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The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
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We describe the spectroscopic data processing pipeline of the Dark Energy Spectroscopic Instrument (DESI), which is conducting a redshift survey of about 40 million galaxies and quasars using a purpose-built instrument on the 4-m Mayall Telescope at Kitt Peak National Observatory. The main goal of DESI is to measure with unprecedented precision the expansion history of the Universe with the Baryon Acoustic Oscillation technique and the growth rate of structure with Redshift Space Distortions. Ten spectrographs with three cameras each disperse the light from 5000 fibers onto 30 CCDs, covering the near UV to near infrared (3600 to 9800 Angstrom) with a spectral resolution ranging from 2000 to 5000. The DESI data pipeline generates wavelength- and flux-calibrated spectra of all the targets, along with spectroscopic classifications and redshift measurements. Fully processed data from each night are typically available to the DESI collaboration the following morning. We give details about the pipeline's algorithms, and provide performance results on the stability of the optics, the quality of the sky background subtraction, and the precision and accuracy of the instrumental calibration. This pipeline has been used to process the DESI Survey Validation data set, and has exceeded the project's requirements for redshift performance, with high efficiency and a purity greater than 99 percent for all target classes.
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Cited by 40 Pith papers
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Clustering of high-redshift quasars with DESI DR2
DESI DR2 quasar sample yields bias b_Q(z=2.48)=3.61 that evolves as b(z)=0.230[(1+z)^2-6.565]+2.394, consistent with constant ~10^12 M_sun halo mass and weak luminosity dependence at fixed redshift.
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Measurement of the galaxy-velocity power spectrum of DESI tracers with the kinematic Sunyaev-Zeldovich effect using DESI DR2 and ACT DR6
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.
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Cosmological analysis of the DESI DR1 Lyman alpha 1D power spectrum
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.
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DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints
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.
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DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations
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.
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DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars
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.
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Lyman-$\alpha$ forest holography: 3D predictions from 1D measurements
One-dimensional Lyman-α forest power spectrum measurements, propagated through the ForestFlow emulator, predict three-dimensional clustering that matches DESI BAO and ACCEL-2 simulation results.
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DESI DR2 Results IV: Alcock-Paczy\'nski Measurements from the Lyman Alpha Forest and Cosmological Constraints
The full shape of DESI DR2 Lyman-alpha forest correlations constrains the distance ratio DM/DH at z=2.33 to 1.0%, twice as precise as BAO alone.
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DESI DR2 Results IV: Alcock-Paczy\'nski Measurements from the Lyman Alpha Forest and Cosmological Constraints
DESI DR2 Lyman-alpha forest full-shape correlations yield a 1% Alcock-Paczyński measurement at z=2.33 and 0.8% distance ratio constraints.
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Probing the matter-dominated expansion with multi-redshift Lyman-$\alpha$ BAO from DESI DR2
DESI DR2 Lyman-alpha BAO measurements split into three redshift bins trace the expansion rate H(z) over z≈2.1–2.8, yielding a power-law slope n=1.34±0.16 consistent with matter-dominated expansion.
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First planetesimals from DESI DR1: 12 highly metal-rich white dwarfs
Twelve white dwarfs from DESI DR1 have accreted debris resembling inner-Solar-System rock, with two systems likely accreting water-rich planetesimals.
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Assessing the large-scale angular clustering of UNIONS Lyman Break Galaxies via cross-correlations
UNIONS Lyman-break galaxy auto-clustering is unusable at large scales due to imaging systematics, but LBG x CMB-lensing and LBG x quasar cross-spectra are measured robustly, with amplitudes consistent with predictions.
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Assessing the large-scale angular clustering of UNIONS Lyman Break Galaxies via cross-correlations
UNIONS LBGs yield robust cross-power spectra with Planck CMB lensing and DESI/Quaia quasars at amplitudes matching theory, despite systematics that render the auto-spectrum unusable.
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Structural Diversity Among the Milky Way's Dwarf Spheroidal Satellites
Where model selection is decisive, the flexible αβγ density model is preferred over Plummer/Sersic/exponential, revealing diverse β and γ across dSphs and larger uncertainties in structural parameters.
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Weak Evolution of Cosmic Atomic Hydrogen over the Past 4.5 Billion Years
Combining FAST and DESI data for 2.5 million galaxies shows cosmic atomic hydrogen density declined by only a factor of 1.35 over 4.5 Gyr, far less than the 2.46-fold decline in star formation.
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The 3D clustering of Lyman Alpha Emitters measured with DESI
DESI LAE clustering measurements give a linear bias of 2.31-2.62 with constraints on radiative transfer effects and halo occupation from correlation functions and power spectra.
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Precision Kinematic Sunyaev--Zel'dovich Measurements Across Halo Mass and Redshift with DESI DR2 and ACT DR6: Part I. Luminous Red Galaxies
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.
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DESI DR2 Baryon Acoustic Oscillations from the Lyman Alpha Forest Multipoles
A Legendre-multipole BAO analysis of the DESI DR2 Lyα forest yields αiso=0.9997±0.0096 and αAP=0.9986±0.0276, consistent with the baseline, using an unsmoothed positive-definite covariance.
