How to bend galaxy disc profiles

The role of halo spin

J. Herpich, G. S. Stinson, A. A. Dutton, H. W. Rix, M. Martig, R. Roskar, Andrea Maccio, T. R. Quinn, J. Wadsley

    Research output: Contribution to journalArticle

    Abstract

    The radial density profiles of stellar galaxy discs can be well approximated as an exponential. Compared to this canonical form, however, the profiles in the majority of disc galaxies show downward or upward breaks at large radii. Currently, there is no coherent explanation in a galaxy formation context of the radial profile per se, along with the two types of profile breaks. Using a set of controlled hydrodynamic simulations of disc galaxy formation, we find a correlation between the host halo's initial angular momentum and the resulting radial profile of the stellar disc: galaxies that live in haloes with a low spin parameter λ≲0.03 show an up-bending break in their disc density profiles, while galaxies in haloes of higher angular momentum show a down-bending break. We find that the case of pure exponential profiles (λ≈0.035) coincides with the peak of the spin parameter distribution from cosmological simulations. Our simulations not only imply an explanation of the observed behaviours, but also suggest that the physical origin of this effect is related to the amount of radial redistribution of stellar mass, which is anticorrelated with λ.

    Original languageEnglish (US)
    Pages (from-to)L99-L103
    JournalMonthly Notices of the Royal Astronomical Society: Letters
    Volume448
    Issue number1
    DOIs
    StatePublished - Jan 1 2015

    Fingerprint

    disk galaxies
    halos
    angular momentum
    profiles
    simulation
    galactic evolution
    hydrodynamics
    canonical forms
    stellar mass
    galaxies
    parameter
    radii

    Keywords

    • Galaxies: spiral
    • Galaxies: structure
    • Hydrodynamics
    • Methods: numerical

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Cite this

    Herpich, J., Stinson, G. S., Dutton, A. A., Rix, H. W., Martig, M., Roskar, R., ... Wadsley, J. (2015). How to bend galaxy disc profiles: The role of halo spin. Monthly Notices of the Royal Astronomical Society: Letters, 448(1), L99-L103. https://doi.org/10.1093/mnrasl/slv006

    How to bend galaxy disc profiles : The role of halo spin. / Herpich, J.; Stinson, G. S.; Dutton, A. A.; Rix, H. W.; Martig, M.; Roskar, R.; Maccio, Andrea; Quinn, T. R.; Wadsley, J.

    In: Monthly Notices of the Royal Astronomical Society: Letters, Vol. 448, No. 1, 01.01.2015, p. L99-L103.

    Research output: Contribution to journalArticle

    Herpich, J, Stinson, GS, Dutton, AA, Rix, HW, Martig, M, Roskar, R, Maccio, A, Quinn, TR & Wadsley, J 2015, 'How to bend galaxy disc profiles: The role of halo spin', Monthly Notices of the Royal Astronomical Society: Letters, vol. 448, no. 1, pp. L99-L103. https://doi.org/10.1093/mnrasl/slv006
    Herpich J, Stinson GS, Dutton AA, Rix HW, Martig M, Roskar R et al. How to bend galaxy disc profiles: The role of halo spin. Monthly Notices of the Royal Astronomical Society: Letters. 2015 Jan 1;448(1):L99-L103. https://doi.org/10.1093/mnrasl/slv006
    Herpich, J. ; Stinson, G. S. ; Dutton, A. A. ; Rix, H. W. ; Martig, M. ; Roskar, R. ; Maccio, Andrea ; Quinn, T. R. ; Wadsley, J. / How to bend galaxy disc profiles : The role of halo spin. In: Monthly Notices of the Royal Astronomical Society: Letters. 2015 ; Vol. 448, No. 1. pp. L99-L103.
    @article{23d1184b0c8349c38cae06df53c493b6,
    title = "How to bend galaxy disc profiles: The role of halo spin",
    abstract = "The radial density profiles of stellar galaxy discs can be well approximated as an exponential. Compared to this canonical form, however, the profiles in the majority of disc galaxies show downward or upward breaks at large radii. Currently, there is no coherent explanation in a galaxy formation context of the radial profile per se, along with the two types of profile breaks. Using a set of controlled hydrodynamic simulations of disc galaxy formation, we find a correlation between the host halo's initial angular momentum and the resulting radial profile of the stellar disc: galaxies that live in haloes with a low spin parameter λ≲0.03 show an up-bending break in their disc density profiles, while galaxies in haloes of higher angular momentum show a down-bending break. We find that the case of pure exponential profiles (λ≈0.035) coincides with the peak of the spin parameter distribution from cosmological simulations. Our simulations not only imply an explanation of the observed behaviours, but also suggest that the physical origin of this effect is related to the amount of radial redistribution of stellar mass, which is anticorrelated with λ.",
    keywords = "Galaxies: spiral, Galaxies: structure, Hydrodynamics, Methods: numerical",
    author = "J. Herpich and Stinson, {G. S.} and Dutton, {A. A.} and Rix, {H. W.} and M. Martig and R. Roskar and Andrea Maccio and Quinn, {T. R.} and J. Wadsley",
    year = "2015",
    month = "1",
    day = "1",
    doi = "10.1093/mnrasl/slv006",
    language = "English (US)",
    volume = "448",
    pages = "L99--L103",
    journal = "Monthly Notices of the Royal Astronomical Society: Letters",
    issn = "1745-3925",
    publisher = "Oxford University Press",
    number = "1",

