 10.1086/131801

    Horne, K. 1986, PASP, 98, 609, doi: 10.1086/131801

    1986 doi

  53. [63]

    1991, ApJS, 76, 55, doi: 10.1086/191565

    Iben, Icko, J. 1991, ApJS, 76, 55, doi: 10.1086/191565

    1991 doi

  54. [64]

    T., Breedt, E., et al

    Inight, K., G¨ ansicke, B. T., Breedt, E., et al. 2023a, MNRAS, 524, 4867, doi: 10.1093/mnras/stad2018

    doi

  55. [65]

    T., Schwope, A., et al

    Inight, K., G¨ ansicke, B. T., Schwope, A., et al. 2023b, MNRAS, 525, 3597, doi: 10.1093/mnras/stad2409 —. 2023c, MNRAS, 525, 3597, doi: 10.1093/mnras/stad2409

    doi

  56. [66]

    D., Makarov, D

    Karachentsev, I. D., Makarov, D. I., & Kaisina, E. I. 2013, AJ, 145, 101, doi: 10.1088/0004-6256/145/4/101

    2013 doi

  57. [67]

    2023, A&A, 674, A5, doi: 10.1051/0004-6361/202244220

    Katz, D., Sartoretti, P., Guerrier, A., et al. 2023, A&A, 674, A5, doi: 10.1051/0004-6361/202244220

    2023 doi

  58. [68]

    C., Funes, J

    Kennicutt, Robert C., J., Lee, J. C., Funes, J. G., et al. 2008, ApJS, 178, 247, doi: 10.1086/590058

    2008 doi

  59. [69]

    L., Martini, P., Davis, T

    King, A. L., Martini, P., Davis, T. M., et al. 2015, MNRAS, 453, 1701, doi: 10.1093/mnras/stv1718

    2015 doi

  60. [70]

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

    Kollmeier, J. A., Zasowski, G., Rix, H.-W., et al. 2017, ArXiv e-prints. https://arxiv.org/abs/1711.03234

    2017 arXiv

  61. [71]

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

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

    2022 doi

  62. [72]

    Hillenbrand, L. A. 2011, ApJ, 731, 8, doi: 10.1088/0004-637X/731/1/8

    2011 doi

  63. [73]

    V., Egorova, E., et al

    Kreckel, K., Egorov, O. V., Egorova, E., et al. 2024, A&A, 689, A352, doi: 10.1051/0004-6361/202449943

    2024 doi

  64. [74]

    J., Mink, D

    Kurtz, M. J., Mink, D. J., Wyatt, W. F., et al. 1992, in Astronomical Society of the Pacific Conference Series, Vol. 25, Astronomical Data Analysis Software and Systems I, ed. D. M

    1992

  65. [75]

    Lacerda, E. A. D., S´ anchez, S. F., Mej ´ ıa-Narv´ aez, A., et al. 2022, arXiv e-prints, arXiv:2202.08027. https://arxiv.org/abs/2202.08027

    2022 arXiv

  66. [76]

    M., Cales, S., Moran, E

    LaMassa, S. M., Cales, S., Moran, E. C., et al. 2015, ApJ, 800, 144, doi: 10.1088/0004-637X/800/2/144

    2015 doi

  67. [77]

    2010, AJ, 139, 1782, doi: 10.1088/0004-6256/139/5/1782 Lema ˆ ıtre, G

    Roweis, S. 2010, AJ, 139, 1782, doi: 10.1088/0004-6256/139/5/1782 Lema ˆ ıtre, G. 1927, Annales de la Soci&eacute;t&eacute; Scientifique de Bruxelles, 47, 49

    2010 doi

  68. [78]

    K., Sandstrom, K

    Leroy, A. K., Sandstrom, K. M., Lang, D., et al. 2019, ApJS, 244, 24, doi: 10.3847/1538-4365/ab3925

    2019 doi

  69. [79]

