It is now day well know the existence of a link between the morphology and star formation activity of galaxies. However, how a galaxy reduces/stops the formation of new stars is a not well-understood process. Moreover, while many mechanisms are proposed to act as drivers of this process, their role/impact in the quenching is still a debated question, as well as if there is one or several of them acting simultaneously. Aiming to shed light on those open questions, we carried out a multi-wavelength analysis of the galaxies' structure. We took advantage of exquisite resolution and multi-wavelength coverage of HST data, to resolve and analyze bulges and discs for a large sample of galaxies. We found that the structure of the inner components weakly depends on the star-formation activity of the hosting galaxies. If one or more mechanisms are guiding the quenching, their effect results in a similar final structure. Moreover, we detected the presence of red bulges in star-forming galaxies, while there is a lack of red discs. This suggests that bulges are required but not necessary for quenching. Most, if not all, galaxies in the sample, present a negative color gradient. Such finding suggests an inside-out quenching. However, a rejuvenation mechanism would leave a similar signature. To differentiate the two mechanisms, we extended the analysis to the 54 narrow bands of J-PAS, to recover more precise and detailed stellar population properties like SFR and ages of bulges and discs.