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We precisely constrain the inner mass profile of Abell 2261 (z=0.225) for thefirst time and determine this cluster is not "over-concentrated" as foundpreviously, implying a formation time in agreement with {\Lambda}CDMexpectations. These results are based on strong lensing analyses of new 16-bandHST imaging obtained as part of the Cluster Lensing and Supernova survey withHubble (CLASH). Combining this with revised weak lensing analyses of Subaruwide field imaging with 5-band Subaru + KPNO photometry, we place tight newconstraints on the halo virial mass M_vir = 2.2\pm0.2\times10^15 M\odot/h70(within r \approx 3 Mpc/h70) and concentration c = 6.2 \pm 0.3 when assuming aspherical halo. This agrees broadly with average c(M,z) predictions from recent{\Lambda}CDM simulations which span 5 <~ <c> <~ 8. Our most significantsystematic uncertainty is halo elongation along the line of sight. To estimatethis, we also derive a mass profile based on archival Chandra X-rayobservations and find it to be ~35% lower than our lensing-derived profile atr2500 ~ 600 kpc. Agreement can be achieved by a halo elongated with a ~2:1 axisratio along our line of sight. For this elongated halo model, we find M_vir =1.7\pm0.2\times10^15 M\odot/h70 and c_vir = 4.6\pm0.2, placing rough lowerlimits on these values. The need for halo elongation can be partially obviatedby non-thermal pressure support and, perhaps entirely, by systematic errors inthe X-ray mass measurements. We estimate the effect of background structuresbased on MMT/Hectospec spectroscopic redshifts and find these tend to lowerMvir further by ~7% and increase cvir by ~5%.

CLASH: Precise New Constraints on the Mass Profile of Abell 2261