Halo Zel’dovich model and perturbation theory: Dark matter power spectrum and correlation function

Abstract Some beyond ΛCDM cosmological models have dark-sector energy densities that suffer phase transitions. Fluctuations entering the horizon during such a transition can receive enhancements that ultimately show up as a distinctive bump in the power spectrum relative to a model with no phase transition. In this work, we study the non-linear evolution of such signatures in the matter power spectrum and correlation function using N-body simulations, perturbation theory and hmcode- a halo-model based method. We focus on modelling the response, computed as the ratio of statistics between a model containing a bump and one without it, rather than in the statistics themselves. Instead of working with a specific theoretical model, we inject a parametric family of Gaussian bumps into otherwise standard ΛCDM spectra. We find that even when the primordial bump is located at linear scales, non-linearities tend to produce a second bump at smaller scales. This effect is understood within the halo model due to a more efficient halo formation. In redshift space these nonlinear signatures are partially erased because of the damping along the line-of-sight direction produced by non-coherent motions of particles at small scales. In configuration space, the bump modulates the correlation function reflecting as oscillations in the response, as it is clear in linear Eulerian theory; however, they become damped because large scale coherent flows have some tendency to occupy regions more depleted of particles. This mechanism is explained within Lagrangian Perturbation Theory and well captured by our simulations.

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Statistical modelling of the cosmological dispersion measure

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab170 ◽

2021 ◽

Vol 502 (2) ◽

pp. 2615-2629

Author(s):

Ryuichi Takahashi ◽

Kunihito Ioka ◽

Asuka Mori ◽

Koki Funahashi

Keyword(s):

Dark Matter ◽

Correlation Function ◽

Probability Distribution ◽

Power Spectrum ◽

Free Electron ◽

Statistical Modelling ◽

Dispersion Measure ◽

Host Galaxies ◽

Angular Power Spectrum ◽

Bias Factor

ABSTRACT We have investigated the basic statistics of the cosmological dispersion measure (DM)—such as its mean, variance, probability distribution, angular power spectrum, and correlation function—using the state-of-the-art hydrodynamic simulations, IllustrisTNG300, for the fast radio burst cosmology. To model the DM statistics, we first measured the free-electron abundance and the power spectrum of its spatial fluctuations. The free-electron power spectrum turns out to be consistent with the dark matter power spectrum at large scales, but it is strongly damped at small scales (≲ Mpc) owing to the stellar and active galactic nucleus feedback. The free-electron power spectrum is well modelled using a scale-dependent bias factor (the ratio of its fluctuation amplitude to that of the dark matter). We provide analytical fitting functions for the free-electron abundance and its bias factor. We next constructed mock sky maps of the DM by performing standard ray-tracing simulations with the TNG300 data. The DM statistics are calculated analytically from the fitting functions of the free-electron distribution, which agree well with the simulation results measured from the mock maps. We have also obtained the probability distribution of source redshift for a given DM, which helps in identifying the host galaxies of FRBs from the measured DMs. The angular two-point correlation function of the DM is described by a simple power law, $\xi (\theta) \approx 2400 (\theta /{\rm deg})^{-1} \, {\rm pc}^2 \, {\rm cm}^{-6}$, which we anticipate will be confirmed by future observations when thousands of FRBs are available.

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Matter power spectrum of light freeze-in dark matter: With or without self-interaction

Physics Letters B ◽

10.1016/j.physletb.2020.135251 ◽

2020 ◽

Vol 802 ◽

pp. 135251

Author(s):

Ran Huo

Keyword(s):

Dark Matter ◽

Power Spectrum ◽

Matter Power Spectrum

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ETHOS – an effective theory of structure formation: formation of the first haloes and their stars

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz766 ◽

2019 ◽

Vol 485 (4) ◽

pp. 5474-5489 ◽

Cited By ~ 6

Author(s):

Mark R Lovell ◽

Jesús Zavala ◽

Mark Vogelsberger

Keyword(s):

Dark Matter ◽

Power Spectrum ◽

Galaxy Formation ◽

Cold Dark Matter ◽

Dwarf Galaxy ◽

Mass Scale ◽

Effective Theory ◽

Matter Power Spectrum ◽

Hydrodynamical Simulations ◽

Stellar Masses

Abstract A cut-off in the linear matter power spectrum at dwarf galaxy scales has been shown to affect the abundance, formation mechanism and age of dwarf haloes, and their galaxies at high and low redshifts. We use hydrodynamical simulations of galaxy formation within the ETHOS framework in a benchmark model that has such a cut-off and that has been shown to be an alternative to the cold dark matter (CDM) model that alleviates its dwarf-scale challenges. We show how galaxies in this model form differently to CDM, on a halo-by-halo basis, at redshifts z ≥ 6. We show that when CDM haloes with masses around the ETHOS half-mode mass scale are resimulated with the ETHOS matter power spectrum, they form with 50 per cent less mass than their CDM counterparts due to their later formation times, yet they retain more of their gas reservoir due to the different behaviour of gas and dark matter during the monolithic collapse of the first haloes in models with a galactic-scale cut-off. As a result, galaxies in ETHOS haloes near the cut-off scale grow rapidly between z = 10 and 6 and by z = 6 end up having very similar stellar masses, higher gas fractions and higher star formation rates relative to their CDM counterparts. We highlight these differences by making predictions for how the number of galaxies with old stellar populations is suppressed in ETHOS for both z = 6 galaxies and for gas-poor Local Group fossil galaxies. Interestingly, we find an age gradient in ETHOS between galaxies that form in high- and low-density environments.

