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We present new results on the auto- and cross-correlation functions ofgalaxies and OVI absorbers in a $\sim 18~\textrm{Gpc}^3$ comoving volume at $z< 1$. We use a sample of 51,296 galaxies and 140 OVI absorbers in the columndensity range $13 \lesssim \log N \lesssim 15$ to measure two-point correlationfunctions in the two dimensions transverse and orthogonal to the line-of-sight$\xi(r_{\perp}, r_{\parallel})$. We furthermore infer the corresponding'real-space' correlation functions, $\xi(r)$, by projecting $\xi(r_{\perp},r_{\parallel})$ along $r_{\parallel}$, and assuming a power-law form, $\xi(r) =(r / r_0)^{-\gamma}$. Comparing the results from the absorber-galaxycross-correlation function, $\xi_{\textrm{ag}}$, the galaxy auto-correlationfunction, $\xi_{\textrm{gg}}$, and the absorber auto-correlation function,$\xi_{\textrm{aa}}$, we constrain the statistical connection between galaxiesand the metal-enriched intergalactic medium as a function of star-formationactivity. We also compare these results to predictions from the EAGLEcosmological hydrodynamical simulation and find a reasonable agreement. We findthat: (i) OVI absorbers show very little velocity dispersion with respect togalaxies on $\sim$ Mpc scales, likely $\lesssim$ 100 \kms; (ii) OVI absorbersand galaxies may not linearly trace the same underlying distribution of matterin general. In particular, our results demonstrate that OVI absorbers are lessclustered, and potentially more extended around galaxies than galaxies arearound themselves; (iii) On $\gtrsim 100$ kpc scales, the likelihood of findingOVI absorbers around star-forming galaxies is similar to the likelihood offinding OVI absorbers around non star-forming galaxies (abridged)

On the connection between the metal-enriched intergalactic medium and galaxies: an OVI-galaxy cross-correlation study at $z < 1$