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The Linear Point Standard Ruler with DESI DR1 and DR2 Data
Linear-point distance measurements on DESI DR1/DR2 galaxy samples agree with template-based BAO measurements once a cosmology-dependent smearing correction is applied.
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Parity-odd Four-Point Correlation Function from DESI Data Release 1 Luminous Red Galaxy Sample
The parity-odd four-point correlation function measured in DESI DR1 LRGs is consistent with zero after correcting for survey-induced covariance mismatches.
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Full calibration of the tomographic redshift distribution from the HSC PDR3 Shape Catalog with DESI
Clustering redshifts with DESI DR1/DR2 calibrate all four HSC Y3 tomographic bins; bins 3 and 4 shift to higher redshift (dz3=-0.039, dz4=-0.048) but less than cosmic shear analyses implied.
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$H_0$ Without the Sound Horizon (or Supernovae): A 2% Measurement in DESI DR1
A heuristic power-spectrum rescaling applied to DESI DR1 BAO data plus CMB acoustic scale anchor yields H0 values of 69.2 to 70.3 km/s/Mpc at sub-2% precision across three independent late-time datasets.
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Probing the limits of cosmological information from the Lyman-$\alpha$ forest 2-point correlation functions
Using idealized synthetic data, knowing the true continuum in Lyα forest auto- and cross-correlations reduces uncertainties on the AP parameter and Ω_m by ~10%, with extension to 240 h^{-1}Mpc scales adding up to ~15%...
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Fiducial-Cosmology-dependent systematics for the DESI 2024 Full-Shape Analysis
Changing the assumed fiducial cosmology in DESI DR1 full-shape mock analyses shifts inferred parameters by at most 0.22 sigma in full-modeling and 0.45 sigma in ShapeFit, both within the survey's statistical uncertainty.
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Measurement of Parity-Violating Modes of the Dark Energy Spectroscopic Instrument (DESI) Year 1 Luminous Red Galaxies' 4-Point Correlation Function
DESI's first parity-violation search shows a strong auto-correlation signal that disappears when the sky is split into patches, pointing to underestimated mocks' variance rather than new physics.
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DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements
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...
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DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars
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.
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DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman Alpha Forest
DESI measures BAO from the Lyα forest at z_eff=2.33, reporting H(z) = (239.2 ± 4.8) (147.09 Mpc/rd) km/s/Mpc and DM(z) = (5.84 ± 0.14) (rd/147.09 Mpc) Gpc.
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Validation of the DESI DR2 Ly$\alpha$ forest full-shape analysis
The DESI DR2 Lyman-alpha forest full-shape analysis passes validation for BAO and Alcock-Paczynski parameters on hundreds of mocks and blinded data, while the fσ8 growth-rate measurement is found biased and excluded.
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Validation of the DESI DR2 Ly$\alpha$ forest full-shape analysis
The DESI DR2 Lyman-alpha full-shape analysis passes validation for BAO and Alcock-Paczynski parameters on 400 mocks and blinded data, while f-sigma-8 is rejected due to a roughly 10% mock bias.
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The DESI View of the Faint Radio Source Population in LoTSS DR2
Probabilistic spectroscopic classification of 251k LoTSS radio sources yields the largest high-confidence sample and confirms LERGs accrete below ~1% Eddington while HERGs accrete above it.
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FolpsD: combining EFT and phenomenological approaches for joint power spectrum and bispectrum analyses
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...
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Local primordial non-Gaussianity using cross-correlations of DESI tracers
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.
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Combined tracer analysis for DESI 2024 BAO
Combining LRG and ELG tracers with bias weighting improves BAO constraints by 11% on alpha_iso and 7% on alpha_AP in DESI DR1 data for the 0.8<z<1.1 bin.
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Constraints on Neutrino Physics from DESI DR2 BAO and DR1 Full Shape
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.
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Cosmological constraints from the DESI DR1 Bispectrum Full-Shape and DR2 BAO
DESI DR1 bispectrum plus DR2 BAO data raise σ8 and S8 by ~1.1-1.2σ while tightening uncertainties, shift DESI-only w0waCDM toward ΛCDM, produce a 2.8σ deviation from ΛCDM when combined with CMB, and yield a neutrino m...
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DESI Data Release 2 ELGs: Property-dependent subsamples, imaging systematics, and clustering
Property-dependent systematic weights derived separately on ELG subsamples, with separate DES footprint treatment, mitigate spurious clustering in ~10% of subsamples but are not optimal for the full sample.
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Testing Scale-Dependent Modified Gravity with DESI DR1
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.
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Extended Dark Energy analysis using DESI DR2 BAO measurements
Extended analysis of DESI DR2 data confirms robust evidence for dynamical dark energy with phantom crossing preference, stable under parametric and non-parametric modeling.
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DESI DR2 Results I: Baryon Acoustic Oscillations from the Lyman Alpha Forest
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.
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