论文标题
多组分模型中的暗物质光环。 iii。从矮人到星系群
Dark matter haloes in the multicomponent model. III. From dwarfs to galaxy clusters
论文作者
论文摘要
DM成为多组分的可能性对在小规模上解决已知的宇宙学问题有很大的意义。除了弹性散射外，该模型还允许非弹性相互作用，可以以“速度踢”参数为特征。最简单的2CDM模型，具有横节$ 0.01 \LISSSIMσ/M <1 \ 1 \ textrm {cm}^{2} {2} {\ rm g}^{ - 1} $和踢速度$ v_ {k} \ simeq 100 \ simeq 100 \ textrm s}在$ n $ n $ - 体宇宙学中的Core-Cusp和Too-to-to-to Fail问题在类似于病毒质量的MW的光环$ \ sim5 \ sim5 \ times 10^{11} $ m $ _ {\ odot} $（Paper I $ \＆$ II）上测试。为了进一步限制2CDM模型可用的参数空间，我们将分析扩展到矮人和星系集群光环，其病毒质量为$ \ sim 10^7-10^8 $和$ \ sim 10^{13} - 10^{14} {14} $ M $ M $ _ {\ odot} $。我们发现$σ_{0} / m \ gtrsim 0.1 \ textrm {cm}^{2} {\ rm g}^{ - 1} $优先不利于dwarfs和Galaxy cluster haloes与观测值相比，而$ fectervations，而$ fextervations $ = 0} / M = 0} / M = 0} / M = 0} / M = M. cm}^{2} {\ rm g}^{ - 1} $在此工作中研究了大多数横截面的速度依赖性，与CDM对应物的差异很小。我们的主要结果是，在合理的参数集中，2CDM模型可以成功解释矮星系和星系群集光环中看到的观察趋势，并且该模型为我们提供了其他可能的替代DM模型的打开窗口。
A possibility of DM being multicomponent has a strong implication on resolving decades-long known cosmological problems on small scale. In addition to elastic scattering, the model allows for inelastic interactions, which can be characterized by a 'velocity kick' parameter. The simplest 2cDM model with cross section $0.01\lesssimσ/m<1\textrm{ cm}^{2}{ \rm g}^{-1}$ and the kick velocity $V_{k}\simeq 100\textrm{ km s}^{-1}$ has been shown to robustly resolve the missing satellites, core-cusp, and too-big-to-fail problems in $N$-body cosmological simulations tested on MW-like haloes of a virial mass $\sim5 \times 10^{11}$ M$_{\odot}$ (Paper I $\&$ II). With the aim of further constraining the parameter space available for the 2cDM model, we extend our analysis to dwarf and galaxy cluster haloes with their virial mass of $\sim 10^7 - 10^8$ and $\sim 10^{13} - 10^{14}$ M$_{\odot}$, respectively. We find $σ_{0} / m \gtrsim 0.1 \textrm{ cm}^{2}{\rm g}^{-1}$ is preferentially disfavored for both dwarfs and galaxy cluster haloes in comparison with observations, while $σ_{0} / m = 0.001 \textrm{ cm}^{2}{\rm g}^{-1}$ causes little perceptible difference from that of the CDM counterpart for most of the cross section's velocity dependence studied in this work. Our main result is that within the reasonable set of parameters the 2cDM model can successfully explain the observational trends seen in dwarf galaxy and galaxy cluster haloes and the model leaves us an open window for other possible alternative DM models.
