  We present near-infrared H-band (1.65 micron) surface brightness profile
decomposition for 1157 galaxies in five nearby clusters of galaxies: Coma,
A1367, Virgo, A262 and Cancer, and in the bridge between Coma and A1367 in the
"Great Wall". The optically selected (m_p<=16.0) sample is representative of
all Hubble types, from E to Irr+BCD, except dE and of significantly different
environments, spanning from isolated regions to rich clusters of galaxies. We
model the surface brightness profiles with a de Vaucouleurs r^(1/4) law (dV),
with an exponential disk law (E), or with a combination of the two (B+D). From
the fitted quantities we derive the H band effective surface brightness (mu_e)
and radius (r_e) of each component, the asymptotic magnitude H_T and the light
concentration index C_31. We find that: i) Less than 50% of the Elliptical
galaxies have pure dV profiles. The majority of E to Sb galaxies is best
represented by a B+D profile. All Scd to BCD galaxies have pure exponential
profiles. ii) The type of decomposition is a strong function of the total H
band luminosity (mass), independent of the Hubble classification: the fraction
of pure exponential decompositions decreases with increasing luminosity, that
of B+D increases with luminosity. Pure dV profiles are absent in the low
luminosity range L_H<10^(10) L_solar and become dominant above 10^(11) L_solar.
