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Data Release 1 of the Dark Energy Spectroscopic Instrument

DESI Collaboration, M. Abdul-Karim, A. G. Adame, D. Aguado, J. Aguilar, S. Ahlen, S. Alam, G. Aldering, D. M. Alexander, R. Alfarsy, L. Allen, C. Allende Prieto, O. Alves, A. Anand, U. Andrade, E. Armengaud, S. Avila, A. Aviles, H. Awan, S. Bailey, A. Baleato Lizancos, O. Ballester, A. Bault, J. Bautista, S. BenZvi, L. Beraldo e Silva, J. R. Bermejo-Climent, F. Beutler, D. Bianchi, C. Blake, R. Blum, A. S. Bolton, M. Bonici, S. Brieden, A. Brodzeller, D. Brooks, E. Buckley-Geer, E. Burtin, R. Canning, A. Carnero Rosell, A. Carr, P. Carrilho, L. Casas, F. J. Castander, R. Cereskaite, J. L. Cervantes-Cota, E. Chaussidon, J. Chaves-Montero, S. Chen, X. Chen, T. Claybaugh, S. Cole, A. P. Cooper, M. -C. Cousinou, A. Cuceu, T. M. Davis, K. S. Dawson, R. de Belsunce, R. de la Cruz, A. de la Macorra, A. de Mattia, N. Deiosso, J. Della Costa, R. Demina, U. Demirbozan, J. DeRose, A. Dey, B. Dey, J. Ding, Z. Ding, P. Doel, K. Douglass, M. Dowicz, H. Ebina, J. Edelstein, D. J. Eisenstein, W. Elbers, N. Emas, S. Escoffier, P. Fagrelius, X. Fan, K. Fanning, V. A. Fawcett, E. Fernández-García, S. Ferraro, N. Findlay, A. Font-Ribera, J. E. Forero-Romero, D. Forero-Sánchez, C. S. Frenk, B. T. Gänsicke, L. Galbany, J. García-Bellido, C. Garcia-Quintero, L. H. Garrison, E. Gaztañaga, H. Gil-Marín, O. Y. Gnedin, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, V. Gonzalez-Perez, C. Gordon, O. Graur, D. Green, D. Gruen, R. Gsponer, C. Guandalin, G. Gutierrez, J. Guy, C. Hahn, J. J. Han, J. Han, S. He, H. K. Herrera-Alcantar, K. Honscheid, J. Hou, C. Howlett, D. Huterer, V. Iršič, M. Ishak, A. Jacques, J. Jimenez, Y. P. Jing, B. Joachimi, S. Joudaki, R. Joyce, E. Jullo, S. Juneau, N. G. Karaçaylı, T. Karim, R. Kehoe, S. Kent, A. Khederlarian, D. Kirkby, T. Kisner, F. -S. Kitaura, N. Kizhuprakkat, H. Kong, S. E. Koposov, A. Kremin, A. Krolewski, O. Lahav, Y. Lai, C. Lamman, T. -W. Lan, M. Landriau, D. Lang, J. U. Lange, J. Lasker, J. M. Le Goff, L. Le Guillou, A. Leauthaud, M. E. Levi, S. Li, T. S. Li, K. Lodha, M. Lokken, Y. Luo, C. Magneville, M. Manera, C. J. Manser, D. Margala, P. Martini, M. Maus, J. McCullough, P. McDonald, G. E. Medina, L. Medina-Varela, A. Meisner, J. Mena-Fernández, A. Menegas, M. Mezcua, R. Miquel, P. Montero-Camacho, J. Moon, J. Moustakas, A. Muñoz-Gutiérrez, D. Muñoz-Santos, A. D. Myers, J. Myles, S. Nadathur, J. Najita, L. Napolitano, J. A. Newman, F. Nikakhtar, R. Nikutta, G. Niz, H. E. Noriega, N. Padmanabhan, E. Paillas, N. Palanque-Delabrouille, A. Palmese, J. Pan, Z. Pan, D. Parkinson, J. Peacock, W. J. Percival, A. Pérez-Fernández, I. Pérez-Ràfols, P. Peterson, J. Piat, M. M. Pieri, M. Pinon, C. Poppett, A. Porredon, F. Prada, R. Pucha, F. Qin, D. Rabinowitz, A. Raichoor, C. Ramírez-Pérez, S. Ramirez-Solano, M. Rashkovetskyi, C. Ravoux, A. H. Riley, A. Rocher, C. Rockosi, J. Rohlf, A. J. Ross, G. Rossi, R. Ruggeri, V. Ruhlmann-Kleider, C. G. Sabiu, K. Said, A. Saintonge, L. Samushia, E. Sanchez, N. Sanders, C. Saulder, E. F. Schlafly, D. Schlegel, D. Scholte, M. Schubnell, H. Seo, A. Shafieloo, R. Sharples, J. Silber, M. Siudek, A. Smith, D. Sprayberry, J. Suárez-Pérez, J. Swanson, T. Tan, G. Tarlé, P. Taylor, G. Thomas, R. Tojeiro, R. J. Turner, W. Turner, L. A. Ureña-López, R. Vaisakh, M. Valluri, M. Vargas-Magaña, L. Verde, M. Walther, B. Wang, M. S. Wang, W. Wang, B. A. Weaver, N. Weaverdyck, R. H. Wechsler, M. White, M. Wolfson, J. Yang, C. Yèche, S. Youles, J. Yu, S. Yuan, E. A. Zaborowski, P. Zarrouk, H. Zhang, C. Zhao, R. Zhao, Z. Zheng, R. Zhou, H. Zou, S. Zou, Y. Zu

