暗物质晕质量函数(Mass function of dark matter halo) 坦特里斯 渔夫 科学求真 赢10 万奖金 · 院士面对面 22 人赞同了该文章 暗物质晕分布的统计性质,即特定红移 z 与质量 M 的暗物质晕的数密度分布 n=n(M,z) ,能够告诉我们结构形成的重要信息。
DARK matterGALACTIC halosRANDOM walksGRAVITATIONAL potentialRHEOLOGYDENSITYHalo abundance and structure play a central role for modeling structure formation and evolution. Without relying on a spherical or ellipsoidal collapse model, we analytically derive the halo mass function and cuspy halo density (inner...
we analytically derive the halo mass function and cuspy halo density (inner slope of −4/3) based on the mass and energy cascade theory in dark matter flow. The hierarchical halo structure formation leads to halo or particle
We show that for a range of CDM cosmologies and for a suitable halo definition, the simulated mass function is almost independent of epoch, of cosmological parameters and of the initial power spectrum when expressed in appropriate variables. This universality is of exactly the kind predicted by ...
We determine the mass function in the concordance Lambda CDM cosmology, as well as its uncertainty, using sixteen 1024(3) particle nested-volume dark matter simulations spanning a mass range of over 5 orders of magnitude. Using the nested volumes and single-halo tests, we find and correct for...
6 The mean luminosity density produced by dark matter annihilation in today’s Universe as a function of halo mass. Solid coloured lines indicate estimates obtained by multiplying the mean \(\langle L/M\rangle \) obtained from well resolved, simulated haloes by the halo number density predicted...
We find a dark matter halo in remarkably good agreement with simulations (log_10 M_200/M_sun = 14.2 +/- 0.2, c_200 = 4.4 (+1.6, -1.4)) and a stellar mass-to-light ratio which favors a Salpeter initial mass function ((M/L)* = 5.7 +/- 1.2). Our measurement of a normal ...
If these models are correct, clustering variations between galaxies of differing morphological types, luminosities, colours and surface brightnesses, must all arise because the halo mass function is skewed towards high mass objects in overdense regions of the Universe and towards low mass objects in ...
Simulating the complexity of the dark matter sheet – II. Halo and subhalo mass functions for non-cold dark matter models We present 'sheet + release' simulations that reliably follow the evolution of dark matter structure at and below the dark matter free-streaming scale, whe... S Jens,RE...
dark mattergalaxies: clusters: generalgalaxies: halosIn the standard excursion-set model for the growth of structure, the statistical properties of halos are governed by the halo mass and are independent of the larger-scale environment in which the halos reside. Numerical simulations, however, have...