Fig. 5.
Best-fit model of the SED of source A using SED3FIT (Berta et al. 2013). The black line is the total fitted emission, whereas blue and green lines represent the contribution of stellar and AGN emission, respectively. The fit uses photometry from CFHT r to IRAC 5.8 μm, and the nondetection in the Spitzer IRAC 8.0 μm and MIPS 24 μm bands (in red). We also show the GTC spectrum of source A (in gray, smoothed for visual purpose). We note the flux excess in the g-band (not included in the fit) due to the strong Lyα emission.
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