Without relying on a spherical or ellipsoidal collapse model, 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 random...
We revisit the derivation of the mass function and the bias of dark matter halos for non-Gaussian initial conditions. We use a steepest-descent approach to point out that exact results can be obtained for the high-mass tail of the halo mass function and the two-point correlation of massive...
Predictions from the peak model are qualitatively consistent with measurements of the linear bias of high mass haloes, which also show some evidence for a dependence on the halo mass M at fixed peak height. The peak approach also predicts a distinctive scale-dependence in the bias of haloes ...
13 Because dark matter is not made of ordinary atoms, such astronomical objects cannot be ordinary stars either. But one can still contemplate the possibility that it is some kind of exotic objects, such as black holes. Generically, one refers to MACHOs which stand for MAssive Compact Halo ...
We investigate galaxy bias in the framework of the ``Halo Occupation Distribution'' (HOD), which defines the bias of a population of galaxies by the condit... AA Berlind,DH Weinberg - 《Astrophysical Journal》 被引量: 680发表: 2002年 How do galaxies populate Dark Matter halos? For any ...
The XENON1T experiment at the Laboratori Nazionali del Gran Sasso (LNGS) is the first WIMP dark matter detector operating with a liquid xenon target mass above the ton-scale. Out of its 3.2 t liquid xenon inventory, 2.0 t constitute the active target of the dual-phase time projection chamb...
Fig. 4.— Bias of dark matter halos in four randomly selected cases upon different mass and redshift. The darkened lines show the fitting formulae of the bias relation. –13 – Table 2. Halo Bias : b(M,z) Halo Mass (h
For the power spectrum, we use the HaloFit non linear power spectrum [35], [36]. For the galaxy power spectrum, we use linear galaxy bias with the non-linear matter power spectrum. The galaxy-matter power spectrum (Σc2Pgκ) is obtained by direct inverse hankel transform of ΔΣ. The...
The effects of assembly bias on galaxy clustering predictions time, density concentration or subhalo occupation number [5, 6].On the other hand, semi-analytical models (SAM) populate galaxies in the dark matter haloes by modelling baryonic processes according to the potentials of dark matter [7....
for random walks with uncorrelated steps and general shapes of the moving barrier; we find the corresponding approximations of the unconditional and conditional halo mass functions for Cold Dark Matter power spectra to represent very well the outcomes of state-of-the-art cosmological N-body simulation...