  We study the effect of quasar feedback on distributions of baryons and
properties of intracluster medium in galaxy groups using high-resolution
numerical simulations. We use the entropy-conserving Gadget code that includes
gas cooling and star formation, modified to include a physically-based model of
quasar feedback. For a sample of ten galaxy group-sized dark matter halos with
masses in the range of 1 to $5\times 10^{13} M_{\odot}/h$, star formation is
suppressed by more than 50% in the inner regions due to the additional pressure
support by quasar feedback, while gas is driven from the inner region towards
the outer region of the halos. As a result, the average gas density is 50%
lower in the inner region and 10% higher in the outer region in the simulation,
compared to a similar simulation with no quasar feedback. Gas pressure is
lowered by about 40% in the inner region and higher in the outer region, while
temperature and entropy are enhanced in the inner region by about 20-40%. The
total group gas fraction in the two simulations generally differs by less than
10%. We also find a small change of the total thermal Sunyaev-Zeldovich
distortion, leading to 10% changes in the microwave angular power spectrum at
angular scales below two arcminutes.
