First joint 2PCF+3PCF full-shape analysis on BOSS DR12 real data improves σ(h) by ~29%, σ(ω_cdm) by ~10%, and σ(A_s) by ~24% over 2PCF alone via extra BAO information in 3PCF triangles.
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9 Pith papers cite this work. Polarity classification is still indexing.
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representative citing papers
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.
No evidence for cosmological parity violation is found in the first kurto-spectrum analysis of BOSS DR12 and DESI DR1 luminous red galaxies.
DESI DR2 identifies 50,088 galaxies with moderate and 27,420 with strong evidence for down-the-barrel NaI D absorption revealing inflows at ~20 km/s and multiple accretion pathways at z < 0.6.
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 mass sum to < 0.071 eV.
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.
Forecasts show that line-of-sight dependent 3PCF tightens sigma_8 constraints by a factor of 5 over 2PCF alone for Roman ELG and DESI LRG samples on scales <80 Mpc/h using AbacusSummit simulations.
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.
The shape of photometric galaxy redshift PDFs can shift the BAO feature position in correlation functions, with performance varying by estimator and parameter (ANNz2 closer to Planck for some cases, DNF for w0 with sufficient data).
citing papers explorer
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First full-shape joint analysis of the two- and three-point correlation functions on real data: $\Lambda$CDM cosmological constraints from BOSS DR12
First joint 2PCF+3PCF full-shape analysis on BOSS DR12 real data improves σ(h) by ~29%, σ(ω_cdm) by ~10%, and σ(A_s) by ~24% over 2PCF alone via extra BAO information in 3PCF triangles.
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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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Testing parity with composite-field spectra of BOSS and DESI luminous red galaxies
No evidence for cosmological parity violation is found in the first kurto-spectrum analysis of BOSS DR12 and DESI DR1 luminous red galaxies.
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Peering down the barrel with DESI DR2: 10 000+ inflows at $z$ < 0.6 reveal how galaxies accrete cold gas
DESI DR2 identifies 50,088 galaxies with moderate and 27,420 with strong evidence for down-the-barrel NaI D absorption revealing inflows at ~20 km/s and multiple accretion pathways at z < 0.6.
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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 mass sum to < 0.071 eV.
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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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Increasing the sensitivity of full-shape galaxy clustering measurements in configuration-space with three-point statistics
Forecasts show that line-of-sight dependent 3PCF tightens sigma_8 constraints by a factor of 5 over 2PCF alone for Roman ELG and DESI LRG samples on scales <80 Mpc/h using AbacusSummit simulations.
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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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Influence of photometric galaxies redshift distribution in BAO estimation
The shape of photometric galaxy redshift PDFs can shift the BAO feature position in correlation functions, with performance varying by estimator and parameter (ANNz2 closer to Planck for some cases, DNF for w0 with sufficient data).