    A., Hern´ andez, J., et al

    Lindegren, L., Klioner, S. A., Hern´ andez, J., et al. 2021, A&A, 649, A2, doi: 10.1051/0004-6361/202039709

    2021 doi

  70. [80]

    2011, MNRAS, 410, 166, doi: 10.1111/j.1365-2966.2010.17432.x

    Lintott, C., Schawinski, K., Bamford, S., et al. 2011, MNRAS, 410, 166, doi: 10.1111/j.1365-2966.2010.17432.x

    2011

  71. [81]

    L., et al

    Lundgren, B., Tojeiro, R., Beaton, R. L., et al. 2019, Boletin de la Asociacion Argentina de Astronomia La Plata Argentina, 61, 261

    2019

  72. [82]

    W., Higley, A

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

    2020 doi

  73. [83]

    2000, ARA&A, 38, 143, doi: 10.1146/annurev.astro.38.1.143

    Maeder, A., & Meynet, G. 2000, ARA&A, 38, 143, doi: 10.1146/annurev.astro.38.1.143

    2000 doi

  74. [84]

    1998, AJ, 115, 2285, doi: 10.1086/300353 74

    Magorrian, J., Tremaine, S., Richstone, D., et al. 1998, AJ, 115, 2285, doi: 10.1086/300353 74

    1998 doi

  75. [85]

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

    Mahadevan, S., Ramsey, L., Bender, C., et al. 2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference

    2012

  76. [86]

    McLean, S. K. Ramsay, & H. Takami, 84461S, doi: 10.1117/12.926102

    doi

  77. [87]

    W., Terrien, R., et al

    Mahadevan, S., Ramsey, L. W., Terrien, R., et al. 2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference

    2014

  78. [88]

    Ramsay, I. S. McLean, & H. Takami, 91471G, doi: 10.1117/12.2056417

    doi

  79. [89]

    2014, A&A, 566, A84, doi: 10.1051/0004-6361/201323202

    Makarem, L., Kneib, J.-P., Gillet, D., et al. 2014, A&A, 566, A84, doi: 10.1051/0004-6361/201323202

    2014 doi

  80. [90]

    Marov, M. Y. 2015, The Fundamentals of Modern Astrophysics, doi: 10.1007/978-1-4614-8730-2

    2015 doi

  81. [91]

    C., Fanson, J., Schiminovich, D., et al

    Martin, D. C., Fanson, J., Schiminovich, D., et al. 2005, The Astrophysical Journal Letters, 619, L1, doi: 10.1086/426387

    2005 doi

  82. [92]

    F., Dale, J

    McLeod, A. F., Dale, J. E., Ginsburg, A., et al. 2015, MNRAS, 450, 1057, doi: 10.1093/mnras/stv680

    2015 doi

  83. [93]

    2012, in Science from the Next Generation Imaging and Spectroscopic Surveys, 43

    Merloni, A. 2012, in Science from the Next Generation Imaging and Spectroscopic Surveys, 43

    2012

  84. [94]

    2016, in Lecture Notes in Physics, Berlin Springer Verlag, ed

    Merloni, A. 2016, in Lecture Notes in Physics, Berlin Springer Verlag, ed. F. Haardt, V. Gorini, U. Moschella, A. Treves, & M. Colpi, Vol. 905, 101, doi: 10.1007/978-3-319-19416-5 4

    2016 doi

  85. [95]

    2024, A&A, 682, A34, doi: 10.1051/0004-6361/202347165

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

    2024 doi

  86. [96]

    J., & Kurtz, M

    Mink, D. J., & Kurtz, M. J. 1998, in Astronomical Society of the Pacific Conference Series, Vol. 145, Astronomical Data Analysis Software and Systems VII, ed. R. Albrecht, R. N. Hook, & H. A. Bushouse, 93

    1998

  87. [97]

