Figure 7. Dust temperature (Td) as a function of total infrared luminosity (LIR) for the line emitters in our survey, color-coded by redshift. At a given redshift, the characteristic dust temperature roughly corresponds to the wavelength at which a galaxy’s SED peaks. Individual line emitters are shown, as well as the median of the sample. The z;4.5 AS2UDS candidate [C II] emitters have warmer dust temperatures, or equivalently their dust SEDs peak at shorter wavelengths, at fixed luminosity compared to z;0 galaxies. For comparison we also show ALESS SMGs from Swinbank et al. (2014) (a typical error bar is shown in the lower left), with median values overplotted and color-coded by redshift. Binned low-redshift SPIRE-selected (U)LIRGs from Symeonidis et al. (2013) are shown by the solid triangles. We indicate the low-redshift correlation by the dotted line. The dashed line shows the approximate selection limit for an 870 μm selected sample with S870>3.6 mJy: sources to the right of this line would be detected. The dotted–dashed line shows the approximate selection limit for 4<z<6.5 sources whose SED peaks at λ 500 μm, socalled “500 μm risers” (Dowell et al. 2014): sources to the right of this line would be selected. Plotted for comparison are three such sources, with spectroscopic redshifts z>4, from the First Look Summary (FLS) of the Herschel Multi-tiered Extragalactic Survey (HerMES; Oliver et al. 2012).
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