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Measurements of the total logarithmic central slope of the mass profile in galaxy clusters constrain their evolution and assembly history and that of their Brightest Cluster Galax-ies. We report the first full surface brightness distribution modelling of the inner region of the galaxy cluster MACS J1149.5+2223. We compare these results with a position-based modelling approach for which we employ more than twice the previously known positional constraints. This is the first time that the detailed lensed image configuration of two non-central cluster galaxies with Einstein rings has been mapped. Due to the extended radial cov-erage provided by the multiple images in this system, we are able to determine the slope ∂ log κ/ ∂ logR = −0.37 of the total projected mass distribution from 8 to 80 kpc. This is within the cluster-to-cluster scatter estimates from previous cluster measurements. Our recon-struction of the image surface brightness distribution of the large central spiral galaxy has a root mean square residual for all image pixels of 1.14 σ, where σ is the observational back-ground noise. This corresponds to a reconstruction of the positions of bright clumps in the central galaxy with a rms of 0.063 arcseconds.
Rau et al. (Thu,) studied this question.
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