We measure the cross-power spectra between luminous red galaxies ( LRGs ) from the Sloan Digital Sky Survey ( SDSS ) -III Data Release Eight ( DR8 ) and Cosmic Infrared Background ( CIB ) anisotropies from Planck and data from the Improved Reprocessing ( IRIS ) of the Infrared Astronomical Satellite ( IRAS ) at 353 , 545 , 857 , and 3000 GHz , corresponding to 850 , 550 , 350 and 100 \thinspace \mu m , respectively , in the multipole range \mathrm { 100 < \mathrm { l } < 1000 } .
Using approximately 6.5 \cdot 10 ^ { 5 } photometrically determined LRGs in 7760 deg ^ { 2 } of the northern hemisphere in the redshift range \mathrm { 0.45 < z < 0.65 } , we model the far-infrared background ( FIRB ) anisotropies with an extended version of the halo model .
With these methods , we confirm the basic picture obtained from recent analyses of FIRB anisotropies with Herschel and Planck that the most efficient halo mass at hosting star forming galaxies is \mathrm { log ( M _ { eff } / M _ { \odot } ) = 12.84 \pm 0.15 } .
We estimate the percentage of FIRB anisotropies correlated with LRGs as approximately 11.8 \% , 3.9 \% , 1.8 \% , and 1.0 \% of the total at 3000 , 857 , 545 , and 353 GHz , respectively .
At redshift \mathrm { z \sim 0.55 } , the bias of FIRB galaxies with respect to the dark matter density field has the value \mathrm { b _ { FIRB } \sim 1.45 } , and the mean dust temperature of FIRB galaxies is T _ { d } =26 K. Finally , we discuss the impact of present and upcoming cross-correlations with far-infrared background anisotropies on the determination of the global star formation history and the link between galaxies and dark matter .