    Mulders, G. D. 2018, in Handbook of Exoplanets, ed. H. J. Deeg & J. A. Belmonte, 153, doi: 10.1007/978-3-319-55333-7 153

    2018 doi

  88. [98]

    Nandra, K., Waddell, S. G. H., Liu, T., et al. 2024, arXiv e-prints, arXiv:2401.17300, doi: 10.48550/arXiv.2401.17300

    2024 doi arXiv

  89. [99]

    J., van Duinen, R., et al

    Neugebauer, G., Habing, H. J., van Duinen, R., et al. 1984, The Astrophysical Journal, 278, L1, doi: 10.1086/184209

    1984 doi

  90. [100]

    L., Holtzman, J

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

    2015 doi

  91. [101]

    2012, A&A, 543, A92, doi: 10.1051/0004-6361/201219040

    Noll, S., Kausch, W., Barden, M., et al. 2012, A&A, 543, A92, doi: 10.1051/0004-6361/201219040

    2012 doi

  92. [102]

    2014, A&A, 567, A25, doi: 10.1051/0004-6361/201423908

    Noll, S., Kausch, W., Kimeswenger, S., et al. 2014, A&A, 567, A25, doi: 10.1051/0004-6361/201423908

    2014 doi

  93. [103]

    F., G¨ ansicke, B

    Pala, A. F., G¨ ansicke, B. T., Breedt, E., et al. 2020, MNRAS, 494, 3799, doi: 10.1093/mnras/staa764

    2020 doi

  94. [104]

    2023, OR-Tools, v9.6

    Perron, L., & Furnon, V. 2023, OR-Tools, v9.6. https://developers.google.com/optimization/

    2023

  95. [105]

    Peterson, B. M. 1993, PASP, 105, 247, doi: 10.1086/133140

    1993 doi

  96. [107]

    2021, A&A, 647, A1, doi: 10.1051/0004-6361/202039313

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

    2021 doi

  97. [109]

    R., Winn, J

    Ricker, G. R., Winn, J. N., Vanderspek, R., et al. 2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 014003, doi: 10.1117/1.JATIS.1.1.014003

    2015 doi

  98. [110]

    2018, IF AC-PapersOnLine, 51, 112, doi: https://doi.org/10.1016/j.ifacol.2018.07.097

    Pavone, M. 2018, IF AC-PapersOnLine, 51, 112, doi: https://doi.org/10.1016/j.ifacol.2018.07.097

    2018 doi

  99. [111]

    C., Cales, S., Ruan, J

    Runnoe, J. C., Cales, S., Ruan, J. J., et al. 2016, MNRAS, 455, 1691, doi: 10.1093/mnras/stv2385

    2016 doi

  100. [112]

    E., de Koter, A., et al

    Sana, H., de Mink, S. E., de Koter, A., et al. 2012, Science, 337, 444, doi: 10.1126/science.1223344

    2012 doi

  101. [113]

    E., et al

    Sana, H., de Koter, A., de Mink, S. E., et al. 2013, A&A, 550, A107, doi: 10.1051/0004-6361/201219621

    2013 doi

  102. [114]

    in prep, L VM Data Analysis Pipeline S´ anchez, S

    Sanchez, S. in prep, L VM Data Analysis Pipeline S´ anchez, S. F., Cardiel, N., Verheijen, M. A. W., et al. 2007, A&A, 465, 207, doi: 10.1051/0004-6361:20066620 75 S´ anchez-Gallego, J. R., Sayres, C., Donor, J., et al. 2020, in Society of Photo-Optical Instrumentation Enginee...

    2007 doi

  103. [115]

    Strategies, Processes, and Systems VIII, ed. D. S. Adler, R. L. Seaman, & C. R. Benn, 114490O, doi: 10.1117/12.2561810 S´ anchez-Gallego, J. R., Cherinka, B., Brownstein, J., et al. 2022, in Software and Cyberinfrastructure for Astronomy VII, ed. J. Ibsen & G. Chiozzi, Vol. 12...

