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With a projected size of about 450 kpc at z~2.3, the Slug Ly-alpha nebula isa rare laboratory to study, in emission, the properties of the intergalacticgas in the Cosmic Web. Since its discovery, the Slug has been the subject ofseveral spectroscopic follow-ups to constrain the properties of the emittinggas. Here we report the results of a deep MUSE integral-field spectroscopicsearch for non-resonant, extended HeII1640 and metal emission. Extended HeIIradiation is detected on scales of about 100 kpc, but only in some regionsassociated with the bright Ly-alpha emission and a continuum-detected source,implying large and abrupt variations in the line ratios across adjacent regionsin projected space. The recent detection of associated H-alpha emission andsimilar abrupt variations in the Ly-alpha kinematics, strongly suggest that theHeII/Ly-alpha gradient is due to large variations in the physical distancesbetween the associated quasar and these regions. This implies that the overalllength of the emitting structure could extend to physical Mpc scales and bemostly oriented along our line of sight. At the same time, the relatively lowHeII/Ly-alpha values suggest that the emitting gas has a broad densitydistribution that - if expressed in terms of a lognormal - implies dispersionsas high as those expected in the interstellar medium of galaxies. These resultsstrengthen the possibility that the density distribution of intergalactic gasat high-redshift is extremely clumpy and multiphase on scales below our currentobservational spatial resolution of a few physical kpc.

The large and small scale properties of the intergalactic gas in the Slug Ly-alpha nebula revealed by MUSE HeII emission observations