TY - JOUR
T1 - A new galaxy Spectral Energy Distribution model with the evolution of dust consistent with chemical evolution
AU - Nishida, Kazuki Y.
AU - Takeuchi, Tsutomu T.
AU - Nagata, Takuma
AU - Asano, Ryosuke S.
AU - Inoue, Akio K.
N1 - Publisher Copyright:
© International Astronomical Union 2020.
PY - 2019
Y1 - 2019
N2 - The spectral energy distribution (SED) model should treat the evolution of a galaxy from its birth. Dust in galaxies affects the formation and evolution of galaxies in various ways. For example, dust grains scatter and absorb stellar emitted ultraviolet (UV) photons and re-emit the radiation at infrared (IR) wavelengths. In this work, we construct a galaxy SED model based on our dust evolution model (Asano et al. 2013a,b, 2014) with a rigorous treatment of the chemical evolution. To reduce the computational cost, we adopt mega-grain approximation (MGA; (MGA; Inoue, 2005). MGA regards a high density dusty region as a huge size (10 pc) dust grain for calculating dust scattering. In this approximation, we can solve the radiative transfer easily and provide SEDs and attenuation curves of galaxies. This model can be used to fit any galaxy in the wavelength range of 10 nm-3 mm.
AB - The spectral energy distribution (SED) model should treat the evolution of a galaxy from its birth. Dust in galaxies affects the formation and evolution of galaxies in various ways. For example, dust grains scatter and absorb stellar emitted ultraviolet (UV) photons and re-emit the radiation at infrared (IR) wavelengths. In this work, we construct a galaxy SED model based on our dust evolution model (Asano et al. 2013a,b, 2014) with a rigorous treatment of the chemical evolution. To reduce the computational cost, we adopt mega-grain approximation (MGA; (MGA; Inoue, 2005). MGA regards a high density dusty region as a huge size (10 pc) dust grain for calculating dust scattering. In this approximation, we can solve the radiative transfer easily and provide SEDs and attenuation curves of galaxies. This model can be used to fit any galaxy in the wavelength range of 10 nm-3 mm.
KW - Panchromatic codes and modeling techniques
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U2 - 10.1017/S1743921319004794
DO - 10.1017/S1743921319004794
M3 - Article
AN - SCOPUS:85106835572
SN - 1743-9213
VL - 15
SP - 152
EP - 156
JO - Proceedings of the International Astronomical Union
JF - Proceedings of the International Astronomical Union
IS - S341
ER -