TL;DR

This paper presents DESI Data Release 1 (DR1), the first public release following the Early Data Release, comprising data from the first 13 months of the DESI main survey and a uniform reprocessing of the Survey Validation data. It documents the DESI instrument and target-selection strategy, the Data Reduction pipeline (Iron production), and the comprehensive suite of data products, including spectra, redshifts, large-scale structure catalogs, and extensive value-added catalogs. DR1 encompasses roughly 18.7 million objects with high-confidence redshifts across 9,739 deg$^{2}$, detailing performance metrics, sample distributions, and data-access pathways (files and databases) with tutorials and licensing. The release enables both cosmological analyses (BAO, full-shape, Ly$$ forest) and a wide array of astrophysical studies, while establishing a framework for reproducible, scalable data processing and public access for future DESI data releases.

Abstract

In 2021 May the Dark Energy Spectroscopic Instrument (DESI) collaboration began a 5-year spectroscopic redshift survey to produce a detailed map of the evolving three-dimensional structure of the universe between $z=0$ and $z\approx4$. DESI's principle scientific objectives are to place precise constraints on the equation of state of dark energy, the gravitationally driven growth of large-scale structure, and the sum of the neutrino masses, and to explore the observational signatures of primordial inflation. We present DESI Data Release 1 (DR1), which consists of all data acquired during the first 13 months of the DESI main survey, as well as a uniform reprocessing of the DESI Survey Validation data which was previously made public in the DESI Early Data Release. The DR1 main survey includes high-confidence redshifts for 18.7M objects, of which 13.1M are spectroscopically classified as galaxies, 1.6M as quasars, and 4M as stars, making DR1 the largest sample of extragalactic redshifts ever assembled. We summarize the DR1 observations, the spectroscopic data-reduction pipeline and data products, large-scale structure catalogs, value-added catalogs, and describe how to access and interact with the data. In addition to fulfilling its core cosmological objectives with unprecedented precision, we expect DR1 to enable a wide range of transformational astrophysical studies and discoveries.

Data Release 1 of the Dark Energy Spectroscopic Instrument

TL;DR

This paper presents DESI Data Release 1 (DR1), the first public release following the Early Data Release, comprising data from the first 13 months of the DESI main survey and a uniform reprocessing of the Survey Validation data. It documents the DESI instrument and target-selection strategy, the Data Reduction pipeline (Iron production), and the comprehensive suite of data products, including spectra, redshifts, large-scale structure catalogs, and extensive value-added catalogs. DR1 encompasses roughly 18.7 million objects with high-confidence redshifts across 9,739 deg, detailing performance metrics, sample distributions, and data-access pathways (files and databases) with tutorials and licensing. The release enables both cosmological analyses (BAO, full-shape, Ly forest) and a wide array of astrophysical studies, while establishing a framework for reproducible, scalable data processing and public access for future DESI data releases.

Abstract

In 2021 May the Dark Energy Spectroscopic Instrument (DESI) collaboration began a 5-year spectroscopic redshift survey to produce a detailed map of the evolving three-dimensional structure of the universe between and . DESI's principle scientific objectives are to place precise constraints on the equation of state of dark energy, the gravitationally driven growth of large-scale structure, and the sum of the neutrino masses, and to explore the observational signatures of primordial inflation. We present DESI Data Release 1 (DR1), which consists of all data acquired during the first 13 months of the DESI main survey, as well as a uniform reprocessing of the DESI Survey Validation data which was previously made public in the DESI Early Data Release. The DR1 main survey includes high-confidence redshifts for 18.7M objects, of which 13.1M are spectroscopically classified as galaxies, 1.6M as quasars, and 4M as stars, making DR1 the largest sample of extragalactic redshifts ever assembled. We summarize the DR1 observations, the spectroscopic data-reduction pipeline and data products, large-scale structure catalogs, value-added catalogs, and describe how to access and interact with the data. In addition to fulfilling its core cosmological objectives with unprecedented precision, we expect DR1 to enable a wide range of transformational astrophysical studies and discoveries.

