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Context: The galaxy cluster Abell S1101 (S1101 hereafter) deviatessignificantly from the X-ray luminosity versus velocity dispersion relation(L-sigma) of galaxy clusters in our previous study. Given reliable X-rayluminosity measurement combining XMM-Newton and ROSAT, this could most likelybe caused by the bias in the velocity dispersion due to interlopers and lowmember statistic in the previous sample of member galaxies, which was solelybased on 20 galaxy redshifts drawn from the literature. Aims: We intend toincrease the galaxy member statistic to perform a precision measurement of thevelocity dispersion and dynamical mass of S1101. We aim for a detailedsubstructure and dynamical state characterization of this cluster, and acomparison of mass estimates derived from (i) the velocity dispersion (M_vir),(ii) the caustic mass computation (M_caustic), and (iii) mass proxies fromX-ray observations and the Sunyaev-Zeldovich (SZ) effect. Methods: We carriedout new optical spectroscopic observations of the galaxies in this clusterfield with VIMOS, obtaining a sample of ~60 member galaxies for S1101. Werevised the cluster redshift and velocity dispersion measurements based on thissample and also applied the Dressler-Shectman substructure test. Results: Thecompleteness of cluster members within r200 was significantly improved for thiscluster. Tests for dynamical substructure did not show evidence for majordisturbances or merging activities in S1101. We find good agreement between thedynamical cluster mass measurements and X-ray mass estimates which confirms therelaxed state of the cluster displayed in the 2D substructure test. The SZ massproxy is slightly higher than the other estimates. The updated measurement ofthe velocity dispersion erased the deviation of S1101 in the L-sigma relation.

Probing the dynamical and X-ray mass proxies of the cluster of galaxies Abell S1101