All Figures

$\begin{figure} \par\includegraphics[angle=-90, width=7.9cm, clip]{2175fig1.ps} \end{figure}$ Figure 1: 22 GHz H₂O megamaser profiles toward Mrk 1066 with a channel spacing of 1.08 km s^-1. $\alpha _{2000}$ = 02 $^{\rm h}$ 59 $^{\rm m}$ 58 $~.\!\!^{\rm s}$ 6, $\delta _{2000} = 36 ^{\circ }$ 49 $^\prime$ 14 $^{\prime \prime }$ . Velocity scales are with respect to the Local Standard of Rest (LSR) and use the optical convention that is equivalent to cz. $V_{\rm sys} = {\rm c}z_{\rm sys} = 3605$ km s^-1 (NASA/IPAC Extragalactic Database (NED)). $V_{\rm LSR} - V_{\rm HEL} = -3.55$ km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.7cm]{2175fig2.ps} \end{figure}$ Figure 2: High spectral resolution profiles of the narrow maser spike in Mrk 1066 (see Fig. 1). The channel spacing is 0.067 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.5cm]{2175fig3.ps} \end{figure}$ Figure 3: Low velocity H₂O megamaser profiles toward Mrk 34 with a channel spacing of 4.65 km s^-1. $\alpha _{2000}$ = 10 $^{\rm h}$ 34 $^{\rm m}$ 08 $~.\!\!^{\rm s}$ 6, $\delta _{2000}$ = 60 $^{\circ }$ 01 $^\prime$ 52 $^{\prime \prime }$ . c $z_{\rm sys}$ = 15145 km s^-1 (de Grijp et al. 1992). $V_{\rm LSR}-V_{\rm HEL} = +5.23$ km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.5cm]{2175fig4.ps} \end{figure}$ Figure 4: High velocity megamaser feature toward Mrk 34 with a channel spacing of 18.65 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.8cm]{2175fig5.ps} \end{figure}$ Figure 5: H₂O kilomaser spectra toward NCG 3556 ( $\alpha _{2000} = 11 ^{\rm h}$ 11 $^{\rm m}$ 31 $~.\!\!^{\rm s}$ 2, $\delta _{2000} = 55$ $^{\circ }$ 40 $^\prime$ 25 $^{\prime \prime }$ ). Channel spacings are 4.2 km s^-1 ( upper panel) and 1.06 km s^-1. cz = 700 km s^-1 (NED). $V_{\rm LSR}-V_{\rm HEL} = +5.90$ km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.7cm]{2175fig6.ps} \end{figure}$ Figure 6: H₂O megamaser profile toward Arp 299 ( $\alpha _{2000} = 11$ $^{\rm h}$ 28 $^{\rm m}$ 31 $~.\!\!^{\rm s}$ 9, $\delta _{2000} = 58$ $^{\circ }$ 33 $^\prime$ 45 $^{\prime \prime }$ ). The channel spacing is 4.3 km s^-1. $V_{\rm LSR}-V_{\rm HEL} = +6.97$ km s^-1. For radial velocities, see Sect. 4.2.3.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=16.2cm]{2175fig7.ps} \end{figure}$ Figure 7: H₂O megamaser profiles toward Arp 299, taken on Jan. 30, 2004, during a night with excellent pointing conditions. The reference position is $\alpha _{2000} = 11 ^{\rm h}$ 28 $^{\rm m}$ 31 $~.\!\!^{\rm s}$ 9, $\delta _{2000} = 58^{\circ }$ 33 $^\prime$ 45 $^{\prime \prime }$ . Offsets in arcsec ( $\Delta \alpha$ , $\Delta \delta$ ) are given in the upper right corner of each box. Spectra with offsets $\Delta \alpha = -20$ $^{\prime \prime }$ trace emission from the "overlap'' region (north) and NGC 3690 (south). Spectra with $\Delta \alpha = +20$ $^{\prime \prime }$ are sensitive to emission from IC 694 (see Sect. 4.2.3). The channel spacing is 16.8 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=8.3cm]{2175fig8.ps} \end{figure}$ Figure 8: Detection rate of the H₂O FIR-maser sample (see Table 2 for the targets and Sect. 1 for selection criteria) including all galaxies exceeding a given IRAS Point Source Catalog $S_{\rm 100~\mu m}$ flux density.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=6.5cm]{2175fig9.ps} \end{figure}$ Figure 9: IRAS Point Source FIR luminosity versus total H₂O luminosity of H₂O detected galaxies (cf. Table 4). For NGC 2146, the total logarithmic H₂O luminosity is 0.9 in solar units (Tarchi et al. 2002a). Stars denote the ten sources belonging to the FIR selected maser sample. The diagonal line shows the correlation found by Jaffe et al. (1981) for individual galactic star forming regions.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.4cm]{2175fig10.ps} \end{figure}$ Figure 10: The 22 GHz H₂O luminosity function (LF) for maser galaxies beyond the Magellanic Clouds (Table 4). The filled circles show the LF for a detection limit of 0.2 Jy km s^-1. The dashed line shows a fit with a slope of -1.3 (for uncertainties in the slope, see Sect. 4.3.2). Error bars of individual points are derived from Poisson statistics following Condon (1989). Not included in the diagram are IC 342 (too low maser luminosity) and UGC 3255, Mrk 3, Mrk 78, NGC 4151, NGC 5256 and NGC 6240 (below the adopted detection limit). The number of masing galaxies in each bin are also shown. To illustrate the effect of changing the sensitivity, we also show the LF for a detection limit of 1 Jy km s^-1 (empty circles; in this case 19 of the 53 galaxies fall below the detection limit).
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.7cm]{2175fig2.ps} \end{figure}$	Figure 2: High spectral resolution profiles of the narrow maser spike in Mrk 1066 (see Fig. 1). The channel spacing is 0.067 km s^-1.
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$\begin{figure} \par\includegraphics[angle=-90, width=7.5cm]{2175fig3.ps} \end{figure}$	Figure 3: Low velocity H₂O megamaser profiles toward Mrk 34 with a channel spacing of 4.65 km s^-1. $\alpha _{2000}$ = 10 $^{\rm h}$ 34 $^{\rm m}$ 08 $~.\!\!^{\rm s}$ 6, $\delta _{2000}$ = 60 $^{\circ }$ 01 $^\prime$ 52 $^{\prime \prime }$ . c $z_{\rm sys}$ = 15145 km s^-1 (de Grijp et al. 1992). $V_{\rm LSR}-V_{\rm HEL} = +5.23$ km s^-1.
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$\begin{figure} \par\includegraphics[angle=-90, width=7.5cm]{2175fig4.ps} \end{figure}$	Figure 4: High velocity megamaser feature toward Mrk 34 with a channel spacing of 18.65 km s^-1.
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$\begin{figure} \par\includegraphics[angle=-90, width=7.8cm]{2175fig5.ps} \end{figure}$	Figure 5: H₂O kilomaser spectra toward NCG 3556 ( $\alpha _{2000} = 11 ^{\rm h}$ 11 $^{\rm m}$ 31 $~.\!\!^{\rm s}$ 2, $\delta _{2000} = 55$ $^{\circ }$ 40 $^\prime$ 25 $^{\prime \prime }$ ). Channel spacings are 4.2 km s^-1 ( upper panel) and 1.06 km s^-1. cz = 700 km s^-1 (NED). $V_{\rm LSR}-V_{\rm HEL} = +5.90$ km s^-1.
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$\begin{figure} \par\includegraphics[angle=-90, width=7.7cm]{2175fig6.ps} \end{figure}$	Figure 6: H₂O megamaser profile toward Arp 299 ( $\alpha _{2000} = 11$ $^{\rm h}$ 28 $^{\rm m}$ 31 $~.\!\!^{\rm s}$ 9, $\delta _{2000} = 58$ $^{\circ }$ 33 $^\prime$ 45 $^{\prime \prime }$ ). The channel spacing is 4.3 km s^-1. $V_{\rm LSR}-V_{\rm HEL} = +6.97$ km s^-1. For radial velocities, see Sect. 4.2.3.
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$\begin{figure} \par\includegraphics[angle=-90, width=8.3cm]{2175fig8.ps} \end{figure}$	Figure 8: Detection rate of the H₂O FIR-maser sample (see Table 2 for the targets and Sect. 1 for selection criteria) including all galaxies exceeding a given IRAS Point Source Catalog $S_{\rm 100~\mu m}$ flux density.
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