We numerically investigate evolution of gaseous halos around disk galaxies in different environments ranging from small groups to rich clusters in order to understand galaxy evolution in these environments .
Our simulations self-consistently incorporate effects of ram pressure of intergalactic medium ( IGM ) on disk and halo gas of galaxies and hydrodynamical interaction between disk and halo gas so that mass fractions of halos gas stripped by ram pressure of IGM ( F _ { strip } ) can be better estimated .
We mainly investigate how F _ { strip } depends on total masses of their host environments ( M _ { host } ) , galactic masses ( M _ { gal } ) , densities and temperature of IGM ( T _ { IGM } and { \rho } _ { IGM } , respectively ) , relative velocities between IGM and galaxies ( V _ { r } ) , and physical properties of disks ( e.g. , gas mass fraction ) .
We find that typically 60 - 80 % of halo gas can be efficiently stripped from Milky Way-type disk galaxies by ram pressure in clusters with M _ { host } \sim 10 ^ { 14 } { M } _ { \odot } .
We also find that F _ { strip } depends on M _ { host } such that F _ { strip } is higher for larger M _ { host } .
Furthermore it is found that F _ { strip } can be higher in disk galaxies with smaller M _ { gal } for a given environment .
Our simulations demonstrate that the presence of disk gas can suppress ram pressure stripping of halo gas owing to hydrodynamical interaction between halo and disk gas .
Ram pressure stripping of halo gas is found to be efficient ( i.e. , F _ { strip } > 0.5 ) even in small and/or compact groups , if { \rho } _ { IGM } \sim 10 ^ { 5 } { M } _ { \odot } kpc ^ { -3 } and V _ { r } \sim 400 km s ^ { -1 } .
Based on the derived radial distributions of remaining halo gas after ram pressure stripping , we propose that truncation of star formation after halo gas stripping can occur outside-in in disk galaxies .
We suggest that although gradual truncation of star formation in disk galaxies can occur in groups , it can proceed less rapidly in comparison with cluster environments .
We also suggest low-mass galaxies are likely to truncate their star formation more rapidly owing to more efficient halo gas stripping in groups and clusters .