Fig. 8.
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Dynamical against stellar masses assuming a Chabrier (2003) IMF (red squares) and a σv-dependent IMF from Treu et al. (2010) (blue circles) for the distant quiescent galaxies in our sample. The dashed line indicates the one-to-one ratio of dynamical vs stellar mass. Light points indicate galaxies for which only lower limits to the rotational velocity could be obtained.
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