All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{6048fig1.ps} \end{figure}$ Figure 1: The pn spectrum of PG 1416-129 (in the observed frame). A power-law has been fit to the 2-5 keV data and extrapolated to lower and higher energies. A weak soft X-ray positive residual is seen between 0.3-1 keV, as well as the presence of a Fe K $\alpha$ complex between about 4.8-5.7 keV ( $\sim$ 5.4-6.4 keV in the quasar frame). For presentation only, the data have been re-binned into groups of 10 bins, after a grouping of a minimum of 20 counts per bin is used for the fit.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{6048fig2.ps} \end{figure}$ Figure 2: The time-averaged pn spectrum of PG 1416-129 (in the observed frame). A relativistically blurred photo-ionized disc model ( REFLION: Ross & Fabian 2005) has been fit, and which provides a good representation of the whole energy band. A primary power-law component is taken into account in the model. Both component models are displayed without blurring in the upper panel. See text for the values of the fit parameters. For presentation only, the data have been re-binned into groups of 10 bins, after group of a minimum of 20 counts per bin is used for the fit.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{6048fig3CMJN.eps} \end{figure}$ Figure 3: The signal-to-noise deviations (in $\sigma$ ) of the Fe K $\alpha$ line above the power-law continuum in the energy-time plane. The energy axis is given in the observed frame. The colour-scale represents excess signal/noise in the line counts above the fitted continuum. Energy and time are oversampled by a factor of 10. Data are top-hat smoothed by 10 ks in time and Gaussian smoothed with ${\it FWHM}=0.14$ keV in energy. The regions 1-3 correspond to the time selections used for the time-resolved spectroscopic analysis. See text for explanation.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{6048fig4.ps} \end{figure}$ Figure 4: The three pn time-resolved spectroscopy spectra (in the observed frame) obtained by splitting the average spectra according to the time regions shown in Fig. 3. The three sub-spectra have been fit with a power-law continuum model. Here, 5.67 keV in the observed frame corresponds to 6.4 keV in the rest frame. Notice the residuals present at 4.8 keV and 5.6 keV in segments 1 ( upper panel) and 3 ( lower panel), respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{6048fig5.ps} \end{figure}$ Figure 5: The pn sub-spectrum 3 of PG 1416-129 (in the observed frame). A power law continuum plus a DISKLINE model have been fit. A narrow annulus is assumed with $\Delta R$ = 1 $R_{\rm g}$ . See text for the best fit parameter values.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{6048fig5.ps} \end{figure}$	Figure 5: The pn sub-spectrum 3 of PG 1416-129 (in the observed frame). A power law continuum plus a DISKLINE model have been fit. A narrow annulus is assumed with $\Delta R$ = 1 $R_{\rm g}$ . See text for the best fit parameter values.
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