Dust scaling relations in a cosmological simulation. (arXiv:1901.02886v1 [astro-ph.GA])

Dust scaling relations in a cosmological simulation. (arXiv:1901.02886v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Hou_K/0/1/0/all/0/1">Kuan-Chou Hou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aoyama_S/0/1/0/all/0/1">Shohei Aoyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirashita_H/0/1/0/all/0/1">Hiroyuki Hirashita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagamine_K/0/1/0/all/0/1">Kentaro Nagamine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shimizu_I/0/1/0/all/0/1">Ikkoh Shimizu</a>

To study the dust evolution in the cosmological structure formation history,
we perform a smoothed particle hydrodynamic simulation with a dust enrichment
model in a cosmological volume. We adopt the dust evolution model that
represents the grain size distribution by two sizes and takes into account
stellar dust production and interstellar dust processing. We examine the dust
mass function and the scaling properties of dust in terms of the
characteristics of galaxies. The simulation broadly reproduces the observed
dust mass functions at redshift $z = 0$, except that it overproduces the
massive end at dust mass $M_mathrm{d} gtrsim 10^{8}$ ${rm M}_odot$. This
overabundance is due to overproducing massive gas/metal-rich systems, but we
also note that the relation between stellar mass and gas-phase metallicity is
reproduced fairly well by our recipe. The relation between dust-to-gas ratio
and metallicity shows a good agreement with the observed one at $z=0$, which
indicates successful implementation of dust evolution in our cosmological
simulation. Star formation consumes not only gas but also dust, causing a
decreasing trend of the dust-to-stellar mass ratio at the high-mass end of
galaxies. We also examine the redshift evolution up to $z sim~ 5$, and find
that the galaxies have on average the highest dust mass at $z = 1-2$. For the
grain size distribution, we find that galaxies with metallicity $sim 0.3~
Z_odot$ tend to have the highest small-to-large grain abundance ratio;
consequently, the extinction curves in those galaxies have the steepest
ultraviolet slopes.

To study the dust evolution in the cosmological structure formation history,
we perform a smoothed particle hydrodynamic simulation with a dust enrichment
model in a cosmological volume. We adopt the dust evolution model that
represents the grain size distribution by two sizes and takes into account
stellar dust production and interstellar dust processing. We examine the dust
mass function and the scaling properties of dust in terms of the
characteristics of galaxies. The simulation broadly reproduces the observed
dust mass functions at redshift $z = 0$, except that it overproduces the
massive end at dust mass $M_mathrm{d} gtrsim 10^{8}$ ${rm M}_odot$. This
overabundance is due to overproducing massive gas/metal-rich systems, but we
also note that the relation between stellar mass and gas-phase metallicity is
reproduced fairly well by our recipe. The relation between dust-to-gas ratio
and metallicity shows a good agreement with the observed one at $z=0$, which
indicates successful implementation of dust evolution in our cosmological
simulation. Star formation consumes not only gas but also dust, causing a
decreasing trend of the dust-to-stellar mass ratio at the high-mass end of
galaxies. We also examine the redshift evolution up to $z sim~ 5$, and find
that the galaxies have on average the highest dust mass at $z = 1-2$. For the
grain size distribution, we find that galaxies with metallicity $sim 0.3~
Z_odot$ tend to have the highest small-to-large grain abundance ratio;
consequently, the extinction curves in those galaxies have the steepest
ultraviolet slopes.

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