A fully Lagrangian, non-parametric bias model for dark matter halos
Abstract
We present a non-parametric Lagrangian biasing model and fit the ratio of the halo and mass densities at the field level using the mass-weighted halo field in the AbacusSummit simulations at z=0.5. Unlike the perturbative halo bias model that has been widely used in interpreting the observed large-scale structure traced by galaxies, we find a non-negative halo-to-mass ratio that increases monotonically with the linear overdensity δ1 in the initial Lagrangian space. The bias expansion, however, does not guarantee non-negativity of the halo counts, and may lead to rising halo number counts at negative overdensities. The shape of the halo-to-mass ratio is unlikely to be described by a polynomial function of δ1 and other quantities. Especially for massive halos with 6×1012h-1 M⊙, the halo-to-mass ratio starts soaring up at δ1>0, substantially different from the predictions of the bias expansion. We show that for the halo masses we consider (M>3×1011 h-1 M⊙) a non-parametric halo-to-mass ratio as a function of δ1 and its local derivative ∇^2δ1 can recover the halo power spectra to sub-percent level accuracy for wavenumbers k=0.01-0.1 h Mpc-1 given a proper smoothing scale to filter the initial density field, even though we do not fit the power spectrum directly.more »
- Authors:
-
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
- Publication Date:
- Research Org.:
- Harvard Univ., Cambridge, MA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC); National Aeronautics and Space Administration (NASA); Smithsonian Astrophysical Observatory; Simons Foundation
- OSTI Identifier:
- 1979353
- Grant/Contract Number:
- SC0013718; 12-EUCLID12-0004; NAS5-02015
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Journal of Cosmology and Astroparticle Physics
- Additional Journal Information:
- Journal Volume: 2022; Journal Issue: 02; Journal ID: ISSN 1475-7516
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS
Citation Formats
Wu, Xiaohan, Muñoz, Julian B., and Eisenstein, Daniel. A fully Lagrangian, non-parametric bias model for dark matter halos. United States: N. p., 2022.
Web. doi:10.1088/1475-7516/2022/02/002.
Wu, Xiaohan, Muñoz, Julian B., & Eisenstein, Daniel. A fully Lagrangian, non-parametric bias model for dark matter halos. United States. https://doi.org/10.1088/1475-7516/2022/02/002
Wu, Xiaohan, Muñoz, Julian B., and Eisenstein, Daniel. Wed .
"A fully Lagrangian, non-parametric bias model for dark matter halos". United States. https://doi.org/10.1088/1475-7516/2022/02/002. https://www.osti.gov/servlets/purl/1979353.
@article{osti_1979353,
title = {A fully Lagrangian, non-parametric bias model for dark matter halos},
author = {Wu, Xiaohan and Muñoz, Julian B. and Eisenstein, Daniel},
abstractNote = {We present a non-parametric Lagrangian biasing model and fit the ratio of the halo and mass densities at the field level using the mass-weighted halo field in the AbacusSummit simulations at z=0.5. Unlike the perturbative halo bias model that has been widely used in interpreting the observed large-scale structure traced by galaxies, we find a non-negative halo-to-mass ratio that increases monotonically with the linear overdensity δ1 in the initial Lagrangian space. The bias expansion, however, does not guarantee non-negativity of the halo counts, and may lead to rising halo number counts at negative overdensities. The shape of the halo-to-mass ratio is unlikely to be described by a polynomial function of δ1 and other quantities. Especially for massive halos with 6×1012h-1 M⊙, the halo-to-mass ratio starts soaring up at δ1>0, substantially different from the predictions of the bias expansion. We show that for the halo masses we consider (M>3×1011 h-1 M⊙) a non-parametric halo-to-mass ratio as a function of δ1 and its local derivative ∇^2δ1 can recover the halo power spectra to sub-percent level accuracy for wavenumbers k=0.01-0.1 h Mpc-1 given a proper smoothing scale to filter the initial density field, even though we do not fit the power spectrum directly. However, there is mild dependence of the recovery of the halo power spectrum on the smoothing scale and other input parameters. At k<0.01 h Mpc-1 and for massive halos with M>6x1012 h-1M⊙, our non-parametric model leads to a few percent overestimation of the halo power spectrum, indicating the need for larger or multiple smoothing scales. The halo-to-mass ratios obtained qualitatively agree with intuitions from extended Press-Schechter theory. We compare our framework to the bias expansion and discuss possible extensions.},
doi = {10.1088/1475-7516/2022/02/002},
journal = {Journal of Cosmology and Astroparticle Physics},
number = 02,
volume = 2022,
place = {United States},
year = {Wed Feb 02 00:00:00 EST 2022},
month = {Wed Feb 02 00:00:00 EST 2022}
}
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