All Figures

$\begin{figure} \par\includegraphics[width=8cm]{figure/8089fig1.ps}\end{figure}$ Figure 1: Distribution of the sample galaxies over the Hubble types ( left panel) and radial velocities with respect to the 3 K background ( right panel).
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In the text

$\begin{figure} \par\includegraphics[width=6cm,angle=90]{figure/8089fig2.ps}\end{figure}$ Figure 2: Comparison between the axis ratios ( left panel) and the position angles ( right panel) measured in this paper and by MH01. Filled dots and open diamonds correspond to values measured for bulges and disks, respectively. Residuals $\Delta q$ and $\rm\Delta PA$ are defined as $1 - q_{\rm ~ MH01}/q_{\rm our}$ and $\rm 1 - PA_{\rm MH01}/PA_{\rm our}$ , respectively.
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In the text

$\begin{figure} \par\includegraphics[width=12.7cm,clip]{figure/8089fig3.ps} \end{figure}$ Figure 3: Correlations between the bulge parameters. Correlation between the Hubble type and effective radius (A), effective surface brightness (B), and shape parameter (C). Correlations between the effective radius and shape parameter (D), effective surface brightness (E), and absolute magnitude (F). In each panel the solid line represent the linear regression through all the points. The Pearson correlation coefficient (r), and the results of the linear fit (y =a + bx) are also given.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fig4.ps}\end{figure}$ Figure 4: Edge-on view of the FP for the 98 early-to-intermediate type bulges of our sample with measured velocity dispersion. The solid line represents the linear fit to the data. The dotted lines represent the $1\sigma$ deviation from the fit. The error bars in the lower right corner of the panel indicate the mean errors of the data.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fig5.ps}\end{figure}$ Figure 5: FJ relation for the 98 early-to-intermediate type bulges of our sample with measured velocity dispersion. The solid line represents the linear fit to the data. The dotted lines represent the $1\sigma$ deviation from the fit. The error bars in the lower right corner of the panel indicate the mean errors of the data.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fig6.ps}\end{figure}$ Figure 6: Edge-on view of the PP for early-to-intermediate bulges of our sample. The solid line represents the linear fit to the data. The dotted lines represent the $1\sigma$ deviation from the fit. The error bars in the lower right corner of the panel indicate the mean errors of the data.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{figure/8089fig7.ps} \end{figure}$ Figure 7: Correlations between the disk parameters. Correlations between the Hubble type and disk scale length (A) and central surface brightness (B). Correlation between the disk scale length and absolute luminosity (C) and central surface brightness (D). Solid lines and coefficients as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=13.2cm,clip]{figure/8089fig8.ps} \end{figure}$ Figure 8: (A) Correlation between the disk scale length and central velocity dispersion for the 98 galaxies of our sample with a measured velocity dispersion. (B) Correlation between the disk scale length and bulge effective radius. (C) The ratio between the bulge and disk exponential scale lengths as a function of the bulge shape parameter. Filled circles and crosses represent the results of our measurements and simulations by Tissera et al. (2006), respectively. Solid lines and coefficients as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fig9.ps}\end{figure}$ Figure 9: Probability distribution function of E for the galaxy IC 4310. The dotted line represents the value of T=0.098 derived for this galaxy. The value of E_1/2 is also shown in the plot.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fi10.ps}\end{figure}$ Figure 10: PDF of T. The probability is normalized over 10 bins, which are geometrically distributed to cover the interval (0,1). The width of the first bin is 0.03 and the width ratio of two consecutive bins is 1.25. Error bars correspond to Poisson statistics.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fi11.ps}\end{figure}$ Figure 11: PDF of E. The probability is normalized over 10 bins, which are geometrically distributed to cover the interval (0,1). The width of the first bin is 0.03 and the width ratio of two consecutive bins is 1.25. The error bar of each P_k(E) bin corresponds to the Poisson statistics of 1000 realizations of P_k(T) after excluding non-physical cases.