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All Figures

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295fig01.eps}}\end{figure}$ Figure 1: Sample H₂O maser spectra of RX Boo showing typical profiles starting in 1987 and ending in early 2007. Note the varying flux density scale.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8295fig02.eps}\end{figure}$ Figure 2: Flux density of the H₂O masers of RX Boo as a function of velocity and time. The time axis covers the years 1987-2007. The time stamp t=0 corresponds to 1987 March 30 (JD 2 446 885). The dotted horizontal lines mark the actual observations averaged in 4-day intervals. Flux densities in between the observations were interpolated linearly. The spectra were resampled to a resolution of 0.3 km s^-1. The dashed vertical line marks the stellar systemic velocity (1 km s^-1) as given by Teyssier et al. (2006). Contours are drawn at levels 3.00, 8.49, 24.03, 68.02, 192.51, 544.85 Jy (logarithmic scale). These six levels are indicated by black and white lines in the flux scale along the right side of the map. (For a colour version of this figure, see the electronic edition.)
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In the text

$\begin{figure} \par\includegraphics[width=13.4cm,clip]{8295fig03.eps}\end{figure}$ Figure 3: Sample H₂O maser images of RX Boo from 1990 February. Each image is separated from its neighbours by the line-of-sight velocity interval 0.658 km s^-1. The synthesised FWHM beam size (major axis: 0. $^{\prime \prime }$ 09; minor axis: 0. $^{\prime \prime }$ 08; position angle of the major axis: 86 $^\circ$ ) is shown in the uppermost left image (7.9 km s^-1). The images are oriented along right ascension and declination and the angular scales are relative to the position $\alpha=14^{\rm {h}}24^{\rm {m}}11\hbox{$.\!\!^{\rm s}$ }6$ , $\delta =+25\hbox {$^\circ $ }42\hbox {$^\prime $ }14\hbox {$^{\prime \prime }$ }$ (J2000). Brightness contours are -0.05 (dashed contour), 0.05, 0.5, 5, 50 Jy per beam area ( $1.45 \times 10^{-13}$ sr).
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In the text

$\begin{figure} \par\includegraphics[width=11cm]{8295fig04.eps}\end{figure}$ Figure 4: All the maser components listed in Table 3 plotted on the sky. Each component is represented by a symbol and a circle whose diameter is logarithmically proportional to the flux density of the component (see text for the mathematical expression). The epochs are represented by different symbols: 1990 February by small circles; 1990 June by asterisks; 1991 October by plus signs; 1992 December by crosses. The circles around the components are colour coded according to the line-of-sight velocity of the component ( $v_{\rm los}$ in the text). (For a colour version of this figure, see the electronic edition.) A circle (dashed) has been fitted to the components on the arc (see text for a detailed list of components) and the origin has been moved to the centre of this circle (Table 3). The filled dark red circle at the origin symbolises the central star with a diameter of 19 mas.
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In the text

$\begin{figure} \par\includegraphics[width=8.75cm,clip]{8295fig05.eps}\end{figure}$ Figure 5: The absolute value of the line-of-sight velocity relative to that of the star (1 km s^-1) plotted against the projected distance of all the spatial components listed in Table 3 from the origin (the central star). The epochs are represented by the same symbols as in Fig. 4. Five of the components (marked by surrounding circles) fit accurately to an ellipse (dotted line) centred on the origin and with its axes along the coordinate axes of the diagram. If the expansion of the stellar envelope is isotropic, this suggests that there exists an inner distance (14-16 AU) at a certain expansion velociy (4-6 km s^-1) where water vapour masers first appear in the expanding gas.
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In the text

$\begin{figure} \par\includegraphics[width=8.75cm,clip]{8295fig06.eps}\end{figure}$ Figure 6: The model expansion velocity as a function of the distance from the star (Eq. (3)). It approaches the terminal velocity (8.4 km s^-1) asymptotically (horizontal straight line). The dots along the expansion law curve symbolise the distances and velocities of the masercomponents.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{8295fig07.eps}\end{figure}$ Figure 7: The three-dimensional distribution of maser components and their associated velocities according to the expansion model given by Eq. (3). The distribution is seen from three cardinal directions: on the sky a), ``from the side'' b) and ``from above'' c). The maser components are represented by the same symbols as earlier. In addition the projected expansion velocities and the line-of-sight velocities are shown in the same scale in units of km s^-1 as the distance scale in units of AU.
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In the text

