Scale-dependent bias in the baryonic-acoustic-oscillation-scale intergalactic neutral hydrogen

Pontzen, Andrew

doi:10.1103/physrevd.89.083010

Cited by 69 publications

(82 citation statements)

References 69 publications

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“…Abel & Haehnelt 1999;Pontzen 2014;Gontcho A Gontcho et al 2014;Davies & Furlanetto 2014;Malloy & Lidz 2015;D'Aloisio et al 2015;. Of course, an immediate solution to this problem in optically thin simulations will be to add some extra dependence on a specific property of each resolution element in the simulation (e.g.…”

Section: Discussionmentioning

confidence: 99%

Self-consistent Modeling of Reionization in Cosmological Hydrodynamical Simulations

Oñorbe

Hennawi

Lukić

2017

ApJ

125

191

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The ultraviolet background (UVB) emitted by quasars and galaxies governs the ionization and thermal state of the intergalactic medium (IGM), regulates the formation of high-redshift galaxies, and is thus a key quantity for modeling cosmic reionization. The vast majority of cosmological hydrodynamical simulations implement the UVB via a set of spatially uniform photoionization and photoheating rates derived from UVB synthesis models. We show that simulations using canonical UVB rates reionize and, perhaps more importantly, spuriously heat the IGM, much earlier z ∼ 15 than they should. This problem arises because at z > 6, where observational constraints are nonexistent, the UVB amplitude is far too high. We introduce a new methodology to remedy this issue, and we generate selfconsistent photoionization and photoheating rates to model any chosen reionization history. Following this approach, we run a suite of hydrodynamical simulations of different reionization scenarios and explore the impact of the timing of reionization and its concomitant heat injection on the the thermal state of the IGM. We present a comprehensive study of the pressure smoothing scale of IGM gas, illustrating its dependence on the details of both hydrogen and helium reionization, and argue that it plays a fundamental role in interpreting Lyman-α forest statistics and the thermal evolution of the IGM. The premature IGM heating we have uncovered implies that previous work has likely dramatically overestimated the impact of photoionization feedback on galaxy formation, which sets the minimum halo mass able to form stars at high redshifts. We make our new UVB photoionization and photoheating rates publicly available for use in future simulations.

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Section: Discussionmentioning

confidence: 99%

Self-consistent Modeling of Reionization in Cosmological Hydrodynamical Simulations

Oñorbe

Hennawi

Lukić

2017

ApJ

125

191

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“…If the scale R * is larger than the spatial length scale (nonlinear scale) controlling the perturbative expansion, then one can correspondingly include higher-order derivative terms. This might be the case for very massive halos [66][67][68], for example, or due to radiative-transfer effects [69][70][71][72][73][74].…”

Section: Higher Derivativesmentioning

confidence: 99%

An EFT description of galaxy intrinsic alignments

Vlah

Chisari

Schmidt

2020

J. Cosmol. Astropart. Phys.

146

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We present a general perturbative effective field theory (EFT) description of galaxy shape correlations, which are commonly known as intrinsic alignments. This rigorous approach extends current analytical modelling strategies in that it only relies on the equivalence principle. We present our results in terms of three-dimensional statistics for two-and three-point functions of both galaxy shapes and number counts. In case of the two-point function, we recover the well-known linear alignment result at leading order, but also present the full next-to-leading order expressions. In case of the three-point function we present leading order results for all the auto-and cross-correlations of galaxy shapes and densities. We use a spherical tensor basis to decompose the tensor perturbations in different helicity modes, which allows us to make use of isotropy and parity properties in the correlators. Combined with the results on projection presented in a forthcoming companion paper, our framework is directly applicable to accounting for intrinsic alignment contamination in weak lensing surveys, and to extracting cosmological information from intrinsic alignments. 42A.1 Two-point functions 44 A.2 Three-point functions 47 B Fields in Fourier space 50 B.1 Bias expansion and renormalisation of the one-loop power spectrum 55 B.2 Degeneracy of the bias operators 62 B.3 Bias expansion of the tree-level bispectrum 63 C Bias renormalisation for tensor fields 65 1 Explicitly, we writewhere the Dirac delta function ensures the total momentum conservation, and is a consequence of the statistical translation invariance.

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“…It is important to highlight that in fact what gets computed from this procedure is the dimensionless power spectrum ∆ m,x HI and hence ∆ m,ψ . We have not included fluctuations in the low-redshift ionizing background, which will also change the flux power spectrum and have been calculated elsewhere (Pontzen 2014;Gontcho A Gontcho et al 2014). To lowest order, the ionizing background effects should be added to the inhomogeneous reionization effects.…”

Section: Conventions and Formalismmentioning

confidence: 99%

Impact of inhomogeneous reionization on the Lyman-α forest

Montero-Camacho

Hirata

Martini

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The Lyman-α forest at high redshifts is a powerful probe of reionization. Modeling and observing this imprint comes with significant technical challenges: inhomogeneous reionization must be taken into account while simultaneously being able to resolve the web-like small-scale structure prior to reionization. In this work we quantify the impact of inhomogeneous reionization on the Lyman-α forest at lower redshifts (2 < z < 4), where upcoming surveys such as DESI will enable precision measurements of the flux power spectrum. We use both small box simulations capable of handling the small-scale structure of the Lyman-α forest and semi-numerical large box simulations capable of representing the effects of inhomogeneous reionization. We find that inhomogeneous reionization could produce a measurable effect on the Lyman-α forest power spectrum. The deviation in the 3D power spectrum at z obs = 4 and k = 0.14 Mpc −1 ranges from 19 -36%, with a larger effect for later reionization. The corrections decrease to 2.0 -4.1% by z obs = 2. The impact on the 1D power spectrum is smaller, and ranges from 3.3 -6.5% at z obs = 4 to 0.35 -0.75% at z obs = 2, values which are comparable to the statistical uncertainties in current and upcoming surveys. Furthermore, we study how can this systematic be constrained with the help of the quadrupole of the 21 cm power spectrum.1 More precisely, the optical depth is proportional to the neutral hydrogen density, which in turn depends on the density and temperature of the gas and the photoionization rate. This is then smeared by the Doppler width of the Lyman-α line.

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Scale-dependent bias in the baryonic-acoustic-oscillation-scale intergalactic neutral hydrogen

Cited by 69 publications

References 69 publications

Self-consistent Modeling of Reionization in Cosmological Hydrodynamical Simulations

Self-consistent Modeling of Reionization in Cosmological Hydrodynamical Simulations

An EFT description of galaxy intrinsic alignments

Impact of inhomogeneous reionization on the Lyman-α forest

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