All Figures

$\begin{figure} \rotatebox{0}{\includegraphics[width=8.8cm,clip]{Figures/5615fig1.ps}} \end{figure}$ Figure 1: Radial dependence of redshift z of line cores (filled circles, left y-axis) and strength of gravitational redshift effect (triangles, right y-axis). Inclination angle amounts to $1^\circ$ .
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In the text

$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig2.ps}} \end{figure}$ Figure 2: Shift of line core energy in units of g-factor with distance to the black hole. Lowly inclined rings, $i=1^\circ$ , are compared to highly inclined rings, $i=75^\circ$ . Note the blueshift g > 1 in the latter case.
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In the text

$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig3.ps}} \end{figure}$ Figure 3: Two example relativistic lines emitted from a highly inclined ring, $i=75^\circ$ , and a face-on ring, $i=1^\circ$ , both with the emission peaking at the same $R_{\rm peak}=100.0 \ r_{\rm g}$ around a Kerr black hole with a/M=0.998. The arrows indicate the core g-factors, $g_{\rm core}\simeq 1.008$ and $g_{\rm core}\simeq 0.985$ respectively for each particular case.
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In the text

$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig4.ps}} \end{figure}$ Figure 4: Line distortion by strong gravity. The emission of narrow rings peaks at the radii as denoted in the legend. There is no way to confuse the lines because line flux successively decreases with decreasing radius of maximum emission $R_{\rm peak}$ . All rings follow Keplerian rotation around a Kerr black hole with a/M=0.998 and all are inclined to an inclination angle of $i=75^\circ$ .
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In the text

$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig5.ps}} \end{figure}$ Figure 5: Distortion of the red relic Doppler peak for rings satisfying $i=75^\circ$ : with decreasing radius the red peak can be found at lower peak energies due to strong gravitational redshift. Very close to the black hole - $r\protect \la 3 \ {r_{\rm g}}$ at this specific inclination - these distortions are such strong that the red Doppler peak is highly blurred and vanishes effectively in the line profile.
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In the text

$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig6.ps}} \end{figure}$ Figure 6: Energetic distance of red and blue Doppler peak at $i=75^\circ$ . This Doppler peak spacing (DPS) is measured in units of g. Far away from the black hole both peaks approach significantly and the double-peaked line profile becomes very narrow: At $\sim$ $3000 \ {r_{\rm g}}$ the peak difference in g only amounts to $\sim$ 0.03.
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In the text

$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig7.ps}} \end{figure}$ Figure 7: Radial dependence of the line core redshift: data for the NLS-1 Mrk 110 taken from K03 (boxes) are compared to the line core redshifts as computed from Kerr ray tracing simulations with different inclination angles. Redshift as a function of distance scales with a power law with identical slope s=-1 for all inclinations but with different projection parameter p that determines the vertical shift of the power law. Best fit for Mrk 110 (solid thick) yields $p\simeq 0.886$ that can be used to determine the inclination of the inner disk.
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In the text

$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig8.ps}} \end{figure}$ Figure 8: Variation of the projection parameter p with inclination i as computed from Kerr ray tracing. The numerical data points can be approximated by a cosine function (solid), $p(i)\sim 4.63~\cos(i)-3.13$ within 10% precision. p measurements from observations give inner disk inclinations. The cross marks the result for Mrk 110 based on K03 data: $i\sim (29.7\pm 1.2)^{\circ }$ .
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In the text

$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig9.ps}} \end{figure}$ Figure 9: Synoptical plot with optical K03 data for Mrk 110 (boxes) and best fitting Kerr ray tracing simulation with $i\sim 30^{\circ }$ (filled circles) as well as lapse functions for a static (Schwarzschild, solid) and rotating (Kerr, dotted) black hole. An essential statement illustrated here is that optical BLR lines can not probe black hole rotation due to their huge distance. Generally, multi-wavelength observations are recommended to fill the gap at smaller radii.
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In the text

$\begin{figure} \rotatebox{0}{\includegraphics[width=8.8cm,clip]{Figures/5615fig1.ps}} \end{figure}$	Figure 1: Radial dependence of redshift z of line cores (filled circles, left y-axis) and strength of gravitational redshift effect (triangles, right y-axis). Inclination angle amounts to $1^\circ$ .
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$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig2.ps}} \end{figure}$	Figure 2: Shift of line core energy in units of g-factor with distance to the black hole. Lowly inclined rings, $i=1^\circ$ , are compared to highly inclined rings, $i=75^\circ$ . Note the blueshift g > 1 in the latter case.
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$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig3.ps}} \end{figure}$	Figure 3: Two example relativistic lines emitted from a highly inclined ring, $i=75^\circ$ , and a face-on ring, $i=1^\circ$ , both with the emission peaking at the same $R_{\rm peak}=100.0 \ r_{\rm g}$ around a Kerr black hole with a/M=0.998. The arrows indicate the core g-factors, $g_{\rm core}\simeq 1.008$ and $g_{\rm core}\simeq 0.985$ respectively for each particular case.
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$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig4.ps}} \end{figure}$	Figure 4: Line distortion by strong gravity. The emission of narrow rings peaks at the radii as denoted in the legend. There is no way to confuse the lines because line flux successively decreases with decreasing radius of maximum emission $R_{\rm peak}$ . All rings follow Keplerian rotation around a Kerr black hole with a/M=0.998 and all are inclined to an inclination angle of $i=75^\circ$ .
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$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig6.ps}} \end{figure}$	Figure 6: Energetic distance of red and blue Doppler peak at $i=75^\circ$ . This Doppler peak spacing (DPS) is measured in units of g. Far away from the black hole both peaks approach significantly and the double-peaked line profile becomes very narrow: At $\sim$ $3000 \ {r_{\rm g}}$ the peak difference in g only amounts to $\sim$ 0.03.
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$\begin{figure} \rotatebox{0}{\includegraphics[width=9cm,clip]{Figures/5615fig8.ps}} \end{figure}$	Figure 8: Variation of the projection parameter p with inclination i as computed from Kerr ray tracing. The numerical data points can be approximated by a cosine function (solid), $p(i)\sim 4.63~\cos(i)-3.13$ within 10% precision. p measurements from observations give inner disk inclinations. The cross marks the result for Mrk 110 based on K03 data: $i\sim (29.7\pm 1.2)^{\circ }$ .
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