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tokens: high SFRs of the present sample result in some of the X-ray luminosities being even greater than the erg s −1 value often used to identify sources as clear AGNs (e.g., Hornschemeier et al. 2001 ; Barger et al. 2002 ; Bauer et al. 2004 ; Szokoly et al. 2004 ) based on maximal local star-forming galaxy X-ray luminosities. Laird et al. ( 2010 ) similarly concluded that very high SFRs were responsible for the high X-ray luminosities of most of the sources in their submillimeter-selected sample in the same field. The AGN-classified sources in Figure 4 (b) show a much wider spread in , ranging from near quasar X-ray luminosities to nearly X-ray undetected sources. However, there are a number of sources with luminosities close to those of the star-forming galaxies, and there is clearly not a one-to-one correlation between our classifications and X-ray luminosity. 4. THE FIR-RADIO CORRELATION Radio power is often used along with the FIR-radio correlation as a measure of the SFR (e.g., Cram et al. 1998 ; Hopkins et al. 2003 ; Netzer et al. 2007 ; Mineo et al. 2014 ; Mushotzky et al. 2014 ). However, this could be risky when no other information is available on whether a source is AGN dominated or star-formation dominated. After all, it is well known that some local radio-quiet AGNs lie on the FIR-radio correlation (e.g., Condon 1992 ; Morić et al. 2010 ; Wong et al. 2016 ), even if it is not understood why. In Figure 5 , we plot (a) luminosity and (b) luminosity versus radio power for the radio sources with spectroscopic or photometric redshifts and erg s −1 Hz −1 . We use colors to denote the sources classified as star-forming galaxies (green circles), composites (blue circles), and AGNs (red circles). In (a), we also mark the sources that Chi et al. ( 2013 ) found to be AGNs using VLBI observations with surrounding black circles. All of these sources lie below the FIR-radio correlation. The star-forming galaxies in (a) have a mean , where we have computed the error with the jackknife resampling statistic; all lie within a multiplicative factor of three of the median value ( q = 2.35), which we denote by shading. Five AGNs and four composites also lie in the region. Figure 5. (a) luminosity and (b) luminosity vs. 20 cm power for the radio sources with spectroscopic or photometric redshifts and erg s −1 Hz −1 . Green circles denote star-forming galaxies, blue circles composites, and red circles AGNs. The central black line shows the median FIR-radio correlation of the star-forming galaxies, and the shading shows the region where we consider the sources to lie on the FIR-radio correlation (multiplicative factor of three of the central value). In (a), we mark the sources that Chi et al. ( 2013 ) found to be AGNs using VLBI observations with surrounding black circles. All of these sources lie below the FIR-radio correlation. In Figure 6 (a), we show the SEDs of 12 of the star-forming galaxies that lie on the FIR-radio correlation, as defined by the