The kinematics of massive quiescent galaxies at \$1.4 {\textless} z {\textless} 2.1\$: dark matter fractions, IMF variation, and the relation to local early-type galaxies. Mendel, J. T., Beifiori, A., Saglia, R., Bender, R., Brammer, G., Chan, J., Forster Schreiber, N., Fossati, M., Galametz, A., Momcheva, I., Nelson, E., Wilman, D., & Wuyts, S. arXiv e-prints, 2006:arXiv:2006.13949, June, 2020. ![The kinematics of massive quiescent galaxies at \$1.4 {\textless} z {\textless} 2.1\$: dark matter fractions, IMF variation, and the relation to local early-type galaxies [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We study the dynamical properties of massive quiescent galaxies at \$1.4 {\textless} z {\textless} 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 KMOS on the ESO VLT. We use these data to show that the typical dynamical-to-stellar mass ratio has increased by \${\textbackslash}sim\$0.2 dex from \$z = 2\$ to the present day, and 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_{\textbackslash}mathrm\{DM\}\$. Comparing our high-redshift sample to their likely descendants at low-redshift, we find that \$f_{\textbackslash}mathrm\{DM\}\$ has increased by a factor of more than 4 since \$z {\textbackslash}approx 1.8\$, from \$f_{\textbackslash}mathrm\{DM\}\$ = \$6.6{\textbackslash}pm1.0\$% to \${\textbackslash}sim\$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 \${\textbackslash}alpha\$, 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 \${\textbackslash}alpha\$ reported among quiescent galaxies at low-redshift is already in place at \$z = 2\$, and 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.
@article{mendel_kinematics_2020,
title = {The kinematics of massive quiescent galaxies at \$1.4 {\textless} z {\textless} 2.1\$: dark matter fractions, {IMF} variation, and the relation to local early-type galaxies},
volume = {2006},
shorttitle = {The kinematics of massive quiescent galaxies at \$1.4 {\textless} z {\textless} 2.1\$},
url = {http://adsabs.harvard.edu/abs/2020arXiv200613949M},
abstract = {We study the dynamical properties of massive quiescent galaxies at \$1.4
{\textless} z {\textless} 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 KMOS on the ESO VLT. We use
these data to show that the typical dynamical-to-stellar mass ratio has
increased by \${\textbackslash}sim\$0.2 dex from \$z = 2\$ to the present day, and
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\_{\textbackslash}mathrm\{DM\}\$. Comparing
our high-redshift sample to their likely descendants at low-redshift, we
find that \$f\_{\textbackslash}mathrm\{DM\}\$ has increased by a factor of more than 4 since
\$z {\textbackslash}approx 1.8\$, from \$f\_{\textbackslash}mathrm\{DM\}\$ = \$6.6{\textbackslash}pm1.0\$\% to \${\textbackslash}sim\$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 \${\textbackslash}alpha\$, 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 \${\textbackslash}alpha\$ reported
among quiescent galaxies at low-redshift is already in place at \$z = 2\$,
and 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.},
urldate = {2020-06-29},
journal = {arXiv e-prints},
author = {Mendel, J. Trevor and Beifiori, Alessandra and Saglia, Roberto and Bender, Ralf and Brammer, Gabe and Chan, Jeffrey and Forster Schreiber, Natascha and Fossati, Matteo and Galametz, Audrey and Momcheva, Iva and Nelson, Erica and Wilman, Dave and Wuyts, Stijn},
month = jun,
year = {2020},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {arXiv:2006.13949},
}
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T.","Beifiori, A.","Saglia, R.","Bender, R.","Brammer, G.","Chan, J.","Forster Schreiber, N.","Fossati, M.","Galametz, A.","Momcheva, I.","Nelson, E.","Wilman, D.","Wuyts, S."],"bibdata":{"bibtype":"article","type":"article","title":"The kinematics of massive quiescent galaxies at \\$1.4 {\\textless} z {\\textless} 2.1\\$: dark matter fractions, IMF variation, and the relation to local early-type galaxies","volume":"2006","shorttitle":"The kinematics of massive quiescent galaxies at \\$1.4 {\\textless} z {\\textless} 2.1\\$","url":"http://adsabs.harvard.edu/abs/2020arXiv200613949M","abstract":"We study the dynamical properties of massive quiescent galaxies at \\$1.4 {\\textless} z {\\textless} 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 KMOS on the ESO VLT. We use these data to show that the typical