    2022 doi

  104. [116]

    2024, arXiv e-prints, arXiv:2407.10788, doi: 10.48550/arXiv.2407.10788

    Saxena, A., Salvato, M., Roster, W., et al. 2024, arXiv e-prints, arXiv:2407.10788, doi: 10.48550/arXiv.2407.10788

    2024 doi arXiv

  105. [117]

    2023, Ph.d., University of Washington, United States – Washington

    Sayres, C. 2023, Ph.d., University of Washington, United States – Washington. https: //www.proquest.com/dissertations-theses/ algorithms-models-methods-sdss-v-wide-field/ docview/2799995603/se-2?accountid=14784

    2023

  106. [118]

    R., Blanton, M

    Sayres, C., S´ anchez-Gallego, J. R., Blanton, M. R., et al. 2021, AJ, 161, 92, doi: 10.3847/1538-3881/abd0f2

    2021 doi

  107. [119]

    R., Blanton, M

    Sayres, C., S´ anchez-Gallego, J. R., Blanton, M. R., et al. 2022, in Ground-based and Airborne Instrumentation for Astronomy IX, ed. C. J

    2022

  108. [120]

    Evans, J. J. Bryant, & K. Motohara, Vol. 12184, International Society for Optics and Photonics (SPIE), 121847K, doi: 10.1117/12.2630507

    doi

  109. [121]

    Schinnerer, E., & Leroy, A. K. 2024, ARA&A, 62, 369, doi: 10.1146/annurev-astro-071221-052651

    2024 doi

  110. [122]

    F., & Finkbeiner, D

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

    2011 doi

  111. [123]

    F., Schlegel, D., BenZvi, S., et al

    Schlafly, E. F., Schlegel, D., BenZvi, S., et al. 2024, The Astronomical Journal, 168, 35, doi: 10.3847/1538-3881/ad4d8c

    2024 doi

  112. [124]

    J., Finkbeiner, D

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

    1998 doi

  113. [125]

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

    Schwab, C., Rakich, A., Gong, Q., 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, 99087H, doi: 10.1117/12.2234411

    2016 doi

  114. [126]

    2024, arXiv e-prints, arXiv:2401.17304, doi: 10.48550/arXiv.2401.17304

    Schwope, A., Kurpas, J., Baecke, P., et al. 2024, arXiv e-prints, arXiv:2401.17304, doi: 10.48550/arXiv.2401.17304

    2024 doi

  115. [127]

    Schwope, A. D. 2018, A&A, 619, A62, doi: 10.1051/0004-6361/201833723

    2018 doi

  116. [128]

    2021, A&A Rv, 29, 4, doi: 10.1007/s00159-021-00132-9

    Serenelli, A., Weiss, A., Aerts, C., et al. 2021, A&A Rv, 29, 4, doi: 10.1007/s00159-021-00132-9

    2021 doi

  117. [129]

    N., Dawson, K

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

    2015 doi

  118. [130]

    J., et al

    Shen, Y., Horne, K., Grier, C. J., et al. 2016, ApJ, 818, 30, doi: 10.3847/0004-637X/818/1/30

    2016 doi

  119. [131]

    B., Horne, K., et al

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

    2019 doi

  120. [132]

    J., Horne, K., et al

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

    2024 doi

  121. [133]

    E., Evans, N

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

    2019 doi

  122. [134]

    F., Cutri, R

    Skrutskie, M. F., Cutri, R. M., Stiening, R., et al. 2006, AJ, 131, 1163, doi: 10.1086/498708

    2006 doi

  123. [135]

    Smartt, S. J. 2009, ARA&A, 47, 63, doi: 10.1146/annurev-astro-082708-101737

    2009 doi

  124. [136]

    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

    2013 doi

  125. [137]

