Angular momentum of z ∼ 1.5 galaxies and their local analogues with adaptive optics. Issue 4 (14th March 2019)

• Record Type: Journal Article
• Authors: Sweet, Sarah M; Fisher, Deanne B; Savorgnan, Giulia; Glazebrook, Karl; Obreschkow, Danail; Gillman, Steven; Tiley, Alfred L; Lagos, Claudia D P; Wang, Liang; Swinbank, A Mark; Bower, Richard; Sharples, Ray M
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 485:Issue 4(2019)
• Page Start: 5700
• Page End: 5714
• Publication Date: 2019-03-14
• Subjects: galaxies: bulges -- galaxies: evolution -- galaxies: fundamental parameters -- galaxies: high-redshift -- galaxies: kinematics and dynamics -- galaxies: spiral; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz750
• Languages: English
• ISSNs: 0035-8711

Abstract

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 r e, 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/ v max, 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.