All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{0150f1.ps} \end{figure}$ Figure 1: Distribution in redshift and luminosity of 95 known AGNs detected in the RXTE slew survey, including 77 emission-line AGNs (solid circles) and 18 blazars (open squares).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0150f2.ps} \end{figure}$ Figure 2: Comparison of the absorption columns estimated from the XSS 8-20 keV/3-8 keV count rate ratio, assuming a $\Gamma =1.8$ power-law intrinsic spectrum, with those derived through spectral analaysis of RXTE/PCA pointed observations for Seyfert 2 galaxies with a significant XSS detection of neutral absorption. The error bars are 1 $\sigma$ statistical uncertainties.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0150f3.ps} \end{figure}$ Figure 3: Upper panel: observed distribution in intrinsic absorption column density ( $N_{{\rm H}}$ ) of emission-line AGNs in our sample. Lower panel: estimated $N_{{\rm H}}$ distribution of the unidentified XSS sources, AGN candidates. Two different histograms are presented, one computed by adopting $N_{{\rm H}}=0$ in those cases where the measured $N_{{\rm H}}$ value is smaller than the 1 $\sigma$ statistical uncertainty, and the other computed using the best-fit $N_{{\rm H}}$ values, regardless of their errors.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{0150f4.ps} \end{figure}$ Figure 4: Relative volume of space probed by the RXTE slew survey with respect to AGNs of given intrinsic (unabsorbed) luminosity with a $\Gamma =1.8$ power-law intrinsic spectrum as a function of absorption column density. The solid and dashed lines correspond to the 3-20 keV and 8-20 keV bands, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0150f5.ps} \end{figure}$ Figure 5: Physical distribution in absorption column density of Compton-thin emission-line AGNs inferred from the XSS AGN sample. The error bars in this and subsequent figures represent 1 $\sigma$ statistical uncertainties.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0150f6.ps} \end{figure}$ Figure 6: Upper panel: AGN absorption column density distribution inferred from the northern (filled circles) and southern (open circles) subsamples of identified AGNs. Lower panel: $N_{{\rm H}}$ distribution estimated for the unidentified XSS sources, assuming that they are AGNs. One estimate (filled circles) is obtained by adopting $N_{{\rm H}}=0$ in those cases where the measured $N_{{\rm H}}$ value is smaller than the 1 $\sigma$ statistical uncertainty, another one (open circles) is based on the measured $N_{{\rm H}}$ values. The different sets of data points are slightly shifted relative to each other along the horizontal axis for better visibility.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0150f7.ps} \end{figure}$ Figure 7: Absorption column density distribution of emission-line AGNs with luminosity L_3-20<10^43.5 erg s^-1 (filled circles) and L_3-20>10^43.5 erg s^-1 (open circles).
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{0150f8.ps} \end{figure}$ Figure 8: Local 3-20 keV luminosity functions obtained here for (i) Compton-thin ( $N_{{\rm H}}<10^{24}$ cm^-2) non-blazar AGNs: in binned form (solid circles with 1 $\sigma$ error bars) and an analytic approximation (thick solid curve) given by Eq. (3) with parameter values quoted in Table 3, (ii) similarly for unabsorbed ( $N_{{\rm H}}<10^{22}$ cm^-2) non-blazar AGNs (open circles and thin solid curve), and (iii) for blazars (open squares within wider bins, no analytic fit is presented). The second set of data points is slighlty shifted along the luminosity axis for better visibility. For comparison are presented previous estimates of the local 2-10 keV AGN luminosity function, recomputed here to the 3-20 keV band and to our adopted value H₀=75 km s^-1 Mpc^-1: by Piccinotti et al. (1982) (dash-dotted curve), by Ueda et al. (2003) (for Compton-thin sources, dotted curve) and by La Franca et al. (2002) (for unabsorbed sources, dashed curve).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0150f9.ps} \end{figure}$ Figure 9: Contribution of AGNs with various luminosities to the local 3-20 keV volume emissivity, estimated from the binned luminosity functions presented in Fig. 8: of Compton-thin non-blazar AGNs (filled circles), of unabsorbed non-blazar AGNs (open circles), and of blazars (open squares).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0150f10.ps} \end{figure}$ Figure 10: 3-20 keV luminosity functions of local Compton-thin non-blazar AGNs inferred from the southern subsample (filled circles) and northern subsample (open circles), in comparison with the best-fit model (Eq. (3), Table 3) found for the whole AGN sample (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{0150f11.ps} \end{figure}$ Figure 11: $V/V_{{\rm m}}$ ratio averaged over luminosity bins for the whole XSS AGN sample. The error bars represent 1 $\sigma$ statistical uncertainties.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{0150f12.ps} \end{figure}$ Figure 12: Local 8-20 keV luminosity functions obtained here for Compton-thin ( $N_{{\rm H}}<10^{24}$ cm^-2) non-blazar AGNs: in binned form (solid circles with 1 $\sigma$ error bars) and an analytic approximation (thick solid curve) given by Eq. (3) with parameter values quoted in Table 3, and for unabsorbed ( $N_{{\rm H}}<10^{22}$ cm^-2) non-blazar AGNs (open circles, no analytic fit is presented).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0150f1.ps} \end{figure}$	Figure 1: Distribution in redshift and luminosity of 95 known AGNs detected in the RXTE slew survey, including 77 emission-line AGNs (solid circles) and 18 blazars (open squares).
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0150f2.ps} \end{figure}$	Figure 2: Comparison of the absorption columns estimated from the XSS 8-20 keV/3-8 keV count rate ratio, assuming a $\Gamma =1.8$ power-law intrinsic spectrum, with those derived through spectral analaysis of RXTE/PCA pointed observations for Seyfert 2 galaxies with a significant XSS detection of neutral absorption. The error bars are 1 $\sigma$ statistical uncertainties.
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{0150f4.ps} \end{figure}$	Figure 4: Relative volume of space probed by the RXTE slew survey with respect to AGNs of given intrinsic (unabsorbed) luminosity with a $\Gamma =1.8$ power-law intrinsic spectrum as a function of absorption column density. The solid and dashed lines correspond to the 3-20 keV and 8-20 keV bands, respectively.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0150f5.ps} \end{figure}$	Figure 5: Physical distribution in absorption column density of Compton-thin emission-line AGNs inferred from the XSS AGN sample. The error bars in this and subsequent figures represent 1 $\sigma$ statistical uncertainties.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0150f7.ps} \end{figure}$	Figure 7: Absorption column density distribution of emission-line AGNs with luminosity L_3-20<10^43.5 erg s^-1 (filled circles) and L_3-20>10^43.5 erg s^-1 (open circles).
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0150f9.ps} \end{figure}$	Figure 9: Contribution of AGNs with various luminosities to the local 3-20 keV volume emissivity, estimated from the binned luminosity functions presented in Fig. 8: of Compton-thin non-blazar AGNs (filled circles), of unabsorbed non-blazar AGNs (open circles), and of blazars (open squares).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0150f10.ps} \end{figure}$	Figure 10: 3-20 keV luminosity functions of local Compton-thin non-blazar AGNs inferred from the southern subsample (filled circles) and northern subsample (open circles), in comparison with the best-fit model (Eq. (3), Table 3) found for the whole AGN sample (solid line).
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{0150f11.ps} \end{figure}$	Figure 11: $V/V_{{\rm m}}$ ratio averaged over luminosity bins for the whole XSS AGN sample. The error bars represent 1 $\sigma$ statistical uncertainties.
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