In all fits, cosmic abundances for the fitted column density N 
and
the photoelectric cross sections of Morrison & McCammon (1983) were
used. A fit was retained acceptable if the corresponding 
probability was equal or larger than 5%. The improvement in the
obtained by adding additional fit parameters was estimated
with the F-test, with a threshold for a significant improvement
P 
=95%.
A single power law model absorbed by the Galactic column density
(N 
cm 
; Murphy et al. 1997) along the
line of sight provides a poor fit to the ASCA data of 3C445, with a
reduced of 
for 421 degrees of freedom (dofs),
which is rejected at > 99% confidence. This fit yields a negative
photon index 
. Figure 1 shows the residuals of
the single power law model for the SIS and GIS detectors
separately. Deviation from the model in the form of excess flux below
1.5 keV and the Fe line at 
6 keV are apparent.
The modelling of the Fe line depends critically on the
parameterization of the underlying continuum. We thus concentrated
first on finding an adequate description of the latter, and restricted
our spectral fits to the energy range 0.6-10 keV excluding the 5-7
keV region. The fits to the continuum are discussed in § 3.1, with
the Fe line fits following in § 3.2. The results of the spectral
fits are summarized in Table 2, where all quoted uncertainties on the
parameters are 90% for 1 parameter of interest
( 
=2.7). All quantities in Table 2 are in the observer's
rest-frame.
