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Fig. 5


Two renditions of the potential for dwarfs. Left: Mstars / LKs fixed. Right: Mstars / LKs variable. Individualized mass-to-light ratios for the plot on the right were estimated from the amount by which the central surface brightness of the sech component deviated from the mean for a given line width under the condition that the galaxies are virialized (see Fig. 6). In both panels, dwarf irregulars (dIs) are marked with open circles, and blue compact dwarfs (BCDs) are flagged by solid circles. No matter how the mass-to-light ratios are computed, BCDs and dIs populate the diagrams in the same way.

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