    }

    TY - JOUR

    T1 - How to bend galaxy disc profiles

    T2 - The role of halo spin

    AU - Herpich, J.

    AU - Stinson, G. S.

    AU - Dutton, A. A.

    AU - Rix, H. W.

    AU - Martig, M.

    AU - Roskar, R.

    AU - Maccio, Andrea

    AU - Quinn, T. R.

    AU - Wadsley, J.

    PY - 2015/1/1

    Y1 - 2015/1/1

    N2 - The radial density profiles of stellar galaxy discs can be well approximated as an exponential. Compared to this canonical form, however, the profiles in the majority of disc galaxies show downward or upward breaks at large radii. Currently, there is no coherent explanation in a galaxy formation context of the radial profile per se, along with the two types of profile breaks. Using a set of controlled hydrodynamic simulations of disc galaxy formation, we find a correlation between the host halo's initial angular momentum and the resulting radial profile of the stellar disc: galaxies that live in haloes with a low spin parameter λ≲0.03 show an up-bending break in their disc density profiles, while galaxies in haloes of higher angular momentum show a down-bending break. We find that the case of pure exponential profiles (λ≈0.035) coincides with the peak of the spin parameter distribution from cosmological simulations. Our simulations not only imply an explanation of the observed behaviours, but also suggest that the physical origin of this effect is related to the amount of radial redistribution of stellar mass, which is anticorrelated with λ.

    AB - The radial density profiles of stellar galaxy discs can be well approximated as an exponential. Compared to this canonical form, however, the profiles in the majority of disc galaxies show downward or upward breaks at large radii. Currently, there is no coherent explanation in a galaxy formation context of the radial profile per se, along with the two types of profile breaks. Using a set of controlled hydrodynamic simulations of disc galaxy formation, we find a correlation between the host halo's initial angular momentum and the resulting radial profile of the stellar disc: galaxies that live in haloes with a low spin parameter λ≲0.03 show an up-bending break in their disc density profiles, while galaxies in haloes of higher angular momentum show a down-bending break. We find that the case of pure exponential profiles (λ≈0.035) coincides with the peak of the spin parameter distribution from cosmological simulations. Our simulations not only imply an explanation of the observed behaviours, but also suggest that the physical origin of this effect is related to the amount of radial redistribution of stellar mass, which is anticorrelated with λ.

    KW - Galaxies: spiral

    KW - Galaxies: structure

    KW - Hydrodynamics

    KW - Methods: numerical

    UR - http://www.scopus.com/inward/record.url?scp=84937921589&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=84937921589&partnerID=8YFLogxK

    U2 - 10.1093/mnrasl/slv006

    DO - 10.1093/mnrasl/slv006

    M3 - Article

    VL - 448

    SP - L99-L103

    JO - Monthly Notices of the Royal Astronomical Society: Letters

    JF - Monthly Notices of the Royal Astronomical Society: Letters

    SN - 1745-3925

    IS - 1

    ER -