Understanding the physical growth of galaxies and their components: a local perspective

Rebecca Lange

    Research output: ThesisDoctoral Thesis

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    Abstract

    [Truncated] At the fundamental level a galaxy can be described by three parameters: its mass M⋆,energy E (which relates to its size), and angular momentum J. In this thesis I study all three parameters via the mass–half-light radius and the mass–specific angular momentumrelations. The over-riding objective is to provide robust local benchmark relations which can be used to compare to simulations and high redshift observational data, to study the formation and evolution of galaxies and their components. Throughout this work I use data from the Galaxy And Mass Assembly (GAMA) survey, and I fit galaxy and component light profiles using the GALFIT3 structural analysis package.

    In Chapter 2 I study the stellar mass – half-light radius (M⋆−Re) relations for ‘early’and ‘late’-type galaxies as defined by either their colour, shape or morphology. The sample spans 10 wavebands from u to Ks in the redshift range of 0.01<z<0.1. The analysis shows that the choice of early- and late-type division is not critical if the fitting algorithm is robust to small changes and outliers are treated carefully. Furthermore the analysis confirms the wavelength dependence of the galaxy size with both disk and elliptical galaxies showing a similar decrease in Re of ∼ 13% from g- to Ks-band at 1010M⊙. This is less thanpreviously reported by e.g. Kelvin et al. (2012) and Vulcani et al. (2014) and we believe due to the significant improvement in imaging depth and quality.

    Original languageEnglish
    QualificationDoctor of Philosophy
    Awarding Institution
    • The University of Western Australia
    Award date18 Jul 2016
    Publication statusUnpublished - 2016

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    galaxies
    radii
    theses
    disk galaxies
    elliptical galaxies
    stellar mass
    structural analysis
    division
    angular momentum
    assembly
    color
    profiles
    wavelengths
    simulation
    energy

    Cite this

    @phdthesis{4741a622360348ce9673fa4f59f959d6,
    title = "Understanding the physical growth of galaxies and their components: a local perspective",
    abstract = "[Truncated] At the fundamental level a galaxy can be described by three parameters: its mass M⋆,energy E (which relates to its size), and angular momentum J. In this thesis I study all three parameters via the mass–half-light radius and the mass–specific angular momentumrelations. The over-riding objective is to provide robust local benchmark relations which can be used to compare to simulations and high redshift observational data, to study the formation and evolution of galaxies and their components. Throughout this work I use data from the Galaxy And Mass Assembly (GAMA) survey, and I fit galaxy and component light profiles using the GALFIT3 structural analysis package.In Chapter 2 I study the stellar mass – half-light radius (M⋆−Re) relations for ‘early’and ‘late’-type galaxies as defined by either their colour, shape or morphology. The sample spans 10 wavebands from u to Ks in the redshift range of 0.01e of ∼ 13{\%} from g- to Ks-band at 1010M⊙. This is less thanpreviously reported by e.g. Kelvin et al. (2012) and Vulcani et al. (2014) and we believe due to the significant improvement in imaging depth and quality.",
    keywords = "Galaxy structure, galaxy mass-size relation, galaxy mass-angular momentum relation, Galaxy morphology, Galaxy discs and bulges",
    author = "Rebecca Lange",
    year = "2016",
    language = "English",
    school = "The University of Western Australia",

    }

    Lange, R 2016, 'Understanding the physical growth of galaxies and their components: a local perspective', Doctor of Philosophy, The University of Western Australia.

    Understanding the physical growth of galaxies and their components: a local perspective. / Lange, Rebecca.

    2016.

    Research output: ThesisDoctoral Thesis

    TY - THES

    T1 - Understanding the physical growth of galaxies and their components: a local perspective

    AU - Lange, Rebecca

    PY - 2016

    Y1 - 2016

    N2 - [Truncated] At the fundamental level a galaxy can be described by three parameters: its mass M⋆,energy E (which relates to its size), and angular momentum J. In this thesis I study all three parameters via the mass–half-light radius and the mass–specific angular momentumrelations. The over-riding objective is to provide robust local benchmark relations which can be used to compare to simulations and high redshift observational data, to study the formation and evolution of galaxies and their components. Throughout this work I use data from the Galaxy And Mass Assembly (GAMA) survey, and I fit galaxy and component light profiles using the GALFIT3 structural analysis package.In Chapter 2 I study the stellar mass – half-light radius (M⋆−Re) relations for ‘early’and ‘late’-type galaxies as defined by either their colour, shape or morphology. The sample spans 10 wavebands from u to Ks in the redshift range of 0.01e of ∼ 13% from g- to Ks-band at 1010M⊙. This is less thanpreviously reported by e.g. Kelvin et al. (2012) and Vulcani et al. (2014) and we believe due to the significant improvement in imaging depth and quality.

    AB - [Truncated] At the fundamental level a galaxy can be described by three parameters: its mass M⋆,energy E (which relates to its size), and angular momentum J. In this thesis I study all three parameters via the mass–half-light radius and the mass–specific angular momentumrelations. The over-riding objective is to provide robust local benchmark relations which can be used to compare to simulations and high redshift observational data, to study the formation and evolution of galaxies and their components. Throughout this work I use data from the Galaxy And Mass Assembly (GAMA) survey, and I fit galaxy and component light profiles using the GALFIT3 structural analysis package.In Chapter 2 I study the stellar mass – half-light radius (M⋆−Re) relations for ‘early’and ‘late’-type galaxies as defined by either their colour, shape or morphology. The sample spans 10 wavebands from u to Ks in the redshift range of 0.01e of ∼ 13% from g- to Ks-band at 1010M⊙. This is less thanpreviously reported by e.g. Kelvin et al. (2012) and Vulcani et al. (2014) and we believe due to the significant improvement in imaging depth and quality.

    KW - Galaxy structure

    KW - galaxy mass-size relation

    KW - galaxy mass-angular momentum relation

    KW - Galaxy morphology

    KW - Galaxy discs and bulges

    M3 - Doctoral Thesis

    ER -