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All Tables

- Table 1:
The sample.
- Table 9:
Dispersion and mean value of the relevant parameters of the
models tested for the sample and the Laor et al. (1997) subsample. See
Sects. 3.2 and 3.3 for details. The mean values of the
*kT* in models A, B and C are given in units of keV.
- Table 11:
Fluxes and absorption-corrected luminosities calculated assuming the best fit
model. The last two columns list the ratio between the strength of the soft
excess and the high energy power law component in the 0.5-2 and
0.5-10 keV band, respectively.
- Table 12:
Spearman-rank correlations among spectral parameters of the
soft excess tested models and X-ray parameters (luminosity and
). The displayed values are
(,
), where
is the rank correlation coefficient and
is the
significance probability. The significant (i.e. >95%) correlations
are marked in boldface (see text for details).
- Table 13:
Spearman-rank correlations among X-ray observables and
the radio-loudness parameter ,
the redshift, the
* FWHM* of the H emission line, the black hole mass
and the accretion rate
with respect to the Eddington rate. The displayed values are
(,
), where
is the rank correlation coefficient and
is the significance probability. The significant (i.e. >95%)
correlations are marked in boldface (see text for details).
- Table 2:
Journal of observations.
- Table 3:
Spectral fitting results. I: power law model applied to the
hard band (2-12 keV). 1001+054 is excluded due to the very poor
statistics in this energy range.
- Table 4:
Spectral fitting results. II: power law model (model PL) applied to the 0.3-12 keV band.
- Table 5:
Spectral fitting results. III: power law plus blackbody model
for the soft excess component (model A).
- Table 6:
Spectral fitting results. IV: power law plus multi-color
blackbody model for the soft excess component (model B).
- Table 7:
Spectral fitting results. V: power law plus bremsstrahlung model for the
soft excess (model C).
- Table 8:
Spectral fitting results. VI: double power law (model D).
- Table 10:
Spectral fitting results. VII: best fit model. A: bb; B: diskbb; C:
brems; D: power law; E: double bb; F: absori; G: double absori + bb; H: partial-covering
(cold)+raymond-smith; I: partial-covering(warm)+emission line;
J: absori+bb; PL: simple power law. Models with
^{*} include an
additional cold absorption component. All but one (i.e. model PL) models
also include a power law component. For the results concerning the Fe K
line see Paper II.