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Fig. 7


Results of the four different steps comprising our algorithm. a) The input to our pipeline is the normalised, line of sight projected velocity-dispersion profile as a function of the projected radius and weighted by the galaxy number density. b) The Richardson-Lucy deprojection algorithm yields an effective galaxy-pressure profile. c) Solving the Volterra integral equation (Eq. (13)), we obtain the three-dimensional, Newtonian potential. d) The last step consists in projecting the gravitational potential of panel c) to find the two-dimensional potential.

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