Paper Structure

This paper contains 48 sections, 7 figures.

Table of Contents

  1. Introduction
  2. The First Year of DESI Data
  3. A High-Level Guide to DESI and Data Release 1
  4. Data Acquisition
  5. Dark Energy Spectroscopic Instrument
  6. Target Selection
  7. Survey Operations
  8. The Main Survey
  9. Survey Validation
  10. Special Tiles
  11. Data Reduction and Data Products
  12. From Raw Spectra to Redshifts
  13. Spectral Extraction and Calibration
  14. Redshifts and Spectral Classifications
  15. Pipeline Improvements and Algorithmic Performance
  16. ...and 33 more sections

Figures (7)

  • Figure 1: A slice of the universe mapped by DR1 drawn from a small wedge of the DESI footprint between $\pm5\arcdeg$ in declination out to $z\approx4$. We render the four major extragalactic samples---bright galaxy survey (BGS) galaxies, luminous red galaxies (LRG), emission-line galaxies (ELG), and QSOs---using yellow, orange, blue, and green points, respectively. Within each target class, the shade of the color maps to declination (lighter colors correspond to higher declination). The inset shows a subset of the BGS survey extending out to redshift $z=0.2$, highlighting the large-scale structure traced by galaxies in the densest survey region. For reference, this small wedge of the BGS survey represents less than 0.1% of the comoving cosmological volume in DR1. Also note the black streaks of apparent missing points (most visible at right ascensions between 40$\arcdeg$--300$\arcdeg$), which are due to incomplete survey coverage in DR1 which will be populated in future data releases (see §\ref{['sec:sample']}).
  • Figure 2: Distribution of Milky Way stars in DESI DR1 observed as part of the Milky Way survey. The colors of individual points represent the spectroscopically inferred iron abundance, [Fe/H], as measured using the RVSPecFit pipeline koposov24a. The distances to individual stars have been derived using a neural network with stellar parameters as inputs. The thin curves represent the disk stellar mass density contours from the price-whelan17aMilkyWayPotential2022 Galactic model. This visualization illustrates the phenomenal size and scale of the DESI stellar survey, the clear negative iron abundance gradient (from the inner disk to the outer stellar halo), as well as the presence of the Sagittarius stream majewski03a, visible as more orange-tinted points at $(x,z)\approx (-10,+40)$ kpc and $(x,z)\approx(20,-20$) kpc above and below the Galactic disk, respectively. The map also shows high-metallicity stars extending above the disk at $x=20$ kpc caused by the Monoceros "stream" structure juric08anewberg02a.
  • Figure 3: Completeness of the DESI main survey based on observations between 2021 May 14 and 2022 June 13 for the bright, dark, and backup programs (from top to bottom). Dark-shaded areas are complete, while white areas have not yet been observed. We use an equal-area Mollweide projection in equatorial coordinates and indicate the per-program DESI main-survey footprint with a thick black curve. As discussed in §\ref{['sec:main']}, the bright- and dark-time footprints are identical, while the backup program footprint extends to lower Galactic latitude. The dashed line shows the Galactic plane, the dotted line shows the ecliptic plane, and we also display the Galactic reddening level outside the DESI footprint in gray.
  • Figure 4: Number of unique SV and main survey tiles in DR1 as a function of night (see Table \ref{['tab:survey_nights_tiles_exp']}). Note that tiles can be observed on multiple nights and that the vertical dashed line indicates the start of the main survey on 2021 May 14. The large gap in observations between 2021 July 10 and 2021 September 20 was due to a major upgrade of the focal-plane electronics.
  • Figure 5: Surface density of all unique targets with good redshifts observed in the bright, dark, and backup main-survey programs (first three panels), and in SV (lower-right panel), rendered using an equal-area Mollweide projection in equatorial coordinates. In each panel, the thin gray curve represents the Galactic plane, which divides the DESI footprint into its North and South Galactic Cap regions (shown as thick black outlines; see Figure \ref{['fig:progress']}). The density of targets in the bright- and dark-time programs extend to above 2000 deg$^{-2}$, compared to the (as-designed) $>8000$ deg$^{-2}$ surface density of targets in SV.
  • ...and 2 more figures