Galaxy cluster mass density profile derived using the submillimetre
  galaxies magnification bias
  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.
