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.
An analytic model for the spatial clustering of dark matter haloes
12 Pith papers cite this work. Polarity classification is still indexing.
12
Pith papers citing it
abstract
We develop a simple analytic model for the gravitational clustering of dark matter haloes to understand how their spatial distribution is biased relative to that of the mass. The statistical distribution of dark haloes within the initial density field (assumed Gaussian) is determined by an extension of the Press-Schechter formalism. Modifications of this distribution caused by gravitationally induced motions are treated using a spherical collapse approximation. We test this model against results from a variety of N-body simulations, and find that it gives an accurate description of a bias function. This bias function is sufficient to calculate the cross-correlation between dark haloes and mass, and again we find excellent agreement between simulation results and analytic predictions. Because haloes are spatially exclusive, the variance in the count of objects within spheres of fixed radius and overdensity is significantly smaller than the Poisson value. This seriously complicates any analytic calculation of the autocorrelation function of dark halos. Our simulation results show that this autocorrelation function is proportional to that of the mass over a wide range in $R$, even including scales where both functions are significantly greater than unity. The constant of proportionality is very close to that predicted on large scales by the analytic model. This result permits an entirely analytic estimate of the autocorrelation function of dark haloes. We use our model to study how the distribution of galaxies may be biased with respect to that of the mass. In conjunction with other data these techniques should make it possible to measure the amplitude of cosmic mass fluctuations and the density of the Universe.
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Tensor-induced non-Gaussianity from primordial gravitational waves generates a unique scale-dependent halo bias correction that can reach order-one amplitude for rare high-redshift halos at z=7.
A calibrated fitting function for the halo mass function that unifies predictions across CDM and non-CDM models over 10 orders of magnitude in mass with typical 12% precision after modeling systematics.
Optimal transport reconstruction of initial conditions from biased tracers in local PNG fields improves when a realistic model for the scale-dependent clustering of the unobserved dust is included.
A lunar array needs at least ~30,000 Fourier modes and distributed stations to reach σ(α_s)=0.034 on inflation, competitive with Planck, though thermal noise limits high-redshift small-scale access.
Quiescent galaxies cluster more strongly than star-forming ones by 0.5-1 dex after halo-mass matching, with one-halo conformity up to z~2 that disappears at higher redshifts.
Fixing the covariance at an incorrect cosmology in cluster count analyses leaves Ω_c, σ_8, and w estimates unbiased but distorts their uncertainties, driven by S_8 amplitude effects; a single update at the recovered best-fit cosmology restores correct normalization for LSST-like surveys.
New hydrodynamical simulations show that dwarf galaxy stellar mass-halo mass relations and star formation histories are more influenced by host halo concentration than by the 5 cMpc scale environment.
Low-mass filament galaxies in TNG50 exhibit smaller asymmetric cold gas discs due to cosmic web tidal fields causing altered accretion or starvation and late-time stripping, while integrated stellar and halo properties remain similar to field counterparts after mass and environment controls.
First measurement of angular clustering w(theta) for radio sources at 816 MHz over 800 deg2 yields positive signal and effective bias 1.53-2.0 depending on N(z) prior.
An updated linear halo bias fit calibrated on high-redshift simulations reduces systematic offsets in early-universe clustering predictions to under 1%.
Lecture series on the physics, phenomenology, and statistics of large-scale cosmic structure evolution and non-Gaussian predictions.
citing papers explorer
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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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Tracing Primordial Gravitational Waves via non-Gaussian Signatures of Halo Bias
Tensor-induced non-Gaussianity from primordial gravitational waves generates a unique scale-dependent halo bias correction that can reach order-one amplitude for rare high-redshift halos at z=7.
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A Unified Halo Mass Function Across Dark Matter Models from High-Resolution Multi-Scale Simulations
A calibrated fitting function for the halo mass function that unifies predictions across CDM and non-CDM models over 10 orders of magnitude in mass with typical 12% precision after modeling systematics.
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Optimal Transport Reconstruction of Biased Tracers in Primordial Non-Gaussian Fields
Optimal transport reconstruction of initial conditions from biased tracers in local PNG fields improves when a realistic model for the scale-dependent clustering of the unobserved dust is included.
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A Designer's Guide to Lunar Far-Side Interferometer Array: Power Spectrum Measurement and Cosmological Constraints from the Dark Ages
A lunar array needs at least ~30,000 Fourier modes and distributed stations to reach σ(α_s)=0.034 on inflation, competitive with Planck, though thermal noise limits high-redshift small-scale access.
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Cosmology-dependent covariance in galaxy cluster number counts: consequences for parameter inference
Fixing the covariance at an incorrect cosmology in cluster count analyses leaves Ω_c, σ_8, and w estimates unbiased but distorts their uncertainties, driven by S_8 amplitude effects; a single update at the recovered best-fit cosmology restores correct normalization for LSST-like surveys.
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Tracing Large-scale Structure with the MeerKLASS On-the-Fly Survey: Angular Clustering of Radio Sources at 816 MHz
First measurement of angular clustering w(theta) for radio sources at 816 MHz over 800 deg2 yields positive signal and effective bias 1.53-2.0 depending on N(z) prior.
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An Improved Fit for Linear Halo Bias at High Redshift
An updated linear halo bias fit calibrated on high-redshift simulations reduces systematic offsets in early-universe clustering predictions to under 1%.
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Large-scale structures of the Universe: physics, phenomenology, statistics
Lecture series on the physics, phenomenology, and statistics of large-scale cosmic structure evolution and non-Gaussian predictions.