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Data from: From peculiar morphologies to Hubble-type spirals: the relation between galaxy dynamics and morphology in star-forming galaxies at z ˜ 1.5

The University of Western Australia
Gillman, Steven ; Tiley, Alfred ; Swinbank, A. M. ; Harrison, C. M. ; Smail, Ian ; Dudzevǐciute, U. ; Sharples, Ray M. ; Cortese, Luca ; Obreschkow, Danail ; Bower, R. G. ; Theuns, Tom ; Cirasuolo, M. ; Fisher, David B. ; Glazebrook, Karl ; Ibar, Edo ; Mendel, J. T. ; Sweet, Sarah 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=https://research-repository.uwa.edu.au/en/datasets/8d3580ab-f436-4d87-97fd-5d108dea2805&rft.title=Data from: From peculiar morphologies to Hubble-type spirals: the relation between galaxy dynamics and morphology in star-forming galaxies at z ˜ 1.5&rft.identifier=8d3580ab-f436-4d87-97fd-5d108dea2805&rft.publisher=SAO/NASA Astrophysics Data System (ADS)&rft.description=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 Hα dynamics from KMOS with the high-resolution imaging to derive the relation between stellar mass (M*) and stellar specific angular momentum (j).We showthat high-redshift star-forming galaxies at z∼1.5 followa power-lawtrend in specific stellar angular momentum with stellarmass 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 scatterwithin the j-M plane and its correlationwith both the integrated dynamical properties of a galaxy (e.g. velocity dispersion, Toomre Qg, Hα star formation rate surface density-SFR) 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. 2019 The Author(s).&rft.creator=Gillman, Steven &rft.creator=Tiley, Alfred &rft.creator=Swinbank, A. M. &rft.creator=Harrison, C. M. &rft.creator=Smail, Ian &rft.creator=Dudzevǐciute, U. &rft.creator=Sharples, Ray M. &rft.creator=Cortese, Luca &rft.creator=Obreschkow, Danail &rft.creator=Bower, R. G. &rft.creator=Theuns, Tom &rft.creator=Cirasuolo, M. &rft.creator=Fisher, David B. &rft.creator=Glazebrook, Karl &rft.creator=Ibar, Edo &rft.creator=Mendel, J. T. &rft.creator=Sweet, Sarah M. &rft.date=2020&rft.relation=http://research-repository.uwa.edu.au/en/publications/b7ed75e9-c89d-4b91-8225-442e8e073806&rft_subject=galaxies: evolution&rft_subject=galaxies: high-redshift&rft_subject=galaxies: kinematics and dynamics&rft_subject=Astrophysics - Astrophysics of Galaxies&rft.type=dataset&rft.language=English Access the data
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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 Hα dynamics from KMOS with the high-resolution imaging to derive the relation between stellar mass (M*) and stellar specific angular momentum (j).We showthat high-redshift star-forming galaxies at z∼1.5 followa power-lawtrend in specific stellar angular momentum with stellarmass 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 scatterwithin the j-M plane and its correlationwith both the integrated dynamical properties of a galaxy (e.g. velocity dispersion, Toomre Qg, Hα star formation rate surface density-SFR) 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. 2019 The Author(s).

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Associated Persons
Steven Gillman (Creator); A. M. Swinbank (Creator); C. M. Harrison (Creator); Ian Smail (Creator); U. Dudzevǐciute (Creator); Ray M. Sharples (Creator); R. G. Bower (Creator); Tom Theuns (Creator); M. Cirasuolo (Creator); David B. Fisher (Creator); Karl Glazebrook (Creator); Edo Ibar (Creator); J. T. Mendel (Creator); Sarah M. Sweet (Creator)

Issued: 2020-02

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Subjects
Astrophysics - Astrophysics of Galaxies | galaxies: evolution | galaxies: high-redshift | galaxies: kinematics and dynamics |

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  • global : 8d3580ab-f436-4d87-97fd-5d108dea2805
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