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Recent observations have successfully detected UV or infrared flux fromgalaxies at the epoch of reionization. However, the origin of their radiativeproperties has not been fully understood yet. Combining cosmologicalhydrodynamic simulations and radiative transfer calculations, we presenttheoretical predictions of multi-wavelength radiative properties of the firstgalaxies at z=6-15. We find that most of the gas and dust are ejected fromstar-forming regions due to supernova (SN) feedback, which allows UV photons toescape. We show that the peak of SED rapidly shifts between UV and infraredwavelengths on a timescale of 100 Myr due to intermittent star formation andfeedback. When dusty gas covers the star-forming regions, the galaxies becomebright in the observed-frame sub-millimeter wavelengths. In addition, we findthat the escape fraction of ionizing photons also changes between 1-40% atz>10. The mass fraction of HII region changes with the star formation history,resulting in the fluctuations of metal lines and Lyman-alpha line luminosities.In the starbursting phase of galaxies with the halo mass $\sim 10^{11}\,{\rmM_{\odot}}$ ($10^{12}\,{\rm M_{\odot}}$), the simulated galaxy has $L_{\rm[O\,III]} \sim 10^{42}\, (10^{43})\, {\rm erg\,s^{-1}}$, which is consistentwith the observed star-forming galaxies at z>7. Our simulations suggest thatdeep [C II] observation with ALMA can trace the distribution of neutral gasextending over $\sim 20$ physical kpc. We also find that the luminosity ratio$L_{\rm [O\,III]}/L_{\rm [C\,II]}$ decreases with bolometric luminosity due tometal enrichment. Our simulations show that the combination of multi-wavelengthobservations by ALMA and JWST will be able to reveal the multi-phase ISMstructure and the transition from starbursting to outflowing phases of high-zgalaxies.

Galaxy evolution and radiative properties in the early Universe: multi-wavelength analysis in cosmological simulations