We investigated the typical environment and physical properties of ‘ ‘ red discs ’ ’ and ‘ ‘ blue bulges ’ ’ , comparing those to the ‘ ‘ normal ’ ’ objects in the blue cloud and red sequence .
Our sample is composed of cluster members and field galaxies at z \leq 0.1 , so that we can assess the impact of the local and global environment .
We find that disc galaxies display a strong dependence on environment , becoming redder for higher densities .
This effect is more pronounced for objects within the virial radius , being also strong related to the stellar mass .
We find that local and global environment affect galaxy properties , but the most effective parameter is stellar mass .
We find evidence for a scenario where ‘ ‘ blue discs ’ ’ are transformed into ‘ ‘ red discs ’ ’ as they grow in mass and move to the inner parts of clusters .
From the metallicity differences of red and blue discs , and the analysis of their star formation histories , we suggest the quenching process is slow .
We estimate a quenching time scale of \sim 2 - 3 Gyr .
We also find from the sSFR - M _ { * } plane that ‘ ‘ red discs ’ ’ gradually change as they move into clusters .
The ‘ ‘ blue bulges ’ ’ have many similar properties than ‘ ‘ blue discs ’ ’ , but some of the former show strong signs of asymmetry .
The high asymmetry ‘ ‘ blue bulges ’ ’ display enhanced recent star formation compared to their regular counterparts .
That indicates some of these systems may have increased their star formation due to mergers .
Nonetheless , there may not be a single evolutionary path for these blue early-type objects .