All Figures

$\begin{figure} \par\includegraphics[angle=270,width=6.5cm,clip]{9312fig1.eps}\end{figure}$ Figure 1: Slit positions for the Phoenix off-star observations of R Hya. All off-star slits are positioned at 1 $^{\prime \prime }$ from the star. In the figure, the slits are shifted for reasons of clarity. The number of each data set as used in the logbook (Table A.1) is indicated.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{9312fig2.ps}\end{figure}$ Figure 2: The low-resolution ISO-SWS spectrum ( $R \sim 100$ ) in the 4 to 7 $\mu$ m wavelength range. The width of the box denotes the observed spectral range of the Phoenix spectrometer. The inset shows the full ISO-SWS spectrum between 2.38 and 45.2 $\mu$ m in the ( $\lambda \times F_{\lambda }$ )-space illustrating the absence of the 10 $\mu$ m silicate feature.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{9312fig3.eps}\end{figure}$ Figure 3: Comparison between the ISO-SWS spectrum of R Hya and theoretical model spectra computed with the MARCS code. The black curve represents the ISO-SWS spectrum, the purple curve a MARCS spectrum at ${T}_{\rm eff}$ = 2600 K and angular diameter ad = 29 mas, the red curve at ${T}_{\rm eff}$ = 2800 K and ad = 27 mas, and the green curve at ${T}_{\rm eff}$ = 3000 K and ad = 25 mas. The inset shows a comparison between the ISO-SWS spectrum of R Hya (black), the theoretical spectrum with ${T}_{\rm eff}$ = 2800 K and the SCAN H₂O linelist of Jørgensen et al. (2001) (red) and the theoretical spectrum with ${T}_{\rm eff}$ = 2800 K and the H₂O linelist of Partridge & Schwenke (1997) (blue).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{9312fig4.ps}\end{figure}$ Figure 4: Comparison between the on-star Phoenix spectrum of R Hya and the theoretical MARCS model spectrum computed with the SCAN H₂O linelist (red) and the AMES H₂O linelist (green) at a ${T}_{\rm eff}$ of 2800 K and an angular diameter of 27 mas. The three photospheric CO R(1), R(2), and R(3) lines are indicated. Telluric H₂O and CO lines are marked with a `` $\oplus$ '' symbol. The stellar CO lines are shifted out of the telluric ones, with a geocentric radial velocity of -32.3 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9312fig5.eps}\end{figure}$ Figure 5: Off-star (full line) and on-star (dashed line) spectrum of R Hya. The three off-star CO vibration-rotation emission lines, which are marked R(1), R(2), and R(3), are partly filled in by emission from the circumstellar CO lines compared to the on-star observations. Telluric CO lines are at 2150.86, 2154.60 and 2158.30 cm^-1, telluric H₂O lines at 2152.50 and 2156.50 cm^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9312fig6.eps}\end{figure}$ Figure 6: The resulting circumstellar CO vibration-rotation flux from the wind of R Hya for data set 128, being a EW-slit N1 E2.5. The intensity is integrated over the full slit area.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9312fig7.eps}\end{figure}$ Figure 7: Set of emission spectra at the east-position from R Hya (data set 142, being a NS-slit E1 S2.5). The spectra are shifted vertically for reasons of clarity. The top spectrum is measured closest to the star, i.e., at $\beta$ = 1 $^{\prime \prime }$ . The subsequent spectra are measured at 1.1 $^{\prime \prime }$ , 1.6 $^{\prime \prime }$ and 2.4 $^{\prime \prime }$ from the star.
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In the text

$\begin{figure} \par\mbox{\subfigure{\includegraphics[width=8cm,clip]{9312fig8a} ... ....5cm} \subfigure{\includegraphics[width=8cm,clip]{9312fig8b.eps} }} \end{figure}$ Figure 8: Decline of the intensity of the circumstellar emission as a function of angular distance $\beta$ in the four slits positioned 1 $^{\prime \prime }$ to the north of R Hya. Left: the decline of the intensity of the four data sets 112 (EW-slit N1 E2.5), 113 (EW-slit N1 W2.5), 127 (EW-slit N1 W2.5), and 128 (EW-slit N1 E2.5) is displayed. Right: mean (and standard deviation) of the intensity decline of the four north-east (NE) and north-west (NW) scans.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9312fig9.eps}\end{figure}$ Figure 9: Decline of the intensity of the circumstellar emission as a function of the angular distance $\beta$ from the star for eight scan directions. The statistical error bars have been omitted for reasons of clarity. Note that data set 149 (NS-slit W1 N2.5) and 15 (NS-slit W1 S2.5) are omitted (see text for more details). The black line represents the mean (and standard deviation) of the eight scan directions.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{9312fig10.ps}\end{figure}$ Figure 10: CO rotational line profiles of R Hya (plotted in grey, see Table 1) compared with (i) black dotted line: the model predictions based on the parameters as given by Wannier & Sahai (1986), who derived a constant mass loss of $\dot{M}$ $\sim$ $1 \times 10^{-7}$ $M_{\odot }$ yr^-1 using a distance of 130 pc; (ii) full black line: the best-fit model with parameters as specified in Table 3; and (iii) black dashed line: the best-