DARK MATTER HALOS IN THE STANDARD COSMOLOGICAL MODEL: RESULTS FROM THE BOLSHOI SIMULATION

By Anatoly Klypin, Sebastian Trujillo-Gomez, Joel R. Primack. 2010

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Lambda Cold Dark Matter (ΛCDM) is now the standard theory of structure formation in the universe. We present the first results from the new Bolshoi dissipationless cosmological ΛCDM simulation that uses cosmological parameters favored by current observations. The Bolshoi simulation was run in a volume 250 h−1 Mpc on a side using ∼8 billion particles with mass and force resolution adequate to follow subhalos down to the completeness limit of Vcirc = 50 km s−1 maximum circular velocity. Using merger trees derived from analysis of 180 stored time steps we find the circular velocities of satellites before they fall into their host halos. Using excellent statistics of halos and subhalos (∼10 million at every moment and ∼50 million over the whole history) we present accurate approximations for statistics such as the halo mass function, the concentrations for distinct halos and subhalos, the abundance of halos as a function of their circular velocity, and the abundance and the spatial distribution of subhalos. We find that at high redshifts the concentration falls to a minimum value of about 4.0 and then rises for higher values of halo mass—a new result. We present approximations for the velocity and mass functions of distinct halos as a function of redshift. We find that while the Sheth–Tormen (ST) approximation for the mass function of halos found by spherical overdensity is quite accurate at low redshifts, the ST formula overpredicts the abundance of halos by nearly an order of magnitude by z = 10. We find that the number of subhalos scales with the circular velocity of the host halo as V1/2host, and that subhalos have nearly the same radial distribution as dark matter particles at radii 0.3–2 times the host halo virial radius. The subhalo velocity function N(> Vsub) scales as V−3circ. Combining the results of Bolshoi and Via Lactea-II simulations, we find that inside the virial radius of halos with the number of satellites is N(> Vsub) = (Vsub/58 km s−1)−3 for satellite circular velocities in the range 4 km s−1 < Vsub < 150 km s−1.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/5d84cdb63e6867deeb101e58ecf1b1e701b569a4

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Citations in the corpus

Sensitivity projections for dark matter searches with the Fermi large area telescope (2016, background): “, provide a statistically-complete sample of DM halos down to a maximum circular velocity of about 50 km/s, or a mass of approximately 10(9) M [219, 220].”
Hunting for the Dark Matter Wake Induced by the Large Magellanic Cloud (2019, background): “The halo spin parameter λ = 0.027 and concentration are consistent with typical MW-like DM halos in cosmological simulations (Klypin et al. 2011).”
The chosen few: the low-mass haloes that host faint galaxies (2014, background): “While the total population follows the vmax – mass relations expected for ΛCDM (e.g. Klypin et al. 2011, not shown), we find that below 109.5M , luminous halos have significantly higher vmax – mass ratios than non-luminous ones.”
Galaxies as simple dynamical systems: observational data disfavor dark matter and stochastic star formation (2014, background): “galaxies such as the Milky Way (MW) and Andromeda ought to have thousands of dark-matter sub-halos orbiting within the dark matter halo which surrounds them with a radius of about 250 kpc as documented by a number of seminal contributions [81–84].”
Galactic Searches for Dark Matter (2012, background): “The two largest volume cosmological simulations to date that resolve a statistical sample of Milky Way-mass halos identify approximately 104 halos with mass near 1012 M (Boylan-Kolchin et al., 2009; Klypin et al., 2011).”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, positive): “We have extracted merger trees from the new Bolshoi N-body simulation (Klypin et al. 2010), which also track the evolution of sub-halos.”
Bent by baryons: the low-mass galaxy-halo relation (2014, methodology): “For consistency with the observations, the halo masses at z = 0 of individual objects in the simulation are derived using the measured maximum circular velocity converted to mass following Klypin et al. (2011).”
Numerical simulations of the dark universe: State of the art and the next decade (2012, background): “4 [262] †For AMR simulations (Ramses, Art) soft refers to the highest resolution cell width.”
THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, methodology): “Given halos from a dark matter simulation, each point in the SM(Mh, z) function parameter space represents an assignment of galaxy stellar masses to every halo at every redshift; the simulation and halo catalogs used by BWC13 are detailed by Klypin et al. (2011) and Behroozi et al. (2013c,d).”
MultiDark simulations: the story of dark matter halo concentrations and density profiles (2014, methodology): “…on mass, redshift, and cosmological parameters – has been the subject of extensive analysis for a long period of time (Navarro et al. 1997; Jing 2000; Bullock et al. 2001; Neto et al. 2007; Gao et al. 2008; Macciò et al. 2008; Klypin et al. 2011; Prada et al. 2012; Dutton & Macciò 2014).”