  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 micron, respectively,
in the multipole range 100<l<1000. Using approximately 6.5 10^5 photometrically
determined LRGs in 7760 deg^2 of the northern hemisphere in the redshift range
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
log(M_ eff/M_\odot)=12.84+/-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
z~0.55, the bias of FIRB galaxies with respect to the dark matter density field
has the value b_{FIRB}~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.
