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We combine wide and deep galaxy number-count data from GAMA, COSMOS/G10, HSTERS, HST UVUDF and various near-, mid- and far- IR datasets from ESO, Spitzerand 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, wederive the IGL and the extrapolated-IGL in all bands. We argue undetected lowsurface brightness galaxies and intra-cluster/group light is modest, and thatour extrapolated-IGL measurements are an accurate representation of theextra-galactic background light. Our data agree with most earlier IGL estimatesand with direct measurements in the far-IR, but disagree strongly with directestimates in the optical. Close agreement between our results and recent veryhigh-energy experiments (H.E.S.S. and MAGIC), suggest that there may be anadditional foreground affecting the direct estimates. The most likely culpritcould be the adopted Zodiacal light model. Finally we use a modified version ofthe two-component model to integrate the EBL and obtain measurements of theCosmic 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 asEuclid and WFIRST, have the capacity to reduce the COB error to $<1\%$, atwhich point comparisons to the very high energy data could have the potentialto provide a direct detection and measurement of the reionisation field.

Extra-galactic background light measurements from the far-UV to the far-IR from deep ground and space-based galaxy counts