We report optical spectroscopy from the Very Large Telescope/FOcal Reducer and low dispersion spectroscopy of the two Ly alpha emitters (LAEs) companions to the quasi-stellar object-sub-millimetre galaxy system BRI1202-0725 at z = 4.7, which have recently been detected in the [C ii]158 mu m line by the Atacama Large Millimetre/Sub-millimetre Array. We detect Ly alpha emission from both sources and so confirm that these LAE candidates are physically associated with the BRI1202-0725 system. We also report the lack of detection of any high-ionization emission lines (N v lambda 1240, Si iv lambda 1396, C iv lambda 1549 and He ii lambda 1640) and find that these systems are likely not photoionized by the quasar, leaving in situ star formation as the main powering source of these LAEs. We also find that both LAEs have Ly alpha emission much broader (similar to 1300 km s(-1)) than the [C ii] emission and broader than most LAEs. In addition, both LAEs have roughly symmetric Ly alpha profiles implying that both systems are within the H ii sphere produced by the quasar. This is the first time that the proximity zone of a quasar is probed by exploiting nearby LAEs. We discuss the observational properties of these galaxies in the context of recent galaxy formation models.