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The cosmological inflow of a galaxy is speculated to be able to enter thegalaxy and enhance the star formation rate (SFR) and black hole accretion rate(BHAR). In this paper, by performing high-resolution hydrodynamic simulationsin the framework of {\it MACER}, we investigate the fate of the inflow and itsimpacts on the evolution of a massive elliptical galaxy. The inflow propertiesare adopted from the cosmological simulation IllustrisTNG. We find that, theinflow gas hardly enters but is blocked beyond $\sim 20$ kpc from the centralgalaxy and becomes part of the circumgalactic medium (CGM). The gas pressuregradient, mainly contributed by the thermalized stellar wind and subdominantlyby the energy input from the AGN, balances gravity and prevents the inflow fromentering the galaxy. The SFR and BHAR are almost not affected by the normalinflow. However, if the rate of cosmological inflow were increased by a factorof 3, a small fraction of the inflow would enter the galaxy and contributeabout 10\% of the gas in the galaxy. In this case, the gas density in thegalaxy would increase by a factor of $\ga$ 20. This increase is not because ofthe additional gas supply by the inflow but the increase of gas density in theCGM caused by the inflow. Consequently, the SFR and BHAR would increase by afactor of $\sim$ 5 and $\sim 1000$ respectively. Finally, AGN feedback canperturb the motion of the inflow and heat the CGM through its intermittentoutbursts.

Active galactic nuclei feedback in an elliptical galaxy (III): the impacts and fate of cosmological inflow