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A large fraction of the baryonic matter in the Universe is located infilaments in the intergalactic medium. However, the low surface brightness ofthese filaments has not yet allowed their direct detection except in veryspecial regions in the circum-galactic medium (CGM). Here we simulate theintensity and spatial fluctuations in Lyman Alpha ${\rm (Ly\alpha)}$ emissionfrom filaments in the intergalactic medium (IGM) and discuss the prospects forthe next generation of space based instruments to detect the low surfacebrightness universe at UV wavelengths. Starting with a high resolution N-bodysimulation we obtain the dark matter density fluctuations and associate baryonswith the dark matter particles assuming that they follow the same spatialdistribution. The IGM thermal and ionization state is set by a model of the UVbackground and by the relevant cooling processes for a hydrogen and helium gas.The ${\rm Ly\alpha}$ emissivity is then estimated, taking into accountrecombination and collisional excitation processes. We find that the detectionof these filaments through their ${\rm Ly\alpha}$ emission is well in the reachof the next generation of UV space based instruments and so it should beachieved in the next decade. The density field is populated with halos andgalaxies and their ${\rm Ly\alpha}$ emission is estimated. Galaxies are treatedas foregrounds and so we discuss methods to reduce their contamination fromobservational maps. Finally, we estimate the UV continuum background as afunction of the redshift of the ${\rm Ly\alpha}$ emission line and discuss howthis continuum can affect observations.

Mapping the low surface brightness Universe in the UV band with Lya emission from IGM filaments