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Information content in the halo-model dark-matter power spectrum -- II. Multiple cosmological parameters

Monthly Notices of the Royal Astronomical Society Letters ◽

10.1111/j.1745-3933.2006.00275.x ◽

2007 ◽

Vol 375 (1) ◽

pp. L51-L55 ◽

Cited By ~ 36

Author(s):

M. C. Neyrinck ◽

I. Szapudi

Keyword(s):

Dark Matter ◽

Power Spectrum ◽

Information Content ◽

Cosmological Parameters ◽

Matter Power Spectrum

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Intensity mapping as a probe of axion dark matter

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3300 ◽

2020 ◽

Vol 500 (3) ◽

pp. 3162-3177

Author(s):

Jurek B Bauer ◽

David J E Marsh ◽

Renée Hložek ◽

Hamsa Padmanabhan ◽

Alex Laguë

Keyword(s):

Dark Matter ◽

Power Spectrum ◽

Neutral Hydrogen ◽

Matrix Formalism ◽

Intensity Mapping ◽

Matter Power Spectrum ◽

Wide Range ◽

Non Linear ◽

Order Of Magnitude ◽

Magnitude Improvement

ABSTRACT We consider intensity mapping (IM) of neutral hydrogen (H i) in the redshift range 0 ≲ z ≲ 3 employing a halo model approach where H i is assumed to follow the distribution of dark matter (DM) haloes. If a portion of the DM is composed of ultralight axions, then the abundance of haloes is changed compared to cold DM below the axion Jeans mass. With fixed total H i density, $\Omega _{\rm H\, \rm {\small I}}$, assumed to reside entirely in haloes, this effect introduces a scale-independent increase in the H i power spectrum on scales above the axion Jeans scale, which our model predicts consistent with N-body simulations. Lighter axions introduce a scale-dependent feature even on linear scales due to its suppression of the matter power spectrum near the Jeans scale. We use the Fisher matrix formalism to forecast the ability of future H i surveys to constrain the axion fraction of DM and marginalize over astrophysical and model uncertainties. We find that a HIRAX-like survey is a very reliable IM survey configuration, being affected minimally by uncertainties due to non-linear scales, while the SKA1MID configuration is the most constraining as it is sensitive to non-linear scales. Including non-linear scales and combining a SKA1MID-like IM survey with the Simons Observatory CMB, the benchmark ‘fuzzy DM’ model with ma = 10−22 eV can be constrained at few per cent. This is almost an order of magnitude improvement over current limits from the Ly α forest. For lighter ULAs, this limit improves below 1 per cent, and allows the possibility to test the connection between axion models and the grand unification scale across a wide range of masses.

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The halo mass function in alternative dark matter models

Monthly Notices of the Royal Astronomical Society Letters ◽

10.1093/mnrasl/slaa005 ◽

2020 ◽

Vol 493 (1) ◽

pp. L11-L15 ◽

Cited By ~ 4

Author(s):

M R Lovell

Keyword(s):

Dark Matter ◽

Power Spectrum ◽

Particle Physics ◽

Mass Function ◽

Small Scale ◽

Acoustic Oscillations ◽

Sterile Neutrinos ◽

Matter Power Spectrum ◽

Alternative Approach ◽

Good Agreement

ABSTRACT The claimed detection of large amounts of substructure in lensing flux anomalies, and in Milky Way stellar stream gap statistics, has led to a step change in constraints on simple warm dark matter models. In this study, we compute predictions for the halo mass function both for these simple models and for comprehensive particle physics models of sterile neutrinos and dark acoustic oscillations. We show that the mass function fit of Lovell et al. underestimates the number of haloes less massive than the half-mode mass, $M_\mathrm {hm}$, by a factor of 2, relative to the extended Press–Schechter (EPS) method. The alternative approach of applying EPS to the Viel et al. matter power spectrum fit instead suggests good agreement at $M_\mathrm {hm}$ relative to the comprehensive model matter power spectrum results, although the number of haloes with mass $\rm{\lt} M_\mathrm {hm}$ is still suppressed due to the absence of small-scale power in the fitting function. Overall, we find that the number of dark matter haloes with masses $\rm{\lt} 10^{8}{\, \rm M_\odot }$ predicted by competitive particle physics models is underestimated by a factor of ∼2 when applying popular fitting functions, although careful studies that follow the stripping and destruction of subhaloes will be required in order to draw robust conclusions.

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