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{figure/8089fi12.ps}\end{figure}$ Figure 12: PDF of E for the different subsamples. (A) Lenticular galaxies ( $-3 \leq HT <0$ ). (B) Spiral galaxies ( $0 \leq HT \leq 3$ ). (C) Galaxies with $n\geq 2$ . (D) Galaxies with n< 2. (E) Faint bulges ( $M_{\rm b}\geq -22$ ). (F) Bright bulges ( $M_{\rm b}<-22$ ). Bin widths and error bars as in Fig. 11. The mean intrinsic ellipticity and the number of galaxies of the subsample are given in each panel.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fi13.ps}\end{figure}$ Figure 13: PDF of E for the original sample (solid lines), for a sample with 30% of bulges with a nuclear bar (dotted line) and for a 100% fraction of galaxies hosting a nuclear bar (dashed line). Bin widths and error bars as in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{figure/8089fig1.ps}\end{figure}$	Figure 1: Distribution of the sample galaxies over the Hubble types ( left panel) and radial velocities with respect to the 3 K background ( right panel).
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$\begin{figure} \par\includegraphics[width=6cm,angle=90]{figure/8089fig2.ps}\end{figure}$	Figure 2: Comparison between the axis ratios ( left panel) and the position angles ( right panel) measured in this paper and by MH01. Filled dots and open diamonds correspond to values measured for bulges and disks, respectively. Residuals $\Delta q$ and $\rm\Delta PA$ are defined as $1 - q_{\rm ~ MH01}/q_{\rm our}$ and $\rm 1 - PA_{\rm MH01}/PA_{\rm our}$ , respectively.
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$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fig4.ps}\end{figure}$	Figure 4: Edge-on view of the FP for the 98 early-to-intermediate type bulges of our sample with measured velocity dispersion. The solid line represents the linear fit to the data. The dotted lines represent the $1\sigma$ deviation from the fit. The error bars in the lower right corner of the panel indicate the mean errors of the data.
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$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fig5.ps}\end{figure}$	Figure 5: FJ relation for the 98 early-to-intermediate type bulges of our sample with measured velocity dispersion. The solid line represents the linear fit to the data. The dotted lines represent the $1\sigma$ deviation from the fit. The error bars in the lower right corner of the panel indicate the mean errors of the data.
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$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fig6.ps}\end{figure}$	Figure 6: Edge-on view of the PP for early-to-intermediate bulges of our sample. The solid line represents the linear fit to the data. The dotted lines represent the $1\sigma$ deviation from the fit. The error bars in the lower right corner of the panel indicate the mean errors of the data.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{figure/8089fig7.ps} \end{figure}$	Figure 7: Correlations between the disk parameters. Correlations between the Hubble type and disk scale length (A) and central surface brightness (B). Correlation between the disk scale length and absolute luminosity (C) and central surface brightness (D). Solid lines and coefficients as in Fig. 3.
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$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fig9.ps}\end{figure}$	Figure 9: Probability distribution function of E for the galaxy IC 4310. The dotted line represents the value of T=0.098 derived for this galaxy. The value of E_1/2 is also shown in the plot.
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$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fi10.ps}\end{figure}$	Figure 10: PDF of T. The probability is normalized over 10 bins, which are geometrically distributed to cover the interval (0,1). The width of the first bin is 0.03 and the width ratio of two consecutive bins is 1.25. Error bars correspond to Poisson statistics.
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$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fi11.ps}\end{figure}$	Figure 11: PDF of E. The probability is normalized over 10 bins, which are geometrically distributed to cover the interval (0,1). The width of the first bin is 0.03 and the width ratio of two consecutive bins is 1.25. The error bar of each P_k(E) bin corresponds to the Poisson statistics of 1000 realizations of P_k(T) after excluding non-physical cases.
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$\begin{figure} \par\includegraphics[width=7cm]{figure/8089fi13.ps}\end{figure}$	Figure 13: PDF of E for the original sample (solid lines), for a sample with 30% of bulges with a nuclear bar (dotted line) and for a 100% fraction of galaxies hosting a nuclear bar (dashed line). Bin widths and error bars as in Fig. 11.
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