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We characterized the kinematics, morphology, and stellar population (SP)properties of a sample of massive compact quiescent galaxies (MCGs, $10\lesssim \log M_\star$/$M_\odot \lesssim 11$ and $r_{\rm e} \sim 1-3 $kpc) inthe MaNGA Survey, with the goal of constraining their formation, assemblyhistory and assessing their relation with non-compact quiescent galaxies. Wecompared their properties with those of a control sample of median-sizedquiescent galaxies ($r_{\rm e} \sim 4-8 $kpc) with similar effective velocitydispersions. MCGs have elevated rotational support, as evidenced by a stronganti-correlation between the Gauss-Hermite moment $h_3$ and $V/\sigma$. Incontrast, 30$\%$ of control sample galaxies (CSGs) are slow rotators, andfast-rotating CSGs generally show a weak $h_3-V/\sigma$ anti-correlation. MCGsand CSGs have similar ages, but MCGs are more metal-rich and $\alpha$-enhanced.Both MCGs and CSGs have shallow negative metallicity gradients and flat[$\alpha$/Fe] gradients. On average, MCGs and CSGs have flat age gradients, butCSGs have a significantly larger dispersion of gradient values. The kinematicsand SP properties of MCGs suggest that they experienced highly-dissipativegas-rich events, such as mergers, followed by an intense, short, and centrallyconcentrated burst of star formation, between 4 to 10 Gyr ago ($z\sim0.4-2$),and had a quiet accretion history since then. This sequence of events might beanalogous to, although less extreme than, the compaction events which formedcompact quiescent galaxies at $z \sim 2$. The small sizes of MCGs, and the highefficiency and short duration of their last star formation episode suggest thatthey are descendants of compact post-starburst galaxies.

The Puzzling Origin of Massive Compact Galaxies in MaNGA