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We present the analysis of the XMM-Newton data of the Circum-Galactic Mediumof MASsive Spirals (CGM-MASS) sample of six extremely massive spiral galaxiesin the local Universe. All the CGM-MASS galaxies have diffuse X-ray emissionfrom hot gas detected above the background extending $\sim(30-100)\rm~kpc$ fromthe galactic center. This doubles the existing detection of such extended hotCGM around massive spiral galaxies. The radial soft X-ray intensity profile ofhot gas can be fitted with a $\beta$-function with the slope typically in therange of $\beta=0.35-0.55$. This range, as well as those $\beta$ valuesmeasured for other massive spiral galaxies, including the Milky Way (MW), arein general consistent with X-ray luminous elliptical galaxies of similar hotgas luminosity and temperature, and with those predicted from a hydrostaticisothermal gaseous halo. Hot gas in such massive spiral galaxy tends to havetemperature comparable to its virial value, indicating the importance ofgravitational heating. This is in contrast to lower mass galaxies where hot gastemperature tends to be systematically higher than the virial one. The ratio ofthe radiative cooling to free fall timescales of hot gas is much larger thanthe critical value of $\sim10$ throughout the entire halos of all the CGM-MASSgalaxies, indicating the inefficiency of gas cooling and precipitation in theCGM. The hot CGM in these massive spiral galaxies is thus most likely in ahydrostatic state, with the feedback material mixed with the CGM, instead ofescaping out of the halo or falling back to the disk. We also homogenize andcompare the halo X-ray luminosity measured for the CGM-MASS galaxies and othergalaxy samples and discuss the "missing" galactic feedback detected in thesemassive spiral galaxies.

The Circum-Galactic Medium of MASsive Spirals II: Probing the Nature of Hot Gaseous Halo around the Most Massive Isolated Spiral Galaxies