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We present spectroscopic observations of the rest-frame UV line emissionaround radio galaxy MRC 2104-242 at z=2.49, obtained with FORS1 on VLT Antu.The morphology of the halo is dominated by two spatially resolved regions. Lyais extended by >12 arcsec along the radio axis, CIV and HeII are extended by ~8arcsec. The overall spectrum is typical for that of high redshift radiogalaxies. The most striking spatial variation is that NV is present in thespectrum of the region associated with the center of the galaxy hosting theradio source, the northern region, while absent in the southern region.Assuming that the gas is photoionized by a hidden quasar, the difference in NVemission can be explained by a metallicity gradient within the halo. This isconsistent with a scenario in which the gas is associated with a massivecooling flow or originates from the debris of the merging of two or moregalaxies.Comment: Accepted for publication in A&A Letter

Deep VLT spectroscopy of the $\vec{z}=$ 2.49 radio galaxy MRC 2104-242