Infrared Spectral Energy Distribution of Galaxies in the AKARI All Sky Survey: Correlations with Galaxy Properties, and Their Physical Origin

We have studied the properties of more than 1600 low-redshift galaxies by utilizing high-quality infrared flux measurements of the AKARI All-Sky Survey and physical quantities based on optical and 21-cm observations. Our goal is to understand the physics determining the infrared spectral energy distribution (SED). The ratio of the total infrared luminosity, L-TIR, to the star-formation rate (SFR) is tightly correlated by a power-law to specific SFR (SSFR), and L-TIR is a good SFR indicator only for galaxies with the largest SSFR. We discovered a tight linear correlation for normal galaxies between the radiation field strength of dust heating, estimated by infrared SED fits (U-h), and that of galactic-scale infrared emission (U-TIR alpha L-TIR/R-2), where R is the optical size of a galaxy. The dispersion of Uh along this relation is similar to 0.3 dex, corresponding to similar to 13% dispersion in the dust temperature. This scaling and the U-h/U-TIR ratio can be explained physically by a thin layer of heating sources embedded in a thicker, optically-thick dust screen. The data also indicate that the heated fraction of the total dust mass is anti-correlated to the dust column density, supporting this interpretation. In the large U-TIR limit, the data of circumnuclear starbursts indicate the existence of an upper limit on U-h, corresponding to the maximum SFR per gas mass of similar to 10 Gyr(-1) We find that the number of galaxies sharply drops when they become optically thin against dust-heating radiation, suggesting that a feedback process to galaxy formation (likely by the photoelectric heating) is working when dust-heating radiation is not self-shielded on a galactic scale. Implications are discussed for the M-H1-size relation, the Kennicutt-Schmidt relation, and galaxy formation in the cosmological context.