Universal structure of dark matter haloes over a mass range of 20 orders of magnitude

Wang, J.; Bose, Sownak; Frenk, Carlos S.; Gao, Liang; Jenkins, Adrian; Springel, Volker; White, Simon D. M.

doi:10.1038/s41586-020-2642-9

Cited by 245 publications

(215 citation statements)

References 41 publications

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“…(3.10) against N -body simulations. For ΛCDM halos (for which z col 10) we use the results in [35] and find C ρ ∼ 600, for axion miniclusters (for which z col 10 3 ) we use the results of [34] and find C ρ ∼ 9 × 10 4 . In the following we use a z col -dependent C ρ which smoothly interpolates between these two values.…”

Section: Jhep06(2021)028mentioning

confidence: 99%

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Probing small-scale power spectra with pulsar timing arrays

Lee

Mitridate

Trickle

et al. 2021

J. High Energ. Phys.

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Models of Dark Matter (DM) can leave unique imprints on the Universe’s small scale structure by boosting density perturbations on small scales. We study the capability of Pulsar Timing Arrays to search for, and constrain, subhalos from such models. The models of DM we consider are ordinary adiabatic perturbations in ΛCDM, QCD axion miniclusters, models with early matter domination, and vector DM produced during inflation. We show that ΛCDM, largely due to tidal stripping effects in the Milky Way, is out of reach for PTAs. Axion miniclusters may be within reach, although this depends crucially on whether the axion relic density is dominated by the misalignment or string contribution. Models where there is matter domination with a reheat temperature below 1 GeV may be observed with future PTAs. Lastly, vector DM produced during inflation can be detected if it is lighter than 10−16 GeV. We also make publicly available a Python Monte Carlo tool for generating the PTA time delay signal from any model of DM substructure.

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Section: Jhep06(2021)028mentioning

confidence: 99%

“…where Ω m and Ω Λ are the matter and vacuum energy densities, normalized to the critical density, ρ c , respectively. The sHMF for standard CDM halos has been computed in the mass range (10 −5 − 10 12 )M [35] but little is known for lighter subhalos. Because of this, we compute the sHMF at infall by using eq.…”

Section: Jhep06(2021)028mentioning

confidence: 99%

Probing small-scale power spectra with pulsar timing arrays

Lee

Mitridate

Trickle

et al. 2021

J. High Energ. Phys.

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“…Throughout this paper we will use the S 8 octree basis functions developed by Jenkins (2013). The S 8 function set have been used in making initial conditions for many cosmological simulations of the Virgo Consortium, 2 from modelling galaxy clusters (Bahé et al 2017) via galaxy groups (Sawala et al 2016) and individual galaxies (Grand et al 2017), down to simulating the smallest cold dark matter (CDM) dark haloes at the present day (Wang et al 2020).…”

Section: Octree Basismentioning

confidence: 99%

Setting the stage: structures from Gaussian random fields

Sawala

Jenkins

McAlpine

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We study structure formation in a set of cosmological simulations to uncover the scales in the initial density field that gave rise to the formation of present-day structures. Our simulations share a common primordial power spectrum (here Λ cold dark matter, ΛCDM), but the introduction of hierarchical variations of the phase information allows us to systematically study the scales that determine the formation of structure at later times. We consider the variance in z = 0 statistics such as the matter power spectrum and halo mass function. We also define a criterion for the existence of individual haloes across simulations, and determine what scales in the initial density field contain sufficient information for the non-linear formation of unique haloes. We study how the characteristics of individual haloes such as the mass and concentration, as well as the position and velocity, are affected by variations on different scales, and give scaling relations for haloes of different mass. Finally, we use the example of a cluster-mass halo to show how our hierarchical parametrization of the initial density field can be used to create variants of particular objects. With properties such as mass, concentration, kinematics, and substructure of haloes set on distinct and well-determined scales, and its unique ability to introduce variations localized in real space, our method is a powerful tool to study structure formation in cosmological simulations.

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“…The ' -cold dark matter' ( CDM) cosmological model makes specific and robust predictions for the growth, structure, and abundance of dark matter haloes, the sites where galaxies form. These are: (i) dark matter haloes grow hierarchically: small haloes form first and larger haloes form subsequently by mergers of smaller haloes and accretion of smooth dark matter; (ii) the internal structure of dark matter haloes is self-similar over ∼20 decades in mass (Navarro, Frenk & White 1996, 1997Wang et al 2020); (iii) the halo mass function rises steeply towards low masses (approximately as M −1 ; e.g. Press & Schechter 1974;Bond et al 1991;Jenkins et al 2001, and references therein), implying that a large fraction of low-mass haloes must remain 'dark' at redshift z = 0 if CDM is to be reconciled with the relatively flat faint end of the observed galaxy stellar mass function (Klypin et al 1999;Bullock, Kravtsov & Weinberg 2000;Somerville 2002;Benson et al 2002b).…”

Section: Introductionmentioning

confidence: 99%

“…Note that the concentration of low-mass CDM haloes is only weakly dependent on halo mass (see e.g Ludlow et al 2014;Wang et al 2020),. so this is a sensible assumption for our purposes.…”

mentioning

confidence: 99%

The detailed structure and the onset of galaxy formation in low-mass gaseous dark matter haloes

Benítez-Llambay

Frenk

2020

Monthly Notices of the Royal Astronomical Society

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We present a model for the formation of the first galaxies before and after the reionization of hydrogen in the early universe. In this model, galaxy formation can only take place in dark matter haloes whose mass exceeds a redshift-dependent critical value, which, before reionization, is equal (in the simplest case) to the mass at which atomic hydrogen cooling becomes effective and, after reionization, is equal to the mass above which gas cannot remain in hydrostatic equilibrium. We define the Halo Occupation Fraction (HOF) as the fraction of haloes that host a luminous galaxy as a function of halo mass. The HOF is established by the interplay between the evolution of the critical mass and the assembly history of haloes and depends on three factors: the minimum halo mass for galaxy formation before reionization, the redshift of reionization, and the intensity of the (evolving) external photoheating rate. Our fiducial model predicts a cutoff in the galaxy mass function at a present-day halo mass, M200 ∼ 3 × 108M⊙; 100% occupation at M200 > 5 × 109M⊙; and a population of starless gaseous haloes of present-day mass in the range 106 ≲ M200/M⊙ ≲ 5 × 109, in which the gas is in thermal equilibrium with the ultraviolet background radiation and in hydrostatic equilibrium in the gravitational potential of the halo. The transition between HOF = 0 and HOF = 1 reflects the stochastic nature of halo mass growth. We explore how these characteristic masses vary with model assumptions and parameter values. The results of our model are in excellent agreement with cosmological hydrodynamic simulations of galaxy formation.

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Universal structure of dark matter haloes over a mass range of 20 orders of magnitude

Cited by 245 publications

References 41 publications

Probing small-scale power spectra with pulsar timing arrays

Probing small-scale power spectra with pulsar timing arrays

Setting the stage: structures from Gaussian random fields

The detailed structure and the onset of galaxy formation in low-mass gaseous dark matter haloes

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