The hot environment of galaxy clusters represents a site of dramatic changes in member galaxies' morphology as they shift from blue gas-rich to red gas-poor objects due to multiple processes.  One of the essential external processes seems to be the ram pressure stripping that galaxies experience while moving with high velocities through the hot intra-cluster medium (ICM). During this process, the gas reservoir of galaxies is gradually depleted from outside in. Without any gas in the disk left, the star formation of the galaxy is quenched. However, a very different story evolves in the tail behind the parent galaxy. After leaving the disk, the displaced gas presumably mixes with the ICM forming a multi-phase environment including the molecular component. In some cases, even a star formation can occur and as a result, the tail lights up and creates what is referred to as a "jellyfish galaxy". Yet, details of the evolution of the tail gas remain unknown and are subject of intense research. We present a new CO observation of 5 Coma cluster galaxies and their tails from the IRAM telescope.