| Autor: |
Gillman, S, Tiley, A L, Swinbank, A M, Harrison, C M, Smail, Ian, Dudzevičiūtė, U, Sharples, R M, Cortese, L, Obreschkow, D, Bower, R G, Theuns, T, Cirasuolo, M, Fisher, D B, Glazebrook, K, Ibar, Edo, Mendel, J Trevor, Sweet, Sarah M |
| Předmět: |
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| Zdroj: |
Monthly Notices of the Royal Astronomical Society; Feb2020, Vol. 492 Issue 1, p1492-1512, 21p |
| Abstrakt: |
We present an analysis of the gas dynamics of star-forming galaxies at z ∼ 1.5 using data from the KMOS Galaxy Evolution Survey. We quantify the morphology of the galaxies using HST candels imaging parametrically and non-parametrically. We combine the H α 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 * ∝ M |$_*^{0.53\, \pm \, 0.10}$|. 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, H α star formation rate surface density ΣSFR) and its parametrized 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 interstellar medium. [ABSTRACT FROM AUTHOR] |
| Databáze: |
Complementary Index |
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