The Radio – Far Infrared Correlation is a very tight empirical correlation believed to originate from the far ends of star-volution occurring in a galaxy. Far-Infrared light is emitted by heated dust around massive young stars, while electrons accelerated in Supernovae magnetic field generate Synchrotron radio emission. In recent studies it was shown that this correlation, usually parametrized by the “q-value”, is affected by the redshift and more importantly by the environment where galaxies reside and their morphology. By looking at a sample of 100 galaxies in the COSMOS field, we were able to determine their “q-value” using the VLA-deep radio survey and constrain their FIR Luminosities by running MAGPHYS on the new Herschel data. GALFIT was used to determine the morphology of the galaxies in the sample, based on the NIR K-Band image from the ULTRAVISTA survey. In my talk I will discuss how the correlation and other parameters, such as SFR and mass effectively change as a function of both redshift and galaxy type.