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We present the analysis of Halpha3, an Halpha imaging survey of galaxiesselected from the HI ALFALFA Survey in the Coma Supercluster. By using theHalpha line as a tracer of the "instantaneous" star formation, complementedwith optical colors from SDSS we explore the hypothesis that a morphologicalsequence of galaxies of progressively earlier type, lower gas-content exists inthe neighborhood of the Coma cluster, with specific star formation activitydecreasing with increasing local galaxy density and velocity dispersion. In thedwarf regime (8.5<\log(M*)< 9.5) we identify a 4-step sequence of galaxies withprogressively redder colors, i.e. of decreasing specific star formation, from(1) HI-rich Late-Type Galaxies belonging to the blue-cloud exhibiting extendedplus nuclear star formation, (2) HI-poor LTGs with nuclear star formation only,(3) HI-poor galaxies with no star formation either extended or nuclear, butwith nuclear Post-Star-Burst signature,(4) Early-type Galaxies in thered-sequence, with no gas or star formation on all scales. Along this sequencethe quenching of the star formation proceeds radially outside-in. Theprogression toward redder colors found along this "morphological" (gas content)sequence is comparable to the one obtained increasing the local galaxy density,from the cosmic filaments (1,2), to the rich clusters (2,3,4). In the dwarfregime we find evidence for evolution of HI-rich LTGs into ETGs, passingthrough HI-poor and PSB galaxies, driven by the environment. We identifyram-pressure as the mechanism most likely responsible for this transformation.We conclude that infall of low-mass galaxies has proceeded for the last 7.5 Gyrbuilding up the Coma cluster at a rate of approximately 100 galaxies per Gyr.

Halpha3: an Halpha imaging survey of HI selected galaxies from ALFALFA. III. Nurture shapes up the Hubble sequence in the Great Wall