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We present a study comparing OVI $\lambda\lambda$1031, 1037 doubletabsorption found towards group galaxy environments with that of isolatedgalaxies. The OVI absorption in the circumgalactic medium (CGM) of isolatedgalaxies has been studied previously by the "Multiphase Galaxy Halos" survey,where the kinematics and absorption properties of the CGM have beeninvestigated. We extend these studies to group environments. We define a galaxygroup to have two or more galaxies having a line-of-sight velocity differenceof no more than 1000 km/s and located within 350 kpc (projected) of abackground quasar sightline. We identified a total of six galaxy groupsassociated with OVI absorption $W_{\rm r}>0.06$ {\AA} that have a medianredshift of $\langle z_{\rm gal} \rangle = 0.1669$ and a median impactparameter of $\langle D \rangle = 134.1$ kpc. An additional 12 non-absorbinggroups were identified with a median redshift of $\langle z_{\rm gal} \rangle =0.2690$ and a median impact parameter of $\langle D \rangle = 274.0$ kpc. Wefind the average equivalent width to be smaller for group galaxies than forisolated galaxies $(3\sigma)$. However, the covering fractions are consistentwith both samples. We used the pixel-velocity two-point correlation functionmethod and find that the velocity spread of OVI in the CGM of group galaxies issignificantly narrower than that of isolated galaxies $(10\sigma)$. We suggestthat the warm/hot CGM does not exist as a superposition of halos, instead, thevirial temperature of the halo is hot enough for OVI to be further ionised. Theremaining OVI likely exists at the interface between hot, diffuse gas andcooler regions of the CGM.

The Impact of the Group Environment on the OVI Circumgalactic Medium