Scaling relations, dynamical heating and tidal disruption in spin s ultralight dark matter models

We explore the impact of spin 0, spin 1 and spin 2 Ultra-Light Dark Matter (ULDM) on small scales by numerically solving the Schrödinger-Poisson system using the time-split method. We perform simulations of ULDM for each spin, starting with different numbers of identical initial solitons and analyse the properties of the resulting halos after they merge. Our findings reveal that higher spin lead to broader, less dense halos with more prominent Navarro-Frenk-White (NFW) tails, a characteristic that persists regardless of the number of solitons involved. Additionally, we study the process of dynamical heating for these haloes, and find that the heating time-scale for higher spin increases order of magnitude compared to the spin 0 case. Then, we identify scaling relations that describe the density profile, core-NFW of spin s ULDM halos as a function of the number of initial solitons Nsol. These relations allow us to construct equivalent halos based on average density or total mass, for arbitrarily large Nsol, without having to simulate those systems. We simulate the orbit of a ULDM satellite in a constructed halo treated as an external potential, and find that for host halos having the same average density, the disruption time of the satellite is as predicted for uniform sphere regardless of the spin. However, satellites orbiting haloes having the same mass for each spin, result in faster disruption in the case of spin 0, whereas for haloes having the same core size result in faster disruption in the case of spin 2.