The Impact of Dust on the Sizes of Galaxies in the Epoch of Reionization
  We study the sizes of galaxies in the Epoch of Reionization using a sample of
~100,000 galaxies from the BlueTides cosmological hydrodynamical simulation
from z=7 to 11. We measure the galaxy sizes from stellar mass and luminosity
maps, defining the effective radius as the minimum radius which could enclose
the pixels containing 50% of the total mass/light in the image. We find an
inverse relationship between stellar mass and effective half-mass radius,
suggesting that the most massive galaxies are more compact and dense than lower
mass galaxies, which have flatter mass distributions. We find a mildly negative
relation between intrinsic far-ultraviolet luminosity and size, while we find a
positive size-luminosity relation when measured from dust-attenuated images.
This suggests that dust is the predominant cause of the observed positive
size-luminosity relation, with dust preferentially attenuating bright sight
lines resulting in a flatter emission profile and thus larger measured
effective radii. We study the size-luminosity relation across the rest-frame
ultraviolet and optical, and find that the slope decreases at longer
wavelengths; this is a consequence of the relation being caused by dust, which
produces less attenuation at longer wavelengths. We find that the
far-ultraviolet size-luminosity relation shows mild evolution from z=7 to 11,
and galaxy size evolves with redshift as $R\propto(1+z)^{-m}$, where
$m=0.662\pm0.009$. Finally, we investigate the sizes of z=7 quasar host
galaxies, and find that while the intrinsic sizes of quasar hosts are small
relative to the overall galaxy sample, they have comparable sizes when measured
from dust-attenuated images.
