tokens: BCGs at 0.5 z 1.0 to derive L TIR and the associated dust-obscured SFR, dust temperature and mass, but neither attempt to mitigate confusion noise in these bands, nor match the observed far-infrared and 24 m emission in their SED template fitting (which are not simultaneously fit for significant number of their sources).] Furthermore, the results of the template fitting show that a customized combination of components provides a better description of the BCG stacked fluxes in most instances than any single template from a pre-existing library, particularly at z 1. It is clear that an elliptical template alone is not sufficient to match any of the SEDs, as the far-infrared emission of the BCGs is one to two orders of magnitude brighter than that of a typical red and dead elliptical galaxy template. As for the star-forming fit, based on the dust scaling relations empirically derived from observations of Herschel Reference Survey galaxies of a large range of spectral type, environment and stellar mass in the local Universe (Cortese etal. 2012 ) specifically the inverse proportionality between dust-to-stellar mass ratio and the stellar mass and specific star formation rate (sSFR) in local galaxies we expect the BCG SED to exhibit a significantly lower dust-to-stellar mass ratio in comparison to a less-massive non-BCG star-forming template, which is exactly what we find. At the lowest redshifts we consider, z avg 0.185, a typical star-forming SED matches the BCG SED longward of 10m, but the BCG stellar bump rises significantly above that of the star-forming template. While these dust scaling relations were derived for local field and cluster galaxies (including those in cluster cores), we do not yet know if they apply to galaxies at higher redshifts (though we might expect them to if we assume an understanding of the physics underlying the trends). Whereas massive elliptical galaxies in the local Universe exhibit relatively low dust-to-stellar mass ratios on account of a diminished level of star formation activity with respect to local star-forming late-type galaxies, we would expect an increasing dust-to-stellar mass ratio for elliptical galaxies of a fixed stellar mass with increasing sSFR towards higher redshift, as observed in our sample (reminding the reader that we select BCGs from clusters of the same mass at every redshift, therefore the BCGs are of the same mass at every redshift based on the linear scaling of BCG stellar mass and host-cluster mass, e.g. Lidman etal. 2012 ). In fact, as we move towards higher redshift, we observe the star-forming templates begin to match the full extent of the BCG SED better and better, as opposed to just the far-IR bump at lower redshifts. Therefore, we fit the stellar emission shortward of 10m in the faint SEDs with only the Polletta 13-Gyr Elliptical model, but add to this model either of the Polletta M82 or S18 templates to fit the stellar emission in the bright SEDs. In the mid- and far-infrared
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