The optical-UV spectral energy distribution of the unabsorbed AGN
  population in the XMM-Newton Bright Serendipitous Survey
  Active galactic nuclei (AGN) emit radiation over a wide range of wavelengths,
with a peak of emission in the far-UV region of the electromagnetic spectrum, a
spectral region that is historically difficult to observe. Using optical, GALEX
UV and XMM-Newton data we derive the spectral energy distribution (SED) from
the optical/UV to X-ray regime of a sizeable sample of AGN. The principal
motivation is to investigate the relationship between the optical/UV emission
and the X-ray emission and provide bolometric corrections to the hard X-ray
(2-10 keV) energy range, kbol, the latter being a fundamental parameter in
current physical cosmology. We construct and study the X-ray to optical SED of
a sample of 195 X-ray selected Type 1 AGN belonging to the XMM-Newton bright
serendipitous survey (XBS). The optical-UV luminosity was computed using data
from the Sloan Digital Sky Survey (SDSS), from our own dedicated optical
spectroscopy and the satellite Galaxy Evolution Explorer (GALEX), while the
X-ray luminosity was computed using XMM-Newton data. Because it covers a wide
range of redshift (0.03 < z < 2.2), X-ray luminosities (41.8 < logL[2-10]keV <
45.5 erg/s) and because it is composed of "bright objects", this sample is
ideal for this kind of investigation. We find a correlation between kbol and
the hard X-ray photon index {\Gamma}(2-10keV) and a tight correlation between
the optical-to-X-ray spectral index {\alpha}ox and kbol, so we conclude that
both {\Gamma}(2-10keV) and {\alpha}ox can be used as a proxy for kbol.
