Bezanson RVan Der Wel APacifici CNoeske KBarišić IBell E.FBrammer G.BCalhau JChauke PVan Dokkum PFranx MGallazzi AVan Houdt JLabbé IMaseda M.VMunos-Mateos J.CMuzzin AVan De Sande JSobral DStraatman CPO-FENG WU2022-11-112022-11-1120180004637Xhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85047201665&doi=10.3847%2f1538-4357%2faabc55&partnerID=40&md5=b727f069e6b16acae8facdf065da1badhttps://scholars.lib.ntu.edu.tw/handle/123456789/624930We present stellar rotation curves and velocity dispersion profiles for 104 quiescent galaxies at z = 0.6-1 from the Large Early Galaxy Astrophysics Census (LEGA-C) spectroscopic survey. Rotation is typically probed across 10-20 kpc, or to an average of 2.7Re. Combined with central stellar velocity dispersions (σ0) this provides the first determination of the dynamical state of a sample selected by a lack of star formation activity at large lookback time. The most massive galaxies (M∗ > 2 ×1011 Mo) generally show no or little rotation measured at 5 kpc ( in eight of ten cases), while ∼64% of less massive galaxies show significant rotation. This is reminiscent of local fast- and slow-rotating ellipticals and implies that low- and high-redshift quiescent galaxies have qualitatively similar dynamical structures. We compare distributions at z ∼ 0.8 and the present day by re-binning and smoothing the kinematic maps of 91 low-redshift quiescent galaxies from the Calar Alto Legacy Integral Field Area (CALIFA) survey and find evidence for a decrease in rotational support since z ∼ 1. This result is especially strong when galaxies are compared at fixed velocity dispersion; if velocity dispersion does not evolve for individual galaxies then the rotational velocity at 5 kpc was an average of 94 ±22% higher in z ∼ 0.8 quiescent galaxies than today. Considering that the number of quiescent galaxies grows with time and that new additions to the population descend from rotationally supported star-forming galaxies, our results imply that quiescent galaxies must lose angular momentum between z ∼ 1 and the present, presumably through dissipationless merging, and/or that the mechanism that transforms star-forming galaxies also reduces their rotational support. © 2018. The American Astronomical Society. All rights reserved.galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: high-redshift; galaxies: kinematics and dynamics; galaxies: structurejournal article10.3847/1538-4357/aabc552-s2.0-85047201665