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Fig. 10
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RHI/R* vs. MHI/M* in the remnant galaxies at z = 0 for our sample, colored by ⟨θr, v⟩ (left) and specific star formation rate (right). In both panels, two galaxies marked by stars exhibit RR galaxies with high values of MHI/M* and RHI/R*, yet their star formation appears to be quenched.
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