From Peculiar Morphologies to Hubble–type Spirals: The relation between galaxy dynamics and morphology in star–forming galaxies at z ∼ 1.5
| dc.contributor.author | Ibar, Eduardo | |
| dc.date.accessioned | 2021-07-23T14:26:14Z | |
| dc.date.available | 2021-07-23T14:26:14Z | |
| dc.date.issued | 2020 | |
| dc.description.abstract | 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 HSTCANDELS 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* ∝ 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, 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. | en_ES |
| dc.identifier.doi | https://doi.org/10.1093/mnras/stz3576 | |
| dc.identifier.uri | http://repositoriobibliotecas.uv.cl/handle/uvscl/2152 | |
| dc.publisher | Royal Astronomical Society | en_ES |
| dc.source | Monthly Notices of the Royal Astronomical Society | en_ES |
| dc.subject | GALAXIES: KINEMATICS AND DYNAMICS | en_ES |
| dc.subject | GALAXIES: HIGH-REDSHIFT | en_ES |
| dc.subject | GALAXIES: EVOLUTION | en_ES |
| dc.title | From Peculiar Morphologies to Hubble–type Spirals: The relation between galaxy dynamics and morphology in star–forming galaxies at z ∼ 1.5 | en_ES |
| dc.type | Articulo | en_ES |
| uv.catalogador | RCR DIBRA | en_ES |