We use ACDM numerical simulations to model the density profiles and substructure populations in a set of sixteen dark matter halos with resolutions of up to seven million particles within the virial radius. These simulations allow us to follow robustly the formation and evolution of the central cusp over a large mass range of 1011 to 1014 M? down to approximately 0.5 % of the virial radius, and from redshift 5 to the present. The cusp of the density profile is set at redshifts of two or greater and remains remarkably stable to the present time, when considered in non-comoving coordinates We fit our halos to a 2 parameter profile where the steepness of the asymptotic cusp is given by 7, and its radial extent is described by the concentration, c7. In our simulations, we find 7 = 1.4 - 0,08Log(M/M") for halos of 0..01M, to 1000M,, with a large scatter of A7 ~ ±0,3; and c7 = 8(Af/M*)~° 16 with a large M/M* dependent scatter roughly equal to ±c7. Our redshift zero halos have inner slope parameters ranging approximately from r"1 to r^1 5, with a median of roughly r^1 3 This two parameter profile fit works well for all halo types present in our simulations, whether or not they show evidence of a steep asymptotic cusp.The substructure population is independent of host halo mass and redshift with halo to halo scatter in the substructure velocity distribution function of a factor of roughly two to four. The radial distribution of substructure halos (subhalos) is consistent with the mass profile over the radial range where the possibility of artificial numerical disruption of subhalos can be most reliably excluded, r Si 0,3 ru,r, although a weakly shallower subhalo profile is favored by the data. We discuss the implications that our results have on gravitational lensing studies of halo structure.
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机译：我们使用ACDM数值模拟在一组十六颗暗物质卤素中模拟密度型材和子结构群体，其中在病毒半径内具有高达七百万颗粒的分辨率。这些模拟使我们能够遵循强大的尖端的形成和演变在1011至1014米的大量质量范围内？低至大约0.5％的病毒半径，以及来自目前的红移5。密度曲线的尖端被设定为两种或更大的红移，并且当在非Comoving坐标中考虑时，我们将光晕突出为2个参数曲线，在渐近CUSP的陡度给出7的情况下，保持显着稳定。并且其径向范围由浓度C7描述。在我们的模拟中，我们发现0..01m的晕圈为1.4 - 0,08次（M / m“），达到1000米，散射大，散射为A7〜±0,3;和C7 = 8（AF / m *）〜°16具有大的M / m *依赖性散射大致等于±C7。我们的红移零晕具有大约从R“1到R ^ 1 5的内斜率参数，其中中位数为R ^ 1 3这两个参数概况适合我们模拟中存在的所有Halo类型，无论它们都显示出陡峭的渐近尖端的证据。下子结构群体与主晕质量和晕圈与光环散射在子结构速度分布函数中独立于HALO散射。一个大约两到四个的因素。子结构晕晕（SubHalos）的径向分布与径向范围内的质量型材一致，其中可以最可靠地排除了亚哈尔斯的人工数值破坏的可能性，R SI 0,3 Ru，R，虽然弱较浅的次麦曲线受数据的青睐。我们讨论了我们的结果对光环结构引力透镜研究的影响。
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