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We present the first comprehensive study of a giant, $\approx \! \! 70$kpc-scale nebula around a radio-quiet quasar at $z<1$. The analysis is based ondeep integral field spectroscopy with MUSE of the field of HE$\,$0238$-$1904, aluminous quasar at $z=0.6282$. The nebula emits strongly in $\mathrm{[O \,II]}$, $\rm H \beta$, and $\mathrm{[O \, III]}$, and the quasar resides in anunusually overdense environment for a radio-quiet system. The environmentlikely consists of two groups which may be merging, and in total have anestimated dynamical mass of $M_{\rm dyn}\approx 4\times 10^{13}$ to $10^{14}\{\rm M_\odot}$. The nebula exhibits largely quiescent kinematics and irregularmorphology. The nebula may arise primarily through interaction-relatedstripping of circumgalactic and interstellar medium (CGM/ISM) of group members,with some potential contributions from quasar outflows. The simultaneouspresence of the giant nebula and a radio-quiet quasar in a rich environmentsuggests a correlation between such circum-quasar nebulae and environmentaleffects. This possibility can be tested with larger samples. The upper limitson the electron number density implied by the $\mathrm{[O \, II]}$ doubletratio range from $\log(n_{\rm e, \, [O \, II]} / \mathrm{cm^{-3}}) < 1.2$ to$2.8$. However, assuming a constant quasar luminosity and negligible projectioneffects, the densities implied from the measured line ratios between differentions (e.g., $\mathrm{[O\,II]}$, $\mathrm{[O\,III]}$, and $\mathrm{[Ne\,V]}$)and photoionization simulations are often $10{-}400$ times larger. This largediscrepancy can be explained by quasar variability on a timescale of $\approx10^4{-}10^5$ years.

The first comprehensive study of a giant nebula around a radio-quiet quasar in the $z < 1$ Universe