  The UV (2000 A) luminosity function (hereafter UV LF) of Coma cluster
galaxies, based on more than 120 members, is computed as the statistical
difference between counts in the Coma direction and in the field. Our UV LF is
an up-date of a preliminary constrain on the UV LF previously computed without
the essential background counts. The UV LF is well described by a power law
with slope alpha~0.46, or equivalently, by a Schechter function with M* much
brighter than the brightest cluster galaxy and with a slope alpha_S~-2.0 or
larger. In spite of what happens in the optical band, low luminosity galaxies
give a large contribution to the integral luminosity, and by inference, to the
total metal production rate. Galaxies blue in UV-b and/or b-r dominate the Coma
cluster UV LF, both in number and luminosity. The major source of error in the
estimate of the UV LF cames from the background determination in the Coma
direction, which is still uncertain, even though constrained at high and low
amplitudes by redshift surveys covering the studied field.