$\begin{figure} \includegraphics[width=9.5cm]{8295fig08a.eps} \includegraphics[width=9.5cm]{8295fig08b.eps}\end{figure}$ Figure 8: Flux density of the H₂O maser of SV Peg as a function of velocity and time. The time axis covers the years 1990-1995 ( bottom) and 2000-2007 ( top). The time stamp t=0 corresponds to 1990 February 17 (JD 2 447 933). The dotted horizontal lines mark the actual observations averaged in 4-day intervals. Flux densities in between the observations were interpolated linearly. The dashed vertical line marks the stellar systemic velocity (5 km s^-1) as given by Kerschbaum & Olofsson (1999). The spectra were resampled to a resolution of 0.3 km s^-1. Contours in the lower panel are drawn at levels 3.00, 4.19, 5.86, 8.18, 11.43, 15.97 Jy (logarithmic scale) and in the upper panel at 3.00, 4.40, 6.45, 9.45, 13.86, 20.32 Jy. These levels are indicated by black and white lines in the flux scales along the right side of the two maps. (For a colour version of this figure, see the electronic edition.)
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In the text

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295fig09.eps}}\end{figure}$ Figure 9: Sample H₂O maser spectra of SV Peg showing typical profiles starting in 1990 and ending in early 2007. Note the varying flux density scale.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=-90,clip]{8295fig10.eps}\end{figure}$ Figure 10: Optical AAVSO lightcurve and the lightcurve of the integrated H₂O maser emission for RX Boo during the years 1987-2007. The optical data are visual magnitudes and the integrated radio flux has been offset by an arbitrary amount.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8295fig11.eps}\end{figure}$ Figure 11: The observed flux density as a function of the absolute value of the aspect angle ( $\theta$ ). The epochs are represented by the same symbols as in Figs. 4 and 5.
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In the text

$\begin{figure} \par\includegraphics[width=4.5cm,angle=-90]{8295fig12a.eps}\\ [0.5cm] \includegraphics[width=4.5cm,angle=-90]{8295fig12b.eps}\end{figure}$ Figure 12: Upper envelope of all spectral profiles of RX Boo ( top) and SV Peg ( bottom). In RX Boo the spectra containing the flare (1995 January-May) were omitted. The flare occured at $\sim$ 3.5 km s^-1 close to the strongest peak in the upper envelope and reached a peak flux of 1600 Jy. The upper envelope is defined as the highest flux density ever achieved in velocity bins of 0.3 km s^-1 during the monitoring program.
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In the text

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295figA01.eps}}\end{figure}$ Figure A.1: H₂O maser spectra of RX Boo. Note the varying flux density scale.
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In the text

$\begin{figure}\par\resizebox{16cm}{!}{\includegraphics{8295figA02.eps}}\end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure}\par\resizebox{16cm}{!}{\includegraphics{8295figA03.eps}}\end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295figA04.eps}}\end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295figA05.eps}}\end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295figA06.eps}}\end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295figA07.eps}}\end{figure}$ Figure A.2: H₂O maser spectra of SV Peg. Note the varying flux density scale.
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In the text

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295figA08.eps}}\end{figure}$ Figure A.2: continued.
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In the text

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295figA09.eps}}\end{figure}$ Figure A.2: continued.
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In the text

$\begin{figure} \par\resizebox{6.03cm}{!}{\includegraphics{8295figA10.eps}}\end{figure}$ Figure A.2: continued.
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In the text

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295fig01.eps}}\end{figure}$	Figure 1: Sample H₂O maser spectra of RX Boo showing typical profiles starting in 1987 and ending in early 2007. Note the varying flux density scale.
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$\begin{figure} \par\includegraphics[width=8.75cm,clip]{8295fig06.eps}\end{figure}$	Figure 6: The model expansion velocity as a function of the distance from the star (Eq. (3)). It approaches the terminal velocity (8.4 km s^-1) asymptotically (horizontal straight line). The dots along the expansion law curve symbolise the distances and velocities of the masercomponents.
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$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295fig09.eps}}\end{figure}$	Figure 9: Sample H₂O maser spectra of SV Peg showing typical profiles starting in 1990 and ending in early 2007. Note the varying flux density scale.
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$\begin{figure} \par\includegraphics[width=7.5cm,angle=-90,clip]{8295fig10.eps}\end{figure}$	Figure 10: Optical AAVSO lightcurve and the lightcurve of the integrated H₂O maser emission for RX Boo during the years 1987-2007. The optical data are visual magnitudes and the integrated radio flux has been offset by an arbitrary amount.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{8295fig11.eps}\end{figure}$	Figure 11: The observed flux density as a function of the absolute value of the aspect angle ( $\theta$ ). The epochs are represented by the same symbols as in Figs. 4 and 5.
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$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295figA01.eps}}\end{figure}$	Figure A.1: H₂O maser spectra of RX Boo. Note the varying flux density scale.
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$\begin{figure}\par\resizebox{16cm}{!}{\includegraphics{8295figA02.eps}}\end{figure}$	Figure A.1: continued.
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$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295figA07.eps}}\end{figure}$	Figure A.2: H₂O maser spectra of SV Peg. Note the varying flux density scale.
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$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics{8295figA08.eps}}\end{figure}$	Figure A.2: continued.
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