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(i) In the first galaxies, the SN feedback ejects most gas and dust
from galaxies, resulting in the intermittent star formation history.
This causes the large fluctuation of escape fraction of UV photons.
The escape fraction of Halo-11 changes in the range of ∼0.2–0.8
at z < 10. As the halo becomes more massive, the fluctuation
is suppressed, and the escape fraction remains low at 0.2. The
transition redshifts are ∼8.5 for Halo-12 and ∼7.5 for Halo-11.
In the case of Halo-10, the escape fraction keeps fluctuating down
to z = 6.
(ii) Stellar UV radiation absorbed by dust is reprocessed into IR
thermal emission. Therefore, the IR flux from galaxies also change
with time as the UV escape fraction fluctuates. This fluctuation of
the IR flux affects the detectability in sub-mm observations. Using
all satellite galaxies within the zoom-in regions, we calculate the
detectability by ALMA telescope. If we set the detection threshold
to 0.1 mJy at 850 μm, the detectability are 0.5 for galaxies with
the halo mass of 1011 M at z 7.
(iii) We calculate the three-dimensional structure of dust temperature, and derive SEDs. By using the peak wavelength of infrared
flux, we estimate the typical dust temperature of modelled galaxies.
The galaxies with LIR 1011 L have Td ∼ 60 K that is higher than
that of observed galaxies at z < 3 (Hwang et al. 2010). Since it is
difficult to measure the dust temperature of observed galaxies at z
≥ 6, the dust temperature of ∼ 40 K is frequently assumed in the
observations (e.g. Watson et al. 2015). Our simulation suggests that
the dust temperatures for high-z galaxies are somewhat higher than
the assumed ones, which will change the estimated dust masses and
SFRs.
(iv) The half-light radius (re ) at UV wavelength fluctuates in the
range of re /rvir ∼ 0.02–0.1, and it increases with time. At z ∼ 6–
8, re becomes ∼ 1 kpc (physical), and the bright galaxies in our
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0.4. These are consistent with the observations of Kawamata et al.
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parts of UV flux can be lost below observational threshold due to
cosmological surface brightness dimming.
(v) We compare our fiducial model (Halo-11) with the different
models with a low star formation amplitude factor (Halo-11-lowSF)
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Therefore, the IR flux of Halo-11-lowSF and Halo-11-noSN is
higher than that of Halo-11. Thus we argue that the star formation
and feedback models for the first galaxies could be constrained by
future observations.
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