Extra-galactic background light measurements from the far-UV to the
  far-IR from deep ground and space-based galaxy counts
  We combine wide and deep galaxy number-count data from GAMA, COSMOS/G10, HST
ERS, HST UVUDF and various near-, mid- and far- IR datasets from ESO, Spitzer
and Herschel. The combined data range from the far-UV (0.15microns) to far-IR
(500microns), and in all cases the contribution to the integrated galaxy light
(IGL) of successively fainter galaxies converges. Using a simple spline fit, we
derive the IGL and the extrapolated-IGL in all bands. We argue undetected low
surface brightness galaxies and intra-cluster/group light is modest, and that
our extrapolated-IGL measurements are an accurate representation of the
extra-galactic background light. Our data agree with most earlier IGL estimates
and with direct measurements in the far-IR, but disagree strongly with direct
estimates in the optical. Close agreement between our results and recent very
high-energy experiments (H.E.S.S. and MAGIC), suggest that there may be an
additional foreground affecting the direct estimates. The most likely culprit
could be the adopted Zodiacal light model. Finally we use a modified version of
the two-component model to integrate the EBL and obtain measurements of the
Cosmic Optical Background (COB) and Cosmic Infrared Background (CIB) of:
$24^{+4}_{-4}$nWm$^{-2}$sr$^{-1}$ and $26^{+5}_{-5}$nWm$^{-2}$sr$^{-1}$
respectively (48:52%). Over the next decade, upcoming space missions such as
Euclid and WFIRST, have the capacity to reduce the COB error to $<1\%$, at
which point comparisons to the very high energy data could have the potential
to provide a direct detection and measurement of the reionisation field.
