Dissecting the Strong-lensing Galaxy Cluster MS 0440.5+0204. I. The Mass
  Density Profile
  We present a parametric strong lensing modeling of the galaxy cluster
MS\,0440.5+0204 (located at $z$ = 0.19). We have performed a strong lensing
mass reconstruction of the cluster using three different models. The first
model uses the image positions of four multiple imaged systems (providing 26
constraints). The second one combines strong lensing constraints with dynamical
information (velocity dispersion) of the cluster. The third one uses the mass
calculated from weak lensing as an additional constraint. Our three models
reproduce equally well the image positions of the arcs, with a root-mean-square
image equal to $\approx$0.5$\arcsec$. However, in the third model, the
inclusion of the velocity dispersion and the weak-lensing mass allows us to
obtain better constraints in the scale radius and the line-of-sight velocity
dispersion of the mass profile. For this model, we obtain $r_s$ =
132$^{+30}_{-32}$ kpc, $\sigma_s$ = 1203$^{+46}_{-47}$ km s$^{-1}$, M$_{200}$ =
3.1$^{+0.6}_{-0.6}$ $\times10^{14}$\,M$_{\odot}$, and a high concentration,
$c_{200}$ = 9.9$^{+2.2}_{-1.4}$. Finally, we used our derived mass profile to
calculate the mass up to 1.5 Mpc. We compare it with X-ray estimates previously
reported, finding a good agreement.