dynamical-to-stellar mass ratio has increased by \\${\\textbackslash}sim\\$0.2 dex from \\$z = 2\\$ to the present day, and 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_{\\textbackslash}mathrm\\{DM\\}\\$. Comparing our high-redshift sample to their likely descendants at low-redshift, we find that \\$f_{\\textbackslash}mathrm\\{DM\\}\\$ has increased by a factor of more than 4 since \\$z {\\textbackslash}approx 1.8\\$, from \\$f_{\\textbackslash}mathrm\\{DM\\}\\$ = \\$6.6{\\textbackslash}pm1.0\\$% to \\${\\textbackslash}sim\\$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 \\${\\textbackslash}alpha\\$, 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 \\${\\textbackslash}alpha\\$ reported among quiescent galaxies at low-redshift is already in place at \\$z = 2\\$, and 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.","urldate":"2020-06-29","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Mendel"],"firstnames":["J.","Trevor"],"suffixes":[]},{"propositions":[],"lastnames":["Beifiori"],"firstnames":["Alessandra"],"suffixes":[]},{"propositions":[],"lastnames":["Saglia"],"firstnames":["Roberto"],"suffixes":[]},{"propositions":[],"lastnames":["Bender"],"firstnames":["Ralf"],"suffixes":[]},{"propositions":[],"lastnames":["Brammer"],"firstnames":["Gabe"],"suffixes":[]},{"propositions":[],"lastnames":["Chan"],"firstnames":["Jeffrey"],"suffixes":[]},{"propositions":[],"lastnames":["Forster","Schreiber"],"firstnames":["Natascha"],"suffixes":[]},{"propositions":[],"lastnames":["Fossati"],"firstnames":["Matteo"],"suffixes":[]},{"propositions":[],"lastnames":["Galametz"],"firstnames":["Audrey"],"suffixes":[]},{"propositions":[],"lastnames":["Momcheva"],"firstnames":["Iva"],"suffixes":[]},{"propositions":[],"lastnames":["Nelson"],"firstnames":["Erica"],"suffixes":[]},{"propositions":[],"lastnames":["Wilman"],"firstnames":["Dave"],"suffixes":[]},{"propositions":[],"lastnames":["Wuyts"],"firstnames":["Stijn"],"suffixes":[]}],"month":"June","year":"2020","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:2006.13949","bibtex":"@article{mendel_kinematics_2020,\n\ttitle = {The kinematics of massive quiescent galaxies at \\$1.4 {\\textless} z {\\textless} 2.1\\$: dark matter fractions, {IMF} variation, and the relation to local early-type galaxies},\n\tvolume = {2006},\n\tshorttitle = {The kinematics of massive quiescent galaxies at \\$1.4 {\\textless} z {\\textless} 2.1\\$},\n\turl = {http://adsabs.harvard.edu/abs/2020arXiv200613949M},\n\tabstract = {We study the dynamical properties of massive quiescent galaxies at \\$1.4 \n{\\textless} z {\\textless} 2.1\\$ using deep Hubble Space Telescope WFC3/F160W imaging\nand a combination of literature stellar velocity dispersion measurements\nand new near-infrared spectra obtained using KMOS on the ESO VLT. We use\nthese data to show that the typical dynamical-to-stellar mass ratio has\nincreased by \\${\\textbackslash}sim\\$0.2 dex from \\$z = 2\\$ to the present day, and\ninvestigate this evolution in the context of possible changes in the\nstellar initial mass function (IMF) and/or fraction of dark matter\ncontained within the galaxy effective radius, \\$f\\_{\\textbackslash}mathrm\\{DM\\}\\$. Comparing\nour high-redshift sample to their likely descendants at low-redshift, we\nfind that \\$f\\_{\\textbackslash}mathrm\\{DM\\}\\$ has increased by a factor of more than 4 since\n\\$z {\\textbackslash}approx 1.8\\$, from \\$f\\_{\\textbackslash}mathrm\\{DM\\}\\$ = \\$6.6{\\textbackslash}pm1.0\\$\\% to \\${\\textbackslash}sim\\$24\\%. The\nobserved increase appears robust to changes in the methods used to\nestimate dynamical masses or match progenitors and descendants. We\nquantify possible variation of the stellar IMF through the offset\nparameter \\${\\textbackslash}alpha\\$, defined as the ratio of dynamical mass in stars to\nthe stellar mass estimated using a Chabrier IMF. We demonstrate that the\ncorrelation between stellar velocity dispersion and \\${\\textbackslash}alpha\\$ reported\namong quiescent galaxies at low-redshift is already in place at \\$z = 2\\$,\nand argue that subsequent evolution through (mostly minor) merging\nshould act to preserve this relation while contributing significantly to\ngalaxies overall growth in size and stellar mass.},\n\turldate = {2020-06-29},\n\tjournal = {arXiv e-prints},\n\tauthor = {Mendel, J. 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