Dark matter haloes in the multicomponent model. III. From dwarfs to galaxy clusters

A possibility of DM being multicomponent has a strong implication on resolving decades-long known cosmological problems small scale. In addition to elastic scattering, the model allows for inelastic interactions, which can be characterized by 'velocity kick' parameter. The simplest 2cDM with cross section $0.01\lesssim\sigma/m<1\textrm{ cm}^{2}{ \rm g}^{-1}$ and kick velocity $V_{k}\simeq 100\textrm{ km s}^{-1}$ been shown robustly resolve missing satellites, core-cusp, too-big-to-fail in $N$-body simulations tested MW-like haloes virial mass $\sim5 \times 10^{11}$ M$_{\odot}$ (Paper I $\&$ II). With aim further constraining parameter space available model, we extend our analysis dwarf galaxy cluster their $\sim 10^7 - 10^8$ 10^{13} 10^{14}$ M$_{\odot}$, respectively. We find $\sigma_{0} / m \gtrsim 0.1 \textrm{ cm}^{2}{\rm is preferentially disfavored both dwarfs comparison observations, while = 0.001 causes little perceptible difference from that CDM counterpart most section's dependence studied this work. Our main result within reasonable set parameters successfully explain observational trends seen leaves us an open window other possible alternative models.