Cosmic Evolution of Dust in Galaxies: Methods and Preliminary Results

    Research output: Contribution to journalArticle

    9 Citations (Scopus)

    Abstract

    We investigate the redshift (z) evolution of dust mass and abundance, their dependences on initial conditions of galaxy formation, and physical correlations between dust, gas, and stellar contents at different z based on our original chemodynamical simulations of galaxy formation with dust growth and destruction. In this preliminary investigation, we first determine the reasonable ranges of the most important two parameters for dust evolution, i.e., the timescales of dust growth and destruction, by comparing the observed and simulated dust mass and abundances and molecular hydrogen (H2) content of the Galaxy. We then investigate the z-evolution of dust-to-gas ratios (D), H2 gas fraction (fH2), and gas-phase chemical abundances (e.g., A O = 12 + log (O/H)) in the simulated disk and dwarf galaxies. The principal results are as follows. Both D and (fH2) can rapidly increase during the early dissipative formation of galactic disks (z ~ 2-3), and the z-evolution of these depends on initial mass densities, spin parameters, and masses of galaxies. The observed A O-D relation can be qualitatively reproduced, but the simulated dispersion of D at a given A O is smaller. The simulated galaxies with larger total dust masses show larger H2 and stellar masses and higher (fH2). Disk galaxies show negative radial gradients of D and the gradients are steeper for more massive galaxies. The observed evolution of dust masses and dust-to-stellar-mass ratios between z = 0 and 0.4 cannot be reproduced so well by the simulated disks. Very extended dusty gaseous halos can be formed during hierarchical buildup of disk galaxies. Dust-to-metal ratios (i.e., dust-depletion levels) are different within a single galaxy and between different galaxies at different z.
    Original languageEnglish
    Pages (from-to)1-25
    JournalThe Astrophysical Journal
    Volume799
    Issue number2
    Early online date27 Jan 2015
    DOIs
    Publication statusPublished - 1 Feb 2015

    Fingerprint

    dust
    galaxies
    disk galaxies
    galactic evolution
    stellar mass
    gas
    destruction
    method
    gases
    gradients
    dwarf galaxies
    mass ratios
    halos
    depletion
    hydrogen
    vapor phases
    timescale
    metal
    metals

    Cite this

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    title = "Cosmic Evolution of Dust in Galaxies: Methods and Preliminary Results",
    abstract = "We investigate the redshift (z) evolution of dust mass and abundance, their dependences on initial conditions of galaxy formation, and physical correlations between dust, gas, and stellar contents at different z based on our original chemodynamical simulations of galaxy formation with dust growth and destruction. In this preliminary investigation, we first determine the reasonable ranges of the most important two parameters for dust evolution, i.e., the timescales of dust growth and destruction, by comparing the observed and simulated dust mass and abundances and molecular hydrogen (H2) content of the Galaxy. We then investigate the z-evolution of dust-to-gas ratios (D), H2 gas fraction (fH2), and gas-phase chemical abundances (e.g., A O = 12 + log (O/H)) in the simulated disk and dwarf galaxies. The principal results are as follows. Both D and (fH2) can rapidly increase during the early dissipative formation of galactic disks (z ~ 2-3), and the z-evolution of these depends on initial mass densities, spin parameters, and masses of galaxies. The observed A O-D relation can be qualitatively reproduced, but the simulated dispersion of D at a given A O is smaller. The simulated galaxies with larger total dust masses show larger H2 and stellar masses and higher (fH2). Disk galaxies show negative radial gradients of D and the gradients are steeper for more massive galaxies. The observed evolution of dust masses and dust-to-stellar-mass ratios between z = 0 and 0.4 cannot be reproduced so well by the simulated disks. Very extended dusty gaseous halos can be formed during hierarchical buildup of disk galaxies. Dust-to-metal ratios (i.e., dust-depletion levels) are different within a single galaxy and between different galaxies at different z.",
    author = "Kenji Bekki",
    year = "2015",
    month = "2",
    day = "1",
    doi = "10.1088/0004-637X/799/2/166",
    language = "English",
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    Cosmic Evolution of Dust in Galaxies: Methods and Preliminary Results. / Bekki, Kenji.

    In: The Astrophysical Journal, Vol. 799, No. 2, 01.02.2015, p. 1-25.

    Research output: Contribution to journalArticle

    TY - JOUR

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    AU - Bekki, Kenji

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    N2 - We investigate the redshift (z) evolution of dust mass and abundance, their dependences on initial conditions of galaxy formation, and physical correlations between dust, gas, and stellar contents at different z based on our original chemodynamical simulations of galaxy formation with dust growth and destruction. In this preliminary investigation, we first determine the reasonable ranges of the most important two parameters for dust evolution, i.e., the timescales of dust growth and destruction, by comparing the observed and simulated dust mass and abundances and molecular hydrogen (H2) content of the Galaxy. We then investigate the z-evolution of dust-to-gas ratios (D), H2 gas fraction (fH2), and gas-phase chemical abundances (e.g., A O = 12 + log (O/H)) in the simulated disk and dwarf galaxies. The principal results are as follows. Both D and (fH2) can rapidly increase during the early dissipative formation of galactic disks (z ~ 2-3), and the z-evolution of these depends on initial mass densities, spin parameters, and masses of galaxies. The observed A O-D relation can be qualitatively reproduced, but the simulated dispersion of D at a given A O is smaller. The simulated galaxies with larger total dust masses show larger H2 and stellar masses and higher (fH2). Disk galaxies show negative radial gradients of D and the gradients are steeper for more massive galaxies. The observed evolution of dust masses and dust-to-stellar-mass ratios between z = 0 and 0.4 cannot be reproduced so well by the simulated disks. Very extended dusty gaseous halos can be formed during hierarchical buildup of disk galaxies. Dust-to-metal ratios (i.e., dust-depletion levels) are different within a single galaxy and between different galaxies at different z.

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