scholarly journals Small-scale structure of primordial black hole dark matter and its implications for accretion

2019 ◽  
Vol 100 (8) ◽  
Author(s):  
Gert Hütsi ◽  
Martti Raidal ◽  
Hardi Veermäe
Keyword(s):  
Black Hole ◽  
Dark Matter ◽  
Scale Structure ◽  
Small Scale ◽  
Primordial Black Hole ◽  
Small Scale Structure

scholarly journals Finite-Size Dark Matter and its Effect on Small-Scale Structure

2020 ◽  
Vol 124 (4) ◽  
Author(s):  
Xiaoyong Chu ◽  
Camilo Garcia-Cely ◽  
Hitoshi Murayama
Keyword(s):  
Dark Matter ◽  
Finite Size ◽  
Scale Structure ◽  
Small Scale ◽  
Small Scale Structure

scholarly journals Dark matter from late decays and the small-scale structure problems

2008 ◽  
Vol 77 (6) ◽  
Author(s):  
Francesca Borzumati ◽  
Torsten Bringmann ◽  
Piero Ullio
Keyword(s):  
Dark Matter ◽  
Scale Structure ◽  
Small Scale ◽  
Small Scale Structure

scholarly journals Small-scale structure of dark matter and microlensing

1997 ◽  
Vol 167 (9) ◽  
pp. 913 ◽  
Author(s):  
Aleksandr V. Gurevich ◽  
Kirill P. Zybin ◽  
V.A. Sirota
Keyword(s):  
Dark Matter ◽  
Scale Structure ◽  
Small Scale ◽  
Small Scale Structure

scholarly journals Quantifying the power spectrum of small-scale structure in semi-analytic galaxies

2019 ◽  
Vol 488 (4) ◽  
pp. 5085-5092 ◽  
Author(s):  
Sean Brennan ◽  
Andrew J Benson ◽  
Francis-Yan Cyr-Racine ◽  
Charles R Keeton ◽  
Leonidas A Moustakas ◽  
...  
Keyword(s):  
Dark Matter ◽  
Power Spectrum ◽  
Gravitational Lensing ◽  
Cold Dark Matter ◽  
Scale Structure ◽  
Small Scale ◽  
Small Scale Structure ◽  
Mass Distributions ◽  
Theoretical Predictions ◽  
Spectrum Distribution

Abstract In the cold dark matter (CDM) picture of structure formation, galaxy mass distributions are predicted to have a considerable amount of structure on small scales. Strong gravitational lensing has proven to be a useful tool for studying this small-scale structure. Much of the attention has been given to detecting individual dark matter subhaloes through lens modelling, but recent work has suggested that the full population of subhaloes could be probed using a power spectrum analysis. In this paper, we quantify the power spectrum of small-scale structure in simulated galaxies, with the goal of understanding theoretical predictions and setting the stage for using measurements of the power spectrum to test dark matter models. We use a sample of simulated galaxies generated from the galacticus semi-analytic model to determine the power spectrum distribution first in the CDM paradigm and then in a warm dark matter scenario. We find that a measurement of the slope and amplitude of the power spectrum on galaxy strong lensing scales (k ∼ 1 kpc−1) could be used to distinguish between CDM and alternate dark matter models, especially if the most massive subhaloes can be directly detected via gravitational imaging.

scholarly journals Seeking Observable Imprints of Small-Scale Structure on the Properties of Dark Matter Haloes

2013 ◽  
Vol 30 ◽  
Author(s):  
C. Power
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Spatial Clustering ◽  
Scale Structure ◽  
Small Scale ◽  
Halo Formation ◽  
Potential Wells ◽  
Massive Galaxies ◽  
Small Scale Structure ◽  
Low Mass

AbstractThe characteristic prediction of the Cold Dark Matter (CDM) model of cosmological structure formation is that the Universe should contain a wealth of small-scale structure—low-mass dark matter haloes and subhaloes. However, galaxy formation is inefficient in their shallow potential wells and so we expect these low-mass haloes and subhaloes to be dark. Can we tell the difference between a Universe in which these low-mass haloes are present but dark and one in which they never formed, thereby providing a robust test of the CDM model? We address this question using cosmological N-body simulations to examine how properties of low-mass haloes that are potentially accessible to observation, such as their spatial clustering, rate of accretions and mergers onto massive galaxies, and the angular momentum content of massive galaxies, differ between a fiducial ΛCDM model and dark matter models in which low-mass halo formation is suppressed. Adopting an effective cut-off mass scale Mcut below which small-scale power is suppressed in the initial conditions, we study dark matter models in which Mcut varies between 5×109h−1M⊙ and 1011h−1M⊙, equivalent to the host haloes of dwarf and low-mass galaxies. Our results show that both the clustering strength of low-mass haloes around galaxy-mass primaries and the rate at which they merge with these primaries are sensitive to the assumed value of Mcut; in contrast, suppressing low-mass halo formation has little influence on the angular momentum content of galaxy-mass haloes—it is the quiescence or violence of a halo's assembly history that has a more marked effect. However, we expect that measuring the effect on spatial clustering or the merger rate is likely to be observationally difficult for realistic values of Mcut, and so isolating the effect of this small-scale structure would appear to be remarkably difficult to detect, at least in the present day Universe.

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