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We present results of the MUSE-ALMA Halos, an ongoing study of theCircum-Galactic Medium (CGM) of low redshift galaxies (z < 1.4), currentlycomprising 14 strong HI absorbers in five quasar fields. We detect 43 galaxiesassociated with absorbers down to star formation rate (SFR) limits of 0.01-0.1solar masses/yr, found within impact parameters (b) of 250 kpc from the quasarsightline. Excluding the targeted absorbers, we report a high detection rate of89 per cent and find that most absorption systems are associated with pairs orgroups of galaxies (three to eleven members). We note that galaxies with thesmallest impact parameters are not necessarily the closest to the absorbing gasin velocity space. Using a multi-wavelength dataset (UVES/HIRES, HST, MUSE), wecombine metal and HI column densities, allowing for derivation of the lowerlimits of neutral gas metallicity as well as emission line diagnostics (SFR,metallicities) of the ionised gas in the galaxies. We find that groups ofassociated galaxies follow the canonical relations of N(HI) -- b and W_r(2796)-- b, defining a region in parameter space below which no absorbers aredetected. The metallicity of the ISM of associated galaxies, when measured, ishigher than the metallicity limits of the absorber. In summary, our findingssuggest that the physical properties of the CGM of complex group environmentswould benefit from associating the kinematics of individual absorbingcomponents with each galaxy member.

MUSE-ALMA Halos V: Physical properties and environment of z < 1.4 HI quasar absorbers