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We present an analysis of the hot interstellar medium (ISM) in the spiralgalaxy NGC 4490, which is interacting with the irregular galaxy NGC 4485, using~100ks of Chandra ACIS-S observations. The high angular resolution of Chandraenables us to remove discrete sources and perform spatially resolvedspectroscopy for the star forming regions and associated outflows, allowing usto look at how the physical properties of the hot ISM such as temperature,hydrogen column density and metal abundances vary throughout these galaxies. Wefind temperatures of >0.41 keV and 0.85 +0.59/-0.12 keV, electron densities of>1.87 eta^(-1/2) x 10^(-3) cm^(-3) and 0.21 +0.03/-0.04 eta^(-1/2) x 10^(-3)cm^(-3), and hot gas masses of >1.1 eta^(1/2) x 10^7 M_{\odot} and ~3.7eta^(1/2) x 10^7 M_{\odot} in the plane and halo of NGC 4490 respectively,where eta is the filling factor of the hot gas. The abundance ratios of Ne, Mgand Si with respect to Fe are found to be consistent with those predicted bytheoretical models of type II supernovae. The thermal energy in the hot ISM is~5% of the total mechanical energy input from supernovae, so it is likely thatthe hot ISM has been enriched and heated by type II supernovae. The X-rayemission is anticorrelated with the H-alpha and mid-infrared emission,suggesting that the hot gas is bounded by filaments of cooler ionized hydrogenmixed with warm dust.

The Hot Interstellar Medium of the Interacting Galaxy NGC 4490