24 fluxes for galaxies at redshift $z \geq 3$, we need to extend these templates to shorter wavelengths. For this purpose we employed the spectra of the individual local luminous (LIRGs) and ultraluminous infrared galaxies (ULIRGs) in Table 3 of Rieke et al. (2009), which extend down to 0.4. From these, we computed mean LIRG and ULIRG spectra and matched them onto the original Rieke templates below the cut-off wavelengths of 4.02 and 5.26. The ULIRG spectrum was used for the templates with log L(TIR)() $>$ 12, and the LIRG spectrum for the remaining templates. The resulting templates should be considered as schematic below $\sim 3$, as we did not attempt to model the stellar population and rest-frame optical extinction in a self-consistent fashion.

The template SEDs were integrated over the appropriate wavelengths ranges to yield the mapping between L(TIR) to L(FIR) shown in Fig. \[fig:LTIRtoFIR\_Rieke\]; the adopted relation between the two quantities is mildly non-linear: log L(FIR) = 1.1log L(TIR) – 1.42. Based on the IRAS Bright Galaxy Sample (Soifer et al. 2007), Marcillac et al. (2006) assumed a linear relation: L(FIR) = 1.91 L(TIR). In Fig. \[fig:RiekesameFIR\] we show the Rieke templates scaled to a common L(FIR).

At 