First observational detection of the moving lens effect via cross-correlation of ACT CMB temperature with DESI galaxies, yielding amplitude b_ML = 1.24 ± 0.26 at 4.8σ consistent with halo-model prediction.
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The DESI Experiment Part I: Science,Targeting, and Survey Design
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DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$\alpha$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions.
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- abstract DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tra
- background recover unbiased measurements of the angular diameter distance, the Hubble parameter, and the growth of structure across all redshift bins, in the same range of scales as the EFT model, and obtain mν <0.63(0.36) eV at 95(68)% C.L. when Planck priors are included. I. INTRODUCTION The study of the large-scale structure (LSS) of the Uni- verse is entering a golden era. A new generation of galaxy surveys-including DESI [1] and Euclid [ 2], -is mapping the three-dimensional distribution of matter ove
- background 7 Final thoughts 21 8 Data Availability 22 A Author Affiliations 30 1 Introduction and summary of main results The Dark Energy Spectroscopic Instrument (DESI), a wide-angle instrument in the Mayall telescope at Kitt Peak [1], Arizona, provides an unprecedented capability to test modifications to Einstein equations during the history of the universe [2], in particular using its most recent release of extra-galactic targets with accurate redshift measurements [3]. At the background level, the DESI
- background ing from the early 2000s, a series of modern spectroscopic surveys, from the spectroscopic component of the SDSS 2) https://www.stsci.edu/hst 3) https://www.eso.org/public/teles-instr/paranal-observatory/vlt/ 4) https://keckobservatory.org/ Cai, et al., et al. Sci. China-Phys. Mech. Astron.January (2023) V ol. 66 No. 1000000-4 [20-22], LAMOST [13], to Dark Energy Spectroscopic In- strument (DESI) [36], Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) [37], Subaru Prime Focus Spectro- graph
- background momentum triangle encodes the specific generation mechanism. A detection of a local-shape primordial bispectrum signal, which peaks in the squeezed limit (k1 ≪k 2, k 3), would rule out the entire class of single-field inflationary models. Current CMB constraints onf loc NL are insufficient to discriminate between inflationary models. The tightest bound from Planck yieldsfloc NL =−0.9±5.1[28], and future CMB ex- periments will not substantially improve this result due to cosmic variance [13]. Rea
- background 42]-at0.6< z <1.6provides a concrete realization. With up to 4 tracers and 10 cross- spectra per redshift bin, the overlap volume functions as a calibration laboratory for the EFT parameters that limit the full DESI analysis. The weaker finger-of-god (FoG) contamination expected in PFS samples motivates an asymmetric scale cut,k PFS max > k DESI max [37]1. This paper is organized as follows. Section 2 describes the multi-survey prior mech- anism. Section 3 details the Fisher forecast setup, incl
- background At a given redshift, the kinetic en- Astrid: Realistic BH Dynamics Weakens Baryonic Suppression5 0 101 102 r [kpc/h] 0.5 1.0 1.5 2.0 2.5 3.0 3.5 ρhydro(r)/ρDMO(r) R500c = 69.2 kpc /h M500c ∈ [1011,1012) M ⊙ /h 5.13 SV-DF SV-Repos SV-DF-S SV-Repos-S 0 101 102 r [kpc/h] R500c = 156.8 kpc /h M500c ∈ [1012,1013) M ⊙ /h 5.15 0 101 102 103 r [kpc/h] R500c = 318.7 kpc /h M500c ∈ [1013,1014) M ⊙ /h 5.17 Figure 2.Halo density profile ratios of halos in the SV hydrodynamical simulations to their matched D
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citing papers explorer
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First detection of the moving lens effect with ACT and DESI LS
First observational detection of the moving lens effect via cross-correlation of ACT CMB temperature with DESI galaxies, yielding amplitude b_ML = 1.24 ± 0.26 at 4.8σ consistent with halo-model prediction.
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Joint inference of weak lensing convergence map and cosmology with diffusion models
A transformer-based diffusion model learns the joint distribution of convergence maps and cosmology from log-normal weak lensing simulations and generates calibrated posterior samples matching MCMC results.
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Galaxy Power Spectrum at Two-Loop Order: Implications for Weak Lensing Surveys and New Physics
Two-loop EFT galaxy power spectrum achieves per-mille agreement with simulations to k=0.85 h/Mpc and yields three times narrower unbiased σ8 errors than linear theory.
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A hierarchical Bayesian framework for cosmology using Type 1 AGN variability
A hierarchical Bayesian framework that uses the empirical anti-correlation between AGN variability amplitude and luminosity to infer cosmological parameters from moderate-baseline light curves via importance reweighting.
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Augmented Correlation Functions for Spectroscopic Galaxy Surveys
Augmented correlation functions extend the two-point correlation function with latent dimensions derived from the galaxy field to isolate additional clustering information in spectroscopic surveys.
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Fewer simulations, sharper covariances: Reducing mock covariance noise with Zeldovich approximation control variates
Control variates with Zeldovich mocks reduce covariance matrix variance by up to an order of magnitude on large scales in DESI-like mocks.
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Field-level multi-tracers simulation-based inference of cosmological parameters from 3D maps
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SDSS-V: Revealing a weak accretion state in X-ray selected red quasars
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Probing nonlinear structure formation beyond $\Lambda$CDM with the LSS bootstrap: a joint power spectrum and bispectrum analysis
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Satellite Metallicity Enhancement I: Suppressed Star Formation, Stellar Mass Loss, and Enriched Inflow of DESI and EAGLE Galaxies around Massive Clusters
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Constraining the Galactic bar using the M92 stellar stream
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Effective Field Theory of Large Scale Structure and Newtonian Motion Gauges
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Informative Priors on Primordial Non-Gaussianity Bias $b_{\phi}$ From Galaxy Formation
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