    F., Bennett, C

    Smoot, G. F., Bennett, C. L., Kogut, A., et al. 1992, The Astrophysical Journal, 396, L1, doi: 10.1086/186504

    1992 doi

  126. [138]

    Stassun, K. G. 2019, VizieR Online Data Catalog, IV/38

    2019

  127. [139]

    F., et al

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

    2024 doi arXiv

  128. [140]

    H., Bernardi, M., et al

    Stoughton, C., Lupton, R. H., Bernardi, M., et al. 2002, AJ, 123, 485, doi: 10.1086/324741

    2002 doi

  129. [141]

    R., & Gray, J

    Szalay, A., Thakar, A. R., & Gray, J. 2008, Computing in Science & Engineering, 10, 38, doi: 10.1109/MCSE.2008.18

    2008 doi

  130. [142]

    2021, idies/SpecDash: SpecDash Alpha 0.2.0, v0.2.0-alpha, Zenodo, doi: 10.5281/zenodo.5083750

    Taghizadeh-Popp, M. 2021, idies/SpecDash: SpecDash Alpha 0.2.0, v0.2.0-alpha, Zenodo, doi: 10.5281/zenodo.5083750

    2021 doi

  131. [143]

    2023, SQLxMatch: In-Database Spatial Cross-Match of Astronomical Catalogs, v1.2.0, Zenodo, doi: 10.5281/zenodo.5083706

    Taghizadeh-Popp, M., & Dobos, L. 2023, SQLxMatch: In-Database Spatial Cross-Match of Astronomical Catalogs, v1.2.0, Zenodo, doi: 10.5281/zenodo.5083706

    2023 doi

  132. [144]

    W., Lemson, G., et al

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

    2020

  133. [145]

    1994, Pulp Fiction

    Tarantino, Q., & Avary, R. 1994, Pulp Fiction

    1994

  134. [146]

    1979, AJ, 84, 1511, doi: 10.1086/112569

    Tonry, J., & Davis, M. 1979, AJ, 84, 1511, doi: 10.1086/112569

    1979 doi

  135. [147]

    2010, A&A Rv, 18, 67, doi: 10.1007/s00159-009-0025-1 Tr¨ umper, J

    Torres, G., Andersen, J., & Gim´ enez, A. 2010, A&A Rv, 18, 67, doi: 10.1007/s00159-009-0025-1 Tr¨ umper, J. 1999, A&A, 500, 497 76

    2010 doi

  136. [148]

    2011, in Narrow-Line Seyfert 1 Galaxies and their Place in the Universe, ed

    Vestergaard, M., Denney, K., Fan, X., et al. 2011, in Narrow-Line Seyfert 1 Galaxies and their Place in the Universe, ed. L. Foschini, M. Colpi, L. Gallo, D. Grupe, S. Komossa, K. Leighly, & S. Mathur, 38, doi: 10.22323/1.126.0038 von Spaeth, O. 2000, Centaurus, 42, 159, doi: ...

    2011

  137. [149]

    Waddell, S. G. H., Nandra, K., Buchner, J., et al. 2023, arXiv e-prints, arXiv:2306.00961, doi: 10.48550/arXiv.2306.00961

    2023 doi arXiv

  138. [150]

    Wang, J., & Fischer, D. A. 2015, AJ, 149, 14, doi: 10.1088/0004-6256/149/1/14

    2015 doi

  139. [151]

    A., Horch, E

    Wang, J., Fischer, D. A., Horch, E. P., & Huang, X. 2015, ApJ, 799, 229, doi: 10.1088/0004-637X/799/2/229

    2015 doi

  140. [152]

    R., & Stauffer, F

    Brownstein, J. R., & Stauffer, F. 2015, PASP, 127, 397, doi: 10.1086/680999

    2015 doi

  141. [153]

