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The cosmic baryonic fluid at low redshifts is similar to a fully developedturbulence. In this work, we use simulation samples produced by the hybridcosmological hydrodynamical/N-body code, to investigate on what scale thedeviation of spatial distributions between baryons and dark matter is caused byturbulence. For this purpose, we do not include the physical processes such asstar formation, supernovae (SNe) and active galactic nucleus (AGN) feedbackinto our code, so that the effect of turbulence heating for IGM can beexhibited to the most extent. By computing cross-correlation functions $r_m(k)$for the density field and $r_v(k)$ for the velocity field of both baryons anddark matter, we find that deviations between the two matter components for bothdensity field and velocity field, as expected, are scale-dependent. That is,the deviations are the most significant at small scales and gradually diminishon larger and larger scales. Also, the deviations are time-dependent, i.e. theybecome larger and larger with increasing cosmic time. The most emphasizedresult is that the spatial deviations between baryons and dark matter revealedby velocity field are more significant than that by density field. At z = 0, atthe 1% level of deviation, the deviation scale is about 3.7 $h^{-1}$Mpc fordensity field, while as large as 23 $h^{-1}$Mpc for velocity field, a scalethat falls within the weakly non-linear regime for the structure formationparadigm. Our results indicate that the effect of turbulence heating is indeedcomparable to that of these processes such as SN and AGN feedback.

Turbulence-induced deviation between baryonic field and dark matter field in the spatial distribution of the Universe