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Fig. 4


Fit of the a = 0 (log M = 6.55) model (see Table 2) to the optical/UV spectrum of RE J1034+396 (red line) to the data (black line); red line below shows the disk contribution, pink line Balmer Continuum, green solid line the Fe II contribution below 2250 Å (Vestergaard & Wilkes 2001), green dashed line the Fe II above 2250 Å (Bruhweiler & Verner 2008). Stars contribute significantly to the spectrum even in UV part. The HST data are renormalized by constant 0.717.

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