MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3* * The spectra presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.

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dc.contributor.authorForrest, Ben
dc.contributor.authorWilson, Gillian
dc.contributor.authorMuzzin, Adam
dc.contributor.authorMarchesini, Danilo
dc.contributor.authorCooper, M.C.
dc.contributor.authorCemile Marsan, Z.
dc.contributor.authorAnnunziatella, Marianna
dc.contributor.authorMcConachie, Ian
dc.contributor.authorZaidi, Kumail
dc.contributor.authorGomez, Percy
dc.contributor.authorUrbano Stawinski, Stephanie M.
dc.contributor.authorChang, Wenjun
dc.contributor.authorLucia, Gabriella de
dc.contributor.authorBarbera, Francesco La
dc.contributor.authorLubin, Lori
dc.contributor.authorNantais, Julie
dc.contributor.authorPeña, Theodore
dc.contributor.authorSaracco, Paolo
dc.contributor.authorSurace, Jason
dc.contributor.authorStefanon, Mauro
dc.date.accessioned2023-07-04T15:04:10Z
dc.date.available2023-07-04T15:04:10Z
dc.date.issued2022-10-01
dc.descriptionIndexación: Scopus.es
dc.description.abstractIn this work, we publish stellar velocity dispersions, sizes, and dynamical masses for eight ultramassive galaxies (UMGs; log ( M * / M ⊙ ) > 11), z ≳ 3) from the Massive Ancient Galaxies At z > 3 NEar-infrared (MAGAZ3NE) Survey, more than doubling the number of such galaxies with velocity dispersion measurements at this epoch. Using the deep Keck/MOSFIRE and Keck/NIRES spectroscopy of these objects in the H and K bandpasses, we obtain large velocity dispersions of ∼400 km s−1 for most of the objects, which are some of the highest stellar velocity dispersions measured and ∼40% larger than those measured for galaxies of similar mass at z ∼ 1.7. The sizes of these objects are also smaller by a factor of 1.5-3 compared to this same z ∼ 1.7 sample. We combine these large velocity dispersions and small sizes to obtain dynamical masses. The dynamical masses are similar to the stellar masses of these galaxies, consistent with a Chabrier initial mass function (IMF). Considered alongside previous studies of massive quiescent galaxies across 0.2 < z < 4.0, there is evidence for an evolution in the relation between the dynamical mass-stellar mass ratio and velocity dispersion as a function of redshift. This implies an IMF with fewer low-mass stars (e.g., Chabrier IMF) for massive quiescent galaxies at higher redshifts in conflict with the bottom-heavy IMF (e.g., Salpeter IMF) found in their likely z ∼ 0 descendants, though a number of alternative explanations such as a different dynamical structure or significant rotation are not ruled out. Similar to data at lower redshifts, we see evidence for an increase of IMF normalization with velocity dispersion, though the z ≳ 3 trend is steeper than that for z ∼ 0.2 early-type galaxies and offset to lower dynamical-to-stellar mass ratios. © 2022. The Author(s). Published by the American Astronomical Society.es
dc.description.urihttps://iopscience-iop-org.recursosbiblioteca.unab.cl/article/10.3847/1538-4357/ac8747
dc.identifier.citationAstrophysical Journal, Volume 938, Issue 2, 1 October 2022, Article number 109es
dc.identifier.doi10.3847/1538-4357/ac8747
dc.identifier.issn0004-637X
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/51350
dc.language.isoenes
dc.publisherInstitute of Physicses
dc.rights.licenseAttribution 4.0 International (CC BY 4.0)
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.subjectStar Formationes
dc.subjectGalaxieses
dc.subjectGalactic Evolutiones
dc.titleMAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3* * The spectra presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.es
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