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Data from : Angular momentum of z ˜ 1.5 galaxies and their local analogues with adaptive optics

The University of Western Australia
Sweet, Sarah M. ; Fisher, Deanne B. ; Savorgnan, Giulia ; Glazebrook, Karl ; Obreschkow, Danail ; Gillman, Steven ; Tiley, Alfred ; Lagos Urbina, Claudia ; Wang, Liang ; Mark Swinbank, A. ; Bower, Richard G. ; Sharples, Ray M.
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ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Adc&rfr_id=info%3Asid%2FANDS&rft_id=info:doi10.1093/mnras/stz750&rft.title=Data from : Angular momentum of z ˜ 1.5 galaxies and their local analogues with adaptive optics&rft.identifier=10.1093/mnras/stz750&rft.publisher=SAO/NASA Astrophysics Data System (ADS)&rft.description=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 data sets improves the measurement uncertainty in j* from 13 per cent (GMOS only) or 16 per cent (OSIRIS only) to 10 per cent. At z ˜ 1.5, systematics allow for at best 20 per cent 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 disc 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 discs.&rft.creator=Sweet, Sarah M. &rft.creator=Fisher, Deanne B. &rft.creator=Savorgnan, Giulia &rft.creator=Glazebrook, Karl &rft.creator=Obreschkow, Danail &rft.creator=Gillman, Steven &rft.creator=Tiley, Alfred &rft.creator=Lagos Urbina, Claudia &rft.creator=Wang, Liang &rft.creator=Mark Swinbank, A. &rft.creator=Bower, Richard G. &rft.creator=Sharples, Ray M. &rft.date=2019&rft.relation=http://research-repository.uwa.edu.au/en/publications/aadf9a3c-e821-496d-b41f-6e5817f2dcc4&rft.type=dataset&rft.language=English Access the data
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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 data sets improves the measurement uncertainty in j* from 13 per cent (GMOS only) or 16 per cent (OSIRIS only) to 10 per cent. At z ˜ 1.5, systematics allow for at best 20 per cent 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 disc 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 discs.

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External Organisations
Swinburne University of Technology; ARC Centre of Excellence for All-sky Astrophysics; ARC Centre of Excellence for Astrophysics in Three Dimensions (ASTRO3D); Durham University; Max Planck Institute for Radio Astronomy
Associated Persons
Sarah M. Sweet (Creator); Deanne B. Fisher (Creator); Giulia Savorgnan (Creator); Karl Glazebrook (Creator); Steven Gillman (Creator); A. Mark Swinbank (Creator); Richard G. Bower (Creator); Ray M. Sharples (Creator)

Created: 2019-03-14 to 2019-03-14

Issued: 2019-06

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