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Numerical Simulations of Hot Halo Gas in Galaxy Mergers

Galaxy merger simulations have explored the behaviour of gas within the galactic disk, yet the dynamics of hot gas within the galaxy halo has been neglected. We report on the results of high-resolution hydrodynamic simulations of colliding galaxies with hot halo gas. We explore a range of mass ratios, gas fractions and orbital configurations to constrain the shocks and gas dynamics within the progenitor haloes. We find that : (i) A strong shock is produced in the galaxy haloes before the first passage, increasing the temperature of the gas by almost an order of magnitude to $T\sim 10^{6.3}$ K. (ii) The X-ray luminosity of the shock is strongly dependent on the gas fraction; it is $\gtrsim 10^{39}$ erg/s for halo gas fractions larger than 10%. (iii) The hot diffuse gas in the simulation produces X-ray luminosities as large as $10^{42}$ erg/s. This contributes to the total X-ray background in the Universe. (iv) We find an analytic fit to the maximum X-ray luminosity of the shock as a function of merger parameters. This fit can be used in semi-analytic recipes of galaxy formation to estimate the total X-ray emission from shocks in merging galaxies. (v) $\sim$ 10-20% of the initial gas mass is unbound from the galaxies for equal-mass mergers, while $3-5%$ of the gas mass is released for the 3:1 and 10:1 mergers. This unbound gas ends up far from the galaxy and can be a feasible mechanism to enrich the IGM with metals.