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We report spectroscopic identification of the host galaxies of 18ultra-strong MgII systems (USMgII) at $0.6 \leq z \leq 0.8$. We created thelargest sample by merging these with 20 host galaxies from our previous surveywithin $0.4 \leq z \leq 0.6$. Using this sample, we confirm that the measuredimpact parameters ($\rm 6.3\leq D[kpc] \leq 120$ with a median of 19 kpc) aremuch larger than expected, and the USMgII host galaxies do not follow thecanonical $\rm W_{2796}-D$ anti-correlation. We show that the presence andsignificance of this anti-correlation may depend on the sample selection. The$\rm W_{2796}-D$ anti-correlation seen for the general MgII absorbers show amild evolution at low $\rm W_{2796}$ end over the redshift range $0.4 \leq z\leq 1.5$ with an increase of the impact parameters. Compared to the hostgalaxies of normal MgII absorbers, USMgII host galaxies are brighter and moremassive for a given impact parameter. While the USMgII systems preferentiallypick star-forming galaxies, they exhibit slightly lower ongoing star-formingrates compared to main sequence galaxies with the same stellar mass, suggestinga transition from star-forming to quiescent states. For a limiting magnitude of$m_r < 23.6$, at least $29\%$ of the USMgII host galaxies are isolated, and thewidth of the MgII absorption in these cases may originate from gas flows(infall/outflow) in isolated halos of massive star-forming but not starburstinggalaxies. We associate more than one galaxy with the absorber in $\ge 21\%$cases where interactions may cause wide velocity spread.

Host galaxies of Ultra-Strong MgII absorbers at $z \sim 0.7$