Fig. 12.—Bolometric corrections as a function of frequency for the SEDs in Fig. 11. The color coding is the same as for the previous figure (except that the full SDSS-DR3 mean quasar SED is now shown in gray instead of cyan). The dashed gray curve shows the full-sample mean SED without correction for the host galaxy contribution. The bolometric correction from 5100 8 for the Elvis et al. (1994) radio-quiet SED is 12.17 (thin solid line). As in Fig. 11, the bottom panel shows the 1 error in the bolometric correction derived from the overall mean SED with the most robust parts of the SED shown by thicker line segments. The kinks in the error spectrum attest to the importance of considering the range of quasar SEDs by demonstrating the homogenizing effects of assuming a singlemean SED in our gap repair process. The vertical lines in the bottom panel indicate the frequencies that are compared in Fig. 13.
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