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$\begin{figure} \par\resizebox{8.8cm}{!}{ \includegraphics[clip]{ms2277_fig1.ps}}\end{figure}$ Figure 1: Detection rate of 15 GHz 150-mas-scale radio nuclei for "L''INERs, "S''eyferts, and "T''ransition nuclei in the Palomar sample. The total number of objects is shown by the upper histogram and the number detected is shown by the grey-shaded histogram. Note the higher detection rates of type 1 (i.e. galaxies with broad H $\alpha$ emission) Seyfert and LINER nuclei.
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In the text

$\begin{figure} \par\resizebox{\textwidth}{!}{ \includegraphics[bb=75 220 560 70... ...ig2d.ps} \includegraphics[bb=75 220 560 700,clip]{ms2277_fig2e.ps}}\end{figure}$ Figure 2: 5 GHz (6 cm) VLBA maps of ( left to right) NGC 2273, NGC 4589, NGC 5353, NGC 5363, and NGC 7626. The contours are integer powers of $\sqrt {2}$ , multiplied by the $2~\sigma$ noise level of 0.25 mJy (0.3 mJy in the case of NGC 5353). The peak flux-densities are 20.6, 6.1, 13.7, 26.1, and 19.0 mJy/beam, respectively. Tick marks are every 2 mas except for NGC 5353 and NGC 5363 (5 mas).
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In the text

$\begin{figure} \par {\resizebox{\textwidth}{!}{ \includegraphics[width=16.5cm,clip]{ms2277_fig3.ps}} } \end{figure}$ Figure 3: A plot of the log of the 15 GHz nuclear (150 mas resolution) radio luminosity versus nuclear H $\alpha$ +[N II] $\lambda \lambda$ 6548,6583 luminosity for all LLAGNs and AGNs in the Palomar sample in elliptical ( left) and non-elliptical ( right) host galaxies. In both panels, Seyferts, LINERs, and transition nuclei from the Palomar sample are shown as triangles, circles, and squares, respectively. For these, filled symbols are used for radio detected nuclei and open symbols are used for upper limits to the radio luminosity. For comparison, radio-detected "classical'' Seyfert galaxies (from Whittle 1992a, i.e. not from the Palomar Sample) are plotted as crosses in both panels, regardless of their galaxy morphological type (for these the [O III] luminosity was converted to an H $\alpha$ +[N II] luminosity using standard flux ratios for Seyferts; see Nagar et al. 2002a). Also shown are the low-luminosity extrapolations of linear fits to the same relationship for FR I and FR II radio galaxies (dashed lines; Zirbel & Baum 1995).
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In the text

$\begin{figure} \par {\resizebox{15cm}{!}{ \includegraphics{ms2277_fig4.ps}} } \end{figure}$ Figure 4: A plot of sub-parsec radio luminosity versus ( left) black hole mass and ( right) bulge luminosity of the host galaxy in the B-band. Only radio-detected sources relatively unambiguously identified with the central engine of the AGN (see text) and with radio fluxes measured at resolution better than 1 pc are plotted as circles (Palomar LLAGNs and AGNs) and triangles (other LLAGNs and AGNs). For these, filled symbols are used for elliptical galaxies, and errors in black hole mass are shown (see text). LLAGNs and AGNs (some of which are in the Palomar sample) with radio luminosities measured at resolution between 1 pc and 5 pc are shown as crosses. Two measurements (at different resolutions; Nagar et al. 2002a) are plotted for the Galaxy. The four dotted lines in the left panel represent Eddington ratios (from 10^-6 to 1) calculated assuming that jet kinetic power dominates the accretion energy output (see Sect. 5.5). The dashed line in the left panel shows a linear fit to the circles and triangles with log $M_{\rm BH}$ > 10⁷ $M_{\odot }$ ; the dashed line in right panel shows a linear fit to the circles and triangles except the Galaxy (see text).
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In the text

$\begin{figure*} \par\resizebox{15cm}{!}{ \includegraphics[clip]{ms2277_fig5a.ps}\hspace*{4mm} \includegraphics[clip]{ms2277_fig5b.ps} }\end{figure*}$ Figure 5: a) The 15 GHz radio luminosity function (RLF) of the 150 mas-scale radio nuclei in the LLAGNs and AGNs of the Palomar sample (open circles, with the number of galaxies in each bin listed above the symbol). For a rough comparison (see text) we also plot the 15 GHz RLFs (after converting to our value of H₀ and frequency; see text) of Markarian Seyferts and CfA Seyferts. The dotted line is a power-law (-0.78) fit to the Palomar nuclear RLF (excluding the two lowest radio luminosity points). Also shown is the estimated 15 GHz nuclear RLF of galaxies in the local group (open square, with 2 galaxies; see text). The upper x axes of both panels show the implied logarithm of the mass accretion rate (in $M_{\odot }$ yr^-1) within the context of a jet model (Falcke & Biermann 1999), assuming both a 10% energy conversion efficiency, and that the jet kinetic power dominates the accretion energy output (see Sect. 5.5); b) the axes and open symbols are the same as in a). The filled symbols show several simulated nuclear RLFs for the Palomar sample which include nuclei not detected in our 15 GHz survey in the RLF calculation (see text for details). The dotted line with slope -0.43 shows a possible fit (made by eye) to the RLF at the lowest luminosities; the other dotted line is the same as in the left panel.
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In the text

$\begin{figure} \par\resizebox{7.7cm}{!}{ \includegraphics{ms2277_fig6.ps} }\end{figure}$ Figure 6: Left: the implied "minimum jet power'', ( $Q_{\rm jet}$ ) of the radio-detected (grey shaded area) and radio non-detected (white area) LLAGNs and AGNs, calculated from the peak VLA 15 GHz flux using Eq. (20) of Falcke & Biermann (1999) and assuming a jet inclination of 45 $^\circ$ to the line of sight. The inset illustrates the range of calculated minimum jet kinetic powers for three assumed inclinations: 20 $^\circ$ , 45 $^\circ$ , and 70 $^\circ$ . Right: log of the ratio of minimum jet power (assuming 45 $^\circ$ jet inclination) to X-ray luminosity (in the 2-10 keV band) for radio detected LLAGNs and AGNs. The grey and white histograms represent LLAGNs/AGNs with detected, and upper limits to, the hard X-ray emission, respectively.
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In the text

$\begin{figure} \par\resizebox{7.7cm}{!}{ \includegraphics{ms2277_fig7.ps} }\end{figure}$ Figure 7: A comparison of the kinetic and radiated accretion power outputs as a fraction of $L_{\rm Eddington}$ in four energetically important wavebands. In both panels the histograms are offset by 0.1 in x for clarity. Left: histograms of the broad H $\alpha$ luminosity (dotted line), hard X-ray luminosity (2-10 keV; dashed line), and minimum jet power ( $Q_{\rm jet}$ ; solid line) for all broad line nuclei, all hard X-ray detected nuclei, and all radio detected nuclei, among the LLAGNs and AGNs of the Palomar Sample, respectively. Right: histograms of the minimum jet power ( $Q_{\rm jet}$ ; solid line) and radiated bolometric luminosity (derived from the [O III] luminosity, see text; dashed line) for the radio detected nuclei in the LLAGNs and AGNs of the Palomar Sample.
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In the text

$\begin{figure} \par\resizebox{10cm}{!}{ \includegraphics{ms2277_fig8.ps} }\end{figure}$ Figure 8: A plot of Jet Power (we use the "minimum jet power'', $Q_{\rm jet}$ , derived from the nuclear radio luminosity; see text) versus the Narrow Line Region (NLR) luminosity (derived from the [O III] luminosity; see text) for radio-detected nuclei in the Palomar Sample (circles). Filled circles are used for elliptical galaxies in the Palomar sample. These Palomar Sample LLAGNs and AGNs nicely fill in the low luminosity end of similar relationships for FR I and FR II radio galaxies (slanted crosses; Rawlings & Saunders 1991, with jet kinetic energy estimated from their kpc-scale radio lobes), and other radio galaxies (crosses; Celotti & Fabian 1993, with jet kinetic energy estimated from their parsec-scale radio jets). The data from other papers have been corrected to the value of H₀ used in this paper.
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In the text

$\begin{figure} \par\resizebox{6.7cm}{!}{ \includegraphics{ms2277_fig9.ps} }\end{figure}$ Figure 9: A comparison of the "minimum jet power'' ( $Q_{\rm jet}$ ) and the kinetic energy injected into the ISM by supernovae type I and II for the radio detected Palomar LLAGNs and AGNs. Filled circles are used for elliptical galaxies. The solid line shows the line of equality.
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In the text

$\begin{figure} \par\resizebox{14.5cm}{!}{ \includegraphics{ms2277_fig10.ps}}\end{figure}$ Figure 10: Plots of the "minimum jet power'' as a fraction of Eddington luminosity (equivalent to the Eddington ratio, ${l_{\rm Edd}}$ , if the jet power dominates the emitted accretion energy) versus a) the nuclear H $\alpha$ +[N II] $\lambda \lambda$ 6548,6583 luminosity; b) the 15 GHz nuclear (150 mas resolution) radio luminosity; and c) ratio of the above two quantities, for all radio-detected LLAGNs and AGNs in the Palomar sample. Seyferts are plotted as triangles, LINERs as circles, and transition nuclei as squares. Filled symbols are used for elliptical galaxies.
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In the text

$\begin{figure} \par\resizebox{5.7cm}{!}{ \includegraphics{ms2277_fig11.ps}}\end{figure}$ Figure 11: The cumulative number of "definite'' (solid lines for nuclei with a hard X-ray nuclear source and dashed lines for type 1 nuclei, i.e. with broad H $\alpha$ emission) AGNs identified by optical spectroscopy (upper two lines; $\sim$ 30 min to 1 h on the Palomar 5 m) and radio imaging (lower two lines; $\sim$ 10-15 min at the VLA), as a function of the luminosity of the narrow H $\alpha$ line.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{ \includegraphics[clip]{ms2277_fig1.ps}}\end{figure}$	Figure 1: Detection rate of 15 GHz 150-mas-scale radio nuclei for "L''INERs, "S''eyferts, and "T''ransition nuclei in the Palomar sample. The total number of objects is shown by the upper histogram and the number detected is shown by the grey-shaded histogram. Note the higher detection rates of type 1 (i.e. galaxies with broad H $\alpha$ emission) Seyfert and LINER nuclei.
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$\begin{figure} \par\resizebox{6.7cm}{!}{ \includegraphics{ms2277_fig9.ps} }\end{figure}$	Figure 9: A comparison of the "minimum jet power'' ( $Q_{\rm jet}$ ) and the kinetic energy injected into the ISM by supernovae type I and II for the radio detected Palomar LLAGNs and AGNs. Filled circles are used for elliptical galaxies. The solid line shows the line of equality.
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