  We derive the Ultra-Violet (UV) luminosity function (LF) of star-forming
galaxies in the redshift range $z = 0.6 - 1.2$, in the rest-frame far-UV
($1500$ \r{A}) wavelength. For this work, we are in particular interested in
the bright end of the UV LF in this redshift range. Data from the XMM-Newton
Optical Monitor (XMM-OM), near-ultraviolet ($2410-3565$ \r{A}) observations
over 1.5 sq. deg of the COSMOS field are employed for this purpose. We compile
a source-list of $879$ sources with $UVW1_\mathrm{AB}$ in the range $\sim
21-24$ mags from the wide-area UVW1 image of the COSMOS field in the two bins
$0.6 \leq z \leq 0.8$ and $0.8 \leq z \leq 1.2$. The $M_{1500}$ for these
sources lies in the interval $[-19.10,-22.50]$. We use the maximum likelihood
to fit a Schechter function model to the un-binned data to estimate the
parameters (faint-end slope, characteristic magnitude, and normalisation) of
the Schechter function. We find the shape of the LF to be consistent with the
Schechter model, and the parameters are in fair agreement with other studies
conducted using direct measurements of the $1500$\r{A} flux. We see a
brightening of the characteristic magnitude as we move from lower ($0.7$) to
higher ($1.0$) redshift. The measures for luminosity density are within the
error margins of past studies. We examine the brightest sources in our sample
for the AGN contribution. These sources are characterised by their spectral
energy distributions, integrated infrared luminosities, and morphologies. We
also explore their overlap with the brightest IR galaxies in a similar redshift
range.
