English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We analyze the first set of cosmological baryonic zoom-in simulations ofgalaxies in dissipative self-interacting dark matter (dSIDM). The simulationsutilize the FIRE-2 galaxy formation physics with the inclusion of dissipativedark matter self-interactions modelled as a constant fractional energydissipation ($f_{\rm diss}=0.5$). In this paper, we examine the properties ofdwarf galaxies with $M_{\ast} \sim 10^{5}\operatorname{-}10^{9}\,{\rmM}_{\odot}$ in both isolation and within Milky Way-mass hosts. For isolateddwarfs, we find more compact galaxy sizes and promotion of stellar/neutral gasdisk formation in dSIDM with $(\sigma/m)\leq 1\,{\rm cm^2\,g^{-1}}$ but theyare still consistent with observed galaxy sizes and masses. In addition, as aresult of the steeper central density profiles developed in dSIDM, the sub-kpccircular velocities of isolated dwarfs in models with $(\sigma/m)\geq 0.1\,{\rmcm^2\,g^{-1}}$ are enhanced by about a factor of two, which are stillconsistent with the measured stellar velocity dispersions of Local Group dwarfsbut in tension with the HI rotation curves of more massive field dwarfs.Meanwhile, for satellites of the simulated Milky Way-mass hosts, the mediancircular velocity profiles are marginally affected by dSIDM physics, but dSIDMmay help address the missing compact dwarf satellites in CDM. The number ofsatellites is slightly enhanced in dSIDM, but the differences are smallcompared with the large host-to-host variations. In conclusion, the dSIDMmodels with constant cross-section $(\sigma/m) \gtrsim 0.1\,{\rm cm^2\,g^{-1}}$(assuming $f_{\rm diss}=0.5$) are effectively ruled out in bright dwarfs($M_{\rm halo}\sim 10^{11}\,{\rm M}_{\odot}$) by circular velocity constraints.However, models with lower effective cross-sections (at this halo mass/velocityscale) are still viable and can give rise to non-trivial observable signatures.

Dissipative Dark Matter on FIRE: II. Observational signatures and constraints from local dwarf galaxies