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Angular momentum of z ∼ 1.5 galaxies and their local analogues with adaptive optics

Sweet, Sarah M; Fisher, Deanne B; Savorgnan, Giulia; Glazebrook, Karl; Obreschkow, Danail; Gillman, Steven; Tiley, Alfred L; Lagos, Claudia DP; Wang, Liang; Swinbank, A Mark; Bower, Richard; Sharples, Ray M

Angular momentum of z ∼ 1.5 galaxies and their local analogues with adaptive optics Thumbnail


Authors

Sarah M Sweet

Deanne B Fisher

Giulia Savorgnan

Karl Glazebrook

Danail Obreschkow

Steven Gillman

Alfred L Tiley

Claudia DP Lagos

Liang Wang

Richard Bower



Abstract

We present stellar specific angular momentum j* measurements of two z ∼ 1.5 galaxies in the KGES sample and 12 DYNAMO z ∼ 0.1 analogues of high-redshift galaxies. We combine natural seeing integral field spectroscopic data to trace line emission out to high multiples of effective radius re, with adaptive optics assisted Keck/OSIRIS observations to trace the rapid rise in rotation curve in the inner regions. Our spaxel-wise integration method gives results that are on average within measurement uncertainty of the traditional rotation curve model method. At z ∼ 0, combining GMOS and OSIRIS datasets improves the measurement uncertainty in j* from 13% (GMOS only) or 16% (OSIRIS only) to 10%. At z ∼ 1.5, systematics allow for at best 20% uncertainty on j*. DYNAMO analogues of high-z galaxies have low j* for their stellar mass M*, and low bulge-to-total light ratio β for their j*/M*. The high-z galaxy COSMOS 127977 has j*/M* consistent with normal local disk galaxies, while UDS 78317 is consistent with local analogues. However, our high-resolution OSIRIS data reveal that UDS 78317 may be a merging system. We report a relationship between distance to the β − j*/M* plane and the ratio of velocity dispersion to rotational velocity σ/vmax, where galaxies that deviate more from the plane are more dispersion-dominated due to turbulence. Much of the scatter in M* − j* that is not explained by variations in the bulge-to-total ratio or evolution with redshift may be driven by increased turbulence due to star formation, or by treating mergers as rotating disks.

Journal Article Type Article
Acceptance Date Mar 9, 2019
Online Publication Date Mar 14, 2019
Publication Date Jun 30, 2019
Deposit Date Mar 25, 2019
Publicly Available Date Mar 26, 2019
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Royal Astronomical Society
Peer Reviewed Peer Reviewed
Volume 485
Issue 4
Pages 5700-5714
DOI https://doi.org/10.1093/mnras/stz750
Public URL https://durham-repository.worktribe.com/output/1334726

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Copyright Statement
© 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.






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