Gas distributions inside and around haloes in the alternative dark matter simulations AIDA-TNG

Le résumé fourni par la source

The nature of dark matter (DM) is one of the greatest mysteries of modern astrophysics. While the standard cold DM (CDM) model successfully explains observations on most astrophysical scales, DM particles have not yet been detected, leaving room for a plethora of different models. In order to identify their observable signatures, we use the AIDA-TNG cosmological simulation suite to predict the distributions of gas and neutral hydrogen (HI) in the CDM, Self-interacting DM (SIDM), velocity-dependent SIDM (vSIDM), and warm DM (WDM) models. We find that the DM models investigated have very limited impact on the median gas and HI profiles of haloes. Nevertheless, for the most massive haloes ( M vir ∼ 10 14 M ⊙ ), we find that DM self-interactions can reduce the central potential, thereby lowering gravitational heating and the central gas temperature. We find that, in all models, the halo-to-halo variation in the HI profiles is explained by AGN feedback, and that the specific characteristics of the DM model are largely subdominant. Nevertheless, we detect some systematic difference in the case of SIDM, with more HI surviving close to the centre with respect to other models. We provide fitting functions for the gas and HI profiles. We investigate the galaxy- Ly α cross-correlation function ( GaL α CC ) for different halo masses, redshifts and observational strategies. We find that at z = 0 vSIDM can be distinguished from CDM in haloes with 10 12 ≲ M vir ≲ 10 13 M ⊙ , while SIDM1 can be distinguished from CDM in haloes with M vir ≳ 10 13 M ⊙ . We estimate that statistically robust detection requires sampling ∼ 160 haloes with ∼ 20 sightlines each, a task that can be achieved with current and future facilities like WEAVE, 4MOST, PFS, ELT and WST.

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