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The kinematics of massive quiescent galaxies at 1.4 < z < 2.1: dark matter fractions, IMF variation, and the relation to local early-type galaxies

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Mendel,  Trevor J.
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Beifiori,  Alessandra
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Saglia,  Roberto P.
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Bender,  Ralf
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Förster Schreiber,  N. M.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Fossati,  Matteo
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Wilman,  Dave J.
Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Wuyts,  Stijn
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Citation

Mendel, T. J., Beifiori, A., Saglia, R. P., Bender, R., Brammer, G. B., Chan, J., et al. (2020). The kinematics of massive quiescent galaxies at 1.4 < z < 2.1: dark matter fractions, IMF variation, and the relation to local early-type galaxies. The Astrophysical Journal, 899(1): 87. doi:10.3847/1538-4357/ab9ffc.


Cite as: http://hdl.handle.net/21.11116/0000-0007-715C-3
Abstract
We study the dynamical properties of massive quiescent galaxies at 1.4 < z < 2.1 using deep Hubble Space Telescope WFC3/F160W imaging and a combination of literature stellar velocity dispersion measurements and new near-infrared spectra obtained using the K-band Multi Object Spectrograph (KMOS) on the ESO Very Large Telescope. We use these data to show that the typical dynamical-to-stellar mass ratio has increased by ~0.2 dex from z = 2 to the present day, and we investigate this evolution in the context of possible changes in the stellar initial mass function (IMF) and/or fraction of dark matter contained within the galaxy effective radius, f DM[<r e]. Comparing our high-redshift sample to their likely descendants at low redshift, we find that f DM[<r e] has increased by a factor of more than 4 since z ≈ 1.8, from f DM[<r e] = 6.6% ± 1.0% to ~24%. The observed increase appears robust to changes in the methods used to estimate dynamical masses or match progenitors and descendants. We quantify possible variation of the stellar IMF through the offset parameter α, defined as the ratio of dynamical mass in stars to the stellar mass estimated using a Chabrier IMF. We demonstrate that the correlation between stellar velocity dispersion and α reported among quiescent galaxies at low redshift is already in place at z = 2, and we argue that subsequent evolution through (mostly minor) merging should act to preserve this relation while contributing significantly to galaxies' overall growth in size and stellar mass.