  We present the three-dimensional numerical simulation of jets modeled with
Relativistic Radiation Hydrodynamics (RRH), that evolve across two
environments: i) a stratified surrounding medium and ii) a 16TI progenitor
model. We consider opacities consistent with various processes of interaction
between the fluid and radiation, specifically, free-free, bound-free,
bound-bound and electron scattering. We explore various initial conditions,
with different radiation energy densities of the beam in hydrodynamical and
radiation pressure dominated scenarios, considering only ultra-relativistic
jets. In order to investigate the impact of the radiation field on the
evolution of the jets, we compare our results with purely hydrodynamical jets.
Comparing among jets driven by RRH, we find that radiation pressure dominated
jets propagate slightly faster than gas pressure dominated ones. Finally, we
construct the luminosity Light Curves (LCs) associated with all these cases.
The construction of LCs uses the fluxes of the radiation field which is fully
coupled to the hydrodynamics equations during the evolution. The main
properties of the jets propagating on the stratified surrounding medium are
that the LCs show the same order of magnitude as the gamma-ray luminosity of
typical Long Gamma-Ray Bursts $10^{50}-10^{54}$erg/s and the difference between
the radiation and gas temperatures is of nearly one order of magnitude. The
properties of jets breaking out from the progenitor star model are that the LCs
are of the order of magnitude of low-luminosity GRBs $10^{46}-10^{49}$ erg/s,
and in this scenario the difference between the gas and radiation temperature
is of four orders of magnitude, which is a case far from thermal equilibrium.