    2020, in Astronomical Society of the Pacific Conference Series, Vol

    Weijmans, A., Brownstein, J., Thakar, A., et al. 2020, in Astronomical Society of the Pacific Conference Series, Vol. 527, Astronomical Data Analysis Software and Systems XXIX, ed. R. Pizzo, E. R. Deul, J. D. Mol, J. de Plaa, & H. Verkouter, 399

    2020

  142. [154]

    S., et al

    Weijmans, A.-M., Blanton, M., Bolton, A. S., et al. 2019, in Astronomical Society of the Pacific Conference Series, Vol. 521, Astronomical Data Analysis Software and Systems XXVI, ed. M. Molinaro, K. Shortridge, & F. Pasian, 177

    2019

  143. [155]

    2015, A&A, 582, A114, doi: 10.1051/0004-6361/201526529

    Kollatschny, W., et al. 2015, A&A, 582, A114, doi: 10.1051/0004-6361/201526529

    2015 doi

  144. [156]

    J., Hall, P

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

    2024 doi

  145. [157]

    Wild, V., & Hewett, P. C. 2005, MNRAS, 358, 1083, doi: 10.1111/j.1365-2966.2005.08844.x

    2005

  146. [158]

    W., Lintott, C

    Willett, K. W., Lintott, C. J., Bamford, S. P., et al. 2013, MNRAS, 435, 2835, doi: 10.1093/mnras/stt1458

    2013 doi

  147. [159]

    2016, Scottish Journal of Performance, 3,1, 59, doi: 10.14439/sjop.2016.0301.05

    Fitzpatrick, T. 2016, Scottish Journal of Performance, 3,1, 59, doi: 10.14439/sjop.2016.0301.05

    2016

  148. [160]

    C., Hearty, F

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

    2019 doi

  149. [161]

    Evans, J. J. Bryant, & K. Motohara, 121847H, doi: 10.1117/12.2630231

    doi

  150. [162]

    C., Rocheleau, D., Fox, J., et al

    Wilson, J. C., Rocheleau, D., Fox, J., et al. 2022b, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 12188, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 121885W, doi: 10.1117/12.2630327

    doi

  151. [163]

    Swank, J. H. 1982, ApJ, 255, 111, doi: 10.1086/159809

    1982 doi

  152. [164]

    L., Eisenhardt, P

    Wright, E. L., Eisenhardt, P. R. M., Mainzer, A. K., et al. 2010, The Astronomical Journal, 140, 1868, doi: 10.1088/0004-6256/140/6/1868

    2010 doi

  153. [165]

    Yakut, K., & Eggleton, P. P. 2005, ApJ, 629, 1055, doi: 10.1086/431300

    2005 doi

  154. [166]

    2023, ApJS, 264, 9, doi: 10.3847/1538-4365/ac9ea8

    Yang, Q., & Shen, Y. 2023, ApJS, 264, 9, doi: 10.3847/1538-4365/ac9ea8

    2023 doi

  155. [168]

    G., Adelman, J., Anderson, John E., J., et al

    York, D. G., Adelman, J., Anderson, John E., J., et al. 2000b, AJ, 120, 1579, doi: 10.1086/301513

    doi

  156. [169]

    2022, ApJL, 939, L16, doi: 10.3847/2041-8213/ac9a47 —

    Zeltyn, G., Trakhtenbrot, B., Eracleous, M., et al. 2022, ApJL, 939, L16, doi: 10.3847/2041-8213/ac9a47 —. 2024, ApJ, 966, 85, doi: 10.3847/1538-4357/ad2f30

    2022 doi

  157. [170]

    2024, ApJS, 274, 42, doi: 10.3847/1538-4365/ad7d01

    Zhuang, M.-Y., Yang, Q., Shen, Y., et al. 2024, ApJS, 274, 42, doi: 10.3847/1538-4365/ad7d01

    2024 doi

  158. [171]

    Zinnecker, H., & Yorke, H. W. 2007, ARA&A, 45, 481, doi: 10.1146/annurev.astro.44.051905.092549

    2007 arXiv

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