Table 8: Fit results, in the 2-12 keV energy band, of a disk reflection model assuming a LAMPPOST geometry for I Zw1, PG 0804+761, PG 1114+445, PG 1116+215 and PG 1309+355, i.e. we assume a height of 10 $R_{\rm g}$ , a ratio of X-ray to disk flux of 0.2 (with solar iron abundance). For PG 1402+261, a lower height above the AD of about 2.5 $R_{\rm g}$ , an iron abundance of 5 relative to solar abundance are required. Its spectrum is dominated by reflection.
Object $\Gamma$ $\theta$ (deg) $r_{\rm in}$ ( $r_{\rm g}$ ) $\chi^{2}$ /d.o.f.

I Zw1 2.28 $\pm$ 0.03 $\rm 42^{+23}_{-19}$ $\rm 16^{+17}_{-10}$ 598.7/590

PG 0804+761 2.07 $\pm$ 0.06 42 $\pm$ 21 <14 212.2/250

PG 1116+215 2.12 $\pm$ 0.09 30 $\pm$ 22 <13 124.6/104

PG 1309+355 1.74 $\pm$ 0.09 <27 <30 62.9/86

PG 1402+261 2.13 $\pm$ 0.10 >60 <5 85.9/92

**Table 8:** Fit results, in the 2-12 keV energy band, of a disk reflection model assuming a LAMPPOST geometry for I Zw1, PG 0804+761, PG 1114+445, PG 1116+215 and PG 1309+355, i.e. we assume a height of 10 $R_{\rm g}$ , a ratio of X-ray to disk flux of 0.2 (with solar iron abundance). For PG 1402+261, a lower height above the AD of about 2.5 $R_{\rm g}$ , an iron abundance of 5 relative to solar abundance are required. Its spectrum is dominated by reflection.
Object	$\Gamma$	$\theta$ (deg)	$r_{\rm in}$ ( $r_{\rm g}$ )	$\chi^{2}$ /d.o.f.
I Zw1	2.28 $\pm$ 0.03	$\rm 42^{+23}_{-19}$	$\rm 16^{+17}_{-10}$	598.7/590
PG 0804+761	2.07 $\pm$ 0.06	42 $\pm$ 21	<14	212.2/250
PG 1116+215	2.12 $\pm$ 0.09	30 $\pm$ 22	<13	124.6/104
PG 1309+355	1.74 $\pm$ 0.09	<27	<30	62.9/86
PG 1402+261	2.13 $\pm$ 0.10	>60	<5	85.9/92

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