  We study the mean tidal coherence of galaxy environments as a function of
intrinsic luminosity determined by the absolute $r$-band magnitude. The tidal
coherence of a galaxy environment is estimated as the cosine of the angle
between two minor eigenvectors of the tidal field smoothed at the scales of $2$
and $30\,h^{-1}$Mpc centered on each of the local galaxies from the Sloan
Digital Sky Data Release 10. Creating four luminosity-selected samples of the
Sloan galaxies, we control them to have identical density distributions, in
order to nullify the dominant effect of the local density. It is found that the
samples containing more luminous wall and field galaxies yield lower mean
values of the tidal coherence, which trend turns out to be robust against the
variation of the smoothing scales. At fixed morphology, the same trend is found
for the late-type spiral and lenticular galaxies in both of the field and wall
environments. The early-type spiral field galaxies show no significant
dependence on the tidal coherence, while both of the least and most luminous
elliptical wall galaxies are found to dwell in the regions with highest tidal
coherence.
