Chandra survey of nearby highly inclined disc galaxies - II. Correlation analysis of galactic coronal properties

X-ray observations provide a key tool for exploring the properties of galactic coronae and their formation processes. In an earlier paper, we have presented a Chandra data analysis of the coronae of 53 nearby highly inclined disc galaxies. Here we study the correlation of the X-ray measurements of the coronae with other galaxy properties and compare the results with those obtained for elliptical galaxies. A good correlation is present between the coronal luminosity (L-X) and the star formation rate (SFR). But we find a better correlation between L-X and the total supernova (SN) mechanical energy input rate (E-SN), including the expected contribution from both core collapsed (CC) and Type Ia SNe. The X-ray radiation efficiency (eta equivalent to L-X/E-SN) of the coronae has a mean value of similar to 0.4 per cent with an rms of 0.50 +/- 0.06 dex. eta further correlates with M-TF/M-* (M-TF is the total baryon mass measured from the rotation velocity and the Tully-Fisher relation, and M-* is the stellar mass measured from the K-band luminosity) and the CC SN rate surface density [F-SN(CC), in units of SN yr(-1) kpc(-2)], which can be characterized as eta =(0.41(-0.12)(+0.13) per cent) M-TF/M-* and eta =(1.4 +/- 0.5 per cent)F-SN(CC)(-(0.29 +/- 0.11)). These correlations reflect the roles played by the gravitational mass and energetic feedback concentrations of the galaxies in determining their X-ray radiation efficiency. The characteristic temperature (T-X) of the coronal gas shows little dependence on the total or specific SFR, the cold gas content or L-X. The coronae of disc galaxies tend to be more X-ray luminous, hotter and lower in the Fe/O abundance ratio than those of elliptical ones of similar masses. Early-type non-starburst disc galaxies tend to be more Fe-rich, while starburst ones have a roughly constant abundance ratio of Fe/O similar to 0.36 +/- 0.12 solar. Our results are consistent with the coronal gas being mainly provided by stellar feedback in a galaxy stellar mass range of similar to 10(8.7-11) M-circle dot. In addition, processes such as charge exchange at cool/hot gas interfaces, as well as various other environmental effects, are also needed to explain the diversity of the observed coronal X-ray properties.