  In this work we want to study the average mass density profile of tens to
hundreds of clusters of galaxies acting as lenses that produce a magnification
bias on the SMGs, and to estimate their associated masses and concentrations
for different richness ranges. The background sample is composed of SMGs
observed by Herschel with 1.2<z<4.0 (mean redshift at ~2.3) while the
foreground sample is made up of galaxy clusters extracted from the SDSS III
with photometric redshifts of 0.05< z< 0.8 (mean redshift at ~0.38).
Measurements are obtained by stacking the SMG--cluster pairs to estimate the
cross-correlation function using the Davis-Peebles estimator. This methodology
allows us to derive the mass density profile for a wide range of angular
scales, ~2-250 arcsec or ~10-1300 kpc for z=0.38, with a high radial
resolution. We find that It is impossible to fit the data with a single mass
density profile at all scales. As for the outer part, the estimated average
masses increase from $M_{200c}=5.8$ to $51.5\times 10^{13} M_\odot$ and the
concentration parameter from C=0.74 to 1.74. In the small-scale regions, the
obtained average masses fluctuate around $M_{200c}=3-4 \times 10^{13}M_\odot$
with average C~4. The total average masses are in perfect agreement with the
M-R relationship estimated from the cluster catalogue. While the estimated
average C values of the central galactic halos are in agreement with
traditional M-C relationships, we find low concentrations for the outer part.
Moreover, C decrease for lower R values, probably indicating that the group of
galaxies cannot be considered to be relaxed systems. Finally, we notice a
systematic lack of signal at the transition between the dominance of the
cluster halo and the central galactic halo (~100 kpc). This feature is also
present in previous studies using different catalogues and/or methodologies,
but is never discussed.
