We present a high spectral resolution optical spectrum ( FWHM=17kms ^ { -1 } ) of the bright quasar Q1037-2704 .
The large number of absorption systems suggests the presence of an intervening supercluster , but the issue remains controversial .

We demonstrate that the strong C iv system at z _ { abs } \sim 2.08 spanning more than 1500kms ^ { -1 } is made up of narrow components with typical Doppler parameter b \sim 8kms ^ { -1 } .
The gas is probably photo-ionized in which case the photo-ionizing spectrum should be dominated by stellar radiation .
Analysis of H i , Si iv , N v and C iv absorptions shows that the gas has a fairly large metal content , Z > 0.1 Z _ { \odot } .

We detect C ii ^ { * } \lambda 1335 absorption in subcomponents of the z _ { abs } \sim 2.133 system , which have moderate total C ii column densities implying an electronic density of n _ { e } \sim 3cm ^ { -3 } .
In addition , the weakness of the O i \lambda 1302 , Si ii \lambda 1304 and Fe ii \lambda 1608 lines allows a detailed analysis of the line profiles .
The results are that the system has four narrow ( b \sim 10kms ^ { -1 } ) components ; the oxygen abundance is of the order of 0.03 solar ; the iron abundance is surprisingly large [ Fe/O ] \sim [ Fe/O ] _ { \odot } +0.3 .
If photo-ionized by the UV flux from the quasar , the distance between the absorber and the quasar should be larger than 0.3 h ^ { -1 } Mpc ( with h in units of H _ { o } =100kms ^ { -1 } Mpc ^ { -1 } and q _ { o } =0.5 ) .

This demontrates that the gas is not associated with the quasar and , together with the detection of eight multiple metal systems between z _ { abs } =1.91 and 2.13 , suggests the presence of a coherent structure extended over 80 h ^ { -1 } Mpc along the line of sight .

Key words : intergalactic medium , quasars : absorption lines