  We present the rest-frame Ultra-Violet (UV) galaxy luminosity function (LF)
and luminosity density (LD) measurements in the far-UV (150 nm) wavelength, in
the redshift range z = 0.6 - 1.2. The UV LF is derived using XMM-Newton Optical
Monitor (XMM-OM), ultraviolet (160 - 400 nm) observations of the Chandra Deep
Field South, over an area of 396 sq. arcmin. Using the deep UV imaging of the
CDFS, we identified more than 2500 galaxies in our sample with faint UVW1(AB)
limit 24.5 mag. This sample along with various other catalogues containing
redshift information, is used to calculate the binned representation of the
galaxy UV LF in the two redshift bins 0.6 - 0.8 and 0.8 - 1.2, having a wide
range of 150 nm rest-frame UV magnitudes, reaching 1 - 1.5 magnitudes fainter
than previous studies at similar redshifts. The binned LF is described well by
the Schechter function form. Using maximum-likelihood the Schechter function is
fitted to the unbinned data to obtain the best-fit values of the the UV galaxy
LF parameters. We find that characteristic magnitude brightens by 0.8 mag from
z = 0.7 to z = 1, implying an increase in the star formation activity between
these redshifts, as reported by past studies. Our estimate of the faint-end
slope -1.10+0.19-0.18 is on the shallower side compared with previous studies
at z = 0.7, whereas a value of -1.56+0.19-0.18 estimated for z = 1.0, agrees
with previous results given the uncertainties.
