We carried out a detailed strong lensing analysis of a sub-sample of eight galaxy clusters of the Cluster Lensing And Supernova survey with Hubble ( CLASH ) in the redshift range of z _ { cluster } = [ 0.23 - 0.59 ] using extensive spectroscopic information , primarily from the Multi Unit Spectroscopic Explorer ( MUSE ) archival data and complemented with CLASH-VLT redshift measurements .
The observed positions of the multiple images of strongly lensed background sources were used to constrain parametric models describing the cluster total mass distributions .
Different models were tested in each cluster depending on the complexity of its mass distribution and on the number of detected multiple images .
Four clusters show more than five spectroscopically confirmed multiple image families .
In this sample , we did not make use of families that are only photometrically identified in order to reduce model degeneracies between the values of the total mass of a cluster source redshifts , in addition to systematics due to the potential misidentifications of multiple images .
For the remaining four clusters , we used additional families without any spectroscopic confirmation to increase the number of strong lensing constraints up to the number of free parameters in our parametric models .
We present spectroscopic confirmation of 27 multiply lensed sources , with no previous spectroscopic measurements , spanning over the redshift range of z _ { src } = [ 0.7 - 6.1 ] .
Moreover , we confirm an average of 48 galaxy members in the core of each cluster thanks to the high efficiency and large field of view of MUSE .
We used this information to derive precise strong lensing models , projected total mass distributions , and magnification maps .
We show that , despite having different properties ( i.e .
number of mass components , total mass , redshift , etc ) , the projected total mass and mass density profiles of all clusters have very similar shapes when rescaled by independent measurements of M _ { 200 c } and R _ { 200 c } .
Specifically , we measured the mean value of the projected total mass of our cluster sample within 10 ( 20 ) % of R _ { 200 c } to be 0.13 ( 0.32 ) of M _ { 200 c } , with a remarkably small scatter of 5 ( 6 ) % .
Furthermore , the large number of high-z sources and the precise magnification maps derived in this work for four clusters add up to the sample of high-quality gravitational telescopes to be used to study the faint and distant Universe .