  This project is the continuation of our study of faint Low Surface Brightness
Galaxies (fLSBs) in one of the densest nearby galaxy regions known, the Coma
cluster. Our goal is to improve our understanding of the nature of these
objects by comparing the broad band spectral energy distribution with
population synthesis models. The data were obtained with the MEGACAM and CFH12K
cameras at the CFHT. We used the resulting photometry in 5 broad band filters
(u*, B, V, R, and I), that included new u*-band data, to fit spectral models.
With these spectral fits we inferred a cluster membership criterium, as well as
the ages, dust extinctions, and photometric types of these fLSBs. We show that
about half of the Coma cluster fLSBs have a spectral energy distribution well
represented in our template library while the other half present a flux deficit
at ultraviolet wavelengths. Among the well represented, ~80% are probably part
of the Coma cluster based on their spectral energy distribution. They are
relatively young (younger than 2.3 Gyrs for 90% of the sample) non-starburst
objects. The later their type, the younger fLSBs are. A significant part of the
fLSBs are quite dusty objects. fLSBs are low stellar mass objects (the later
their type the less massive they are), with stellar masses comparable to
globular clusters for the faintest ones. Their characteristics are correlated
with infall directions, confirming the disruptive origin for part of them.
