From peculiar morphologies to Hubble-type spirals: the relation between galaxy dynamics and morphology in star-forming galaxies at z ∼ 1.5
Gillman, S.; Tiley, A.L.; Swinbank, A.M.; Harrison, C.M.; Smail, I.; Dudzevičiūtė, U; Sharples, R.M.; Cortese, L.; Obreschkow, D.; Bower, R.G.; Theuns, T.; Cirasuolo, M.; Fisher, D.B.; Glazebrook, K.; Ibar, E.; Mendel, J.T.; Sweet, S.M.
Professor Mark Swinbank email@example.com
Professor Ian Smail firstname.lastname@example.org
Ms Ugne Dudzeviciute email@example.com
PGR Student Doctor of Philosophy
Professor Ray Sharples firstname.lastname@example.org
Professor Tom Theuns email@example.com
We present an analysis of the gas dynamics of star–forming galaxies at z ∼ 1.5 using data from the KMOS Galaxy Evolution Survey (KGES). We quantify the morphology of the galaxies using HSTCANDELS imaging parametrically and non-parametrically. We combine the Hα dynamics from KMOS with the high–resolution imaging to derive the relation between stellar mass (M*) and stellar specific angular momentum (j*). We show that high–redshift star–forming galaxies at z ∼ 1.5 follow a power-law trend in specific stellar angular momentum with stellar mass similar to that of local late–type galaxies of the form j* ∝ M0.53±0.10∗. The highest specific angular momentum galaxies are mostly disc–like, although generally, both peculiar morphologies and disc-like systems are found across the sequence of specific angular momentum at a fixed stellar mass. We explore the scatter within the j* – M* plane and its correlation with both the integrated dynamical properties of a galaxy (e.g. velocity dispersion, Toomre Qg, Hα star formation rate surface density ΣSFR) and its parameterised rest-frame UV / optical morphology (e.g. Sérsic index, bulge to total ratio, Clumpiness, Asymmetry and Concentration). We establish that the position in the j* – M* plane is strongly correlated with the star-formation surface density and the Clumpiness of the stellar light distribution. Galaxies with peculiar rest-frame UV / optical morphologies have comparable specific angular momentum to disc – dominated galaxies of the same stellar mass, but are clumpier and have higher star-formation rate surface densities. We propose that the peculiar morphologies in high–redshift systems are driven by higher star formation rate surface densities and higher gas fractions leading to a more clumpy inter-stellar medium.
Gillman, S., Tiley, A., Swinbank, A., Harrison, C., Smail, I., Dudzevičiūtė, U., …Sweet, S. (2020). From peculiar morphologies to Hubble-type spirals: the relation between galaxy dynamics and morphology in star-forming galaxies at z ∼ 1.5. Monthly Notices of the Royal Astronomical Society, 492(1), 1492-1512. https://doi.org/10.1093/mnras/stz3576
|Journal Article Type||Article|
|Acceptance Date||Dec 18, 2019|
|Online Publication Date||Dec 23, 2019|
|Publication Date||Feb 28, 2020|
|Deposit Date||Dec 12, 2019|
|Publicly Available Date||Jan 3, 2020|
|Journal||Monthly Notices of the Royal Astronomical Society|
|Publisher||Royal Astronomical Society|
|Peer Reviewed||Peer Reviewed|
Accepted Journal Article
This article has been accepted for publication in the Monthly notices of the Royal Astronomical Society ©: 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Published Journal Article
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