Fig. 11.—Mean quasar SEDs and the data used to construct them. The points show the data; the lines show themean SEDs. From left to right: black crosses, MIPS70; black points, MIPS24/ ISO15; red points, S8:0; green points, S5:8; cyan points, S4:5; blue points, S3:6; gray points, K; yellow points, H; cyan points, J; black points, z; magenta points, i; red points, r; green points, g; blue points, u; orange points, n; purple points, f ; black crosses, X-ray. The dotted lines show the range of ox with luminosity for the luminosity extremes of our sample (Strateva et al. 2005). From top to bottom (at 1014 Hz) the thick solid lines are color coded as follows: green, optically luminous SDSS quasars; red, optically red SDSS quasars; cyan, all SDSS quasars; blue, optically blue SDSS quasars; black, Elvis et al. (1994) radio-quiet mean SED; gray, Hatziminaoglou et al. (2005) mean SED (normalized to Elvis et al. 1994 at 1 m); orange, optically dim SDSS quasars. The near-IR luminous/dim composites are nearly identical to the optical composites. The thin green, cyan, and orange curves show the host galaxy contribution assuming (LBol/LEdd) ¼ 1 (see eq. [1]) for the elliptical galaxy composite spectrum of Fioc & Rocca-Volmerange (1997). The dashed cyan curve shows the effect of ignoring the host contribution. The inset at the upper right zooms in on theMIR region of the spectrum. The three curves are normalized at 1.3 m, and the y-axis shows relative luminosity ( L ), while the x-axis is in microns. The bottom panel shows the 1 error array (dex) for our overall mean SED. Those frequencies where over 100 quasars contribute to the mean SED are shown as thicker line segments and are relatively unaffected by the gap-repair process.
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