Infrared ( IR ) luminosity is fundamental to understanding the cosmic star formation history and AGN evolution , since their most intense stages are often obscured by dust .
However , local IR luminosity function estimates today are still based on the IRAS survey in the 1980s , with wavelength coverage only up to 100 \mu m. The AKARI IR space telescope performed all sky survey in 6 IR bands ( 9 , 18 , 65 , 90 , 140 , and 160 \mu m ) with 3-10 times better sensitivity , covering the crucial far-IR wavelengths across the peak of the dust emission .
Combined with a better spatial resolution , AKARI can much more precisely measure the total infrared luminosity ( L _ { TIR } ) of individual galaxies , and thus , the total infrared luminosity density in the local Universe .

By fitting modern IR SED models , we have re-measured L _ { TIR } of the IRAS Revised Bright Galaxy Sample , which is a complete sample of local galaxies with S _ { 60 \mu m } > 5.24 Jy .

We present mid-IR monochromatic luminosity ( \nu L _ { \nu } ) to L _ { TIR } correlations for Spitzer 8 \mu m , AKARI 9 \mu m , IRAS 12 \mu m , WISE 12 \mu m , ISO 15 \mu m , AKARI 18 \mu m , WISE 22 \mu m , and Spitzer 24 \mu m filters .
These measures of L _ { MIR } are well correlated with L _ { TIR } , with scatter ranging 13-44 % .
The best-fit L _ { MIR } -to- L _ { TIR } conversions provide us with estimates of L _ { TIR } using only a single MIR band , in which several deep all sky surveys are becoming available such as AKARI MIR and WISE .

Although we found some overestimates of L _ { TIR } by IRAS due to contaminating cirrus/sources , the resulting AKARI IR luminosity function ( LF ) agrees well with that from the IRAS .
We integrate the LF weighted by L _ { TIR } to obtain a cosmic IR luminosity density of \Omega _ { TIR } = ( 8.5 ^ { +1.5 } _ { -2.3 } ) \times 10 ^ { 7 } L _ { \odot } Mpc ^ { -3 } , of which 7 \pm 1 % is produced by LIRGs ( L _ { TIR } > 10 ^ { 11 } L _ { \odot } ) , and only 0.4 \pm 0.1 % is from ULIRGs ( L _ { TIR } > 10 ^ { 12 } L _ { \odot } ) in the local Universe , in a stark contrast to high-redshift results .

We separate the contributions from AGN and star-forming galaxies ( SFG ) .
SFG IR LF shows a steep decline at the bright-end .
Combined with high-redshift results from the AKARI NEP deep survey , these data show a strong evolution of \Omega _ { TIR } ^ { SF } \propto ( 1+z ) ^ { 4.0 \pm 0.5 } , and \Omega _ { TIR } ^ { AGN } \propto ( 1+z ) ^ { 4.4 \pm 0.4 } .
For \Omega _ { TIR } ^ { AGN } , the ULIRG contribution exceeds that from LIRG already by z \sim 1 .
A rapid evolution in both \Omega _ { TIR } ^ { AGN } and \Omega _ { TIR } ^ { SFG } suggests the correlation between star formation and black hole accretion rate continues up to higher redshifts .
We compare the evolution of \Omega _ { TIR } ^ { AGN } to that of X-ray luminosity density .
The \Omega _ { TIR } ^ { AGN } / \Omega _ { X - ray } ^ { AGN } ratio shows a possible increase at z > 1 , suggesting an increase of obscured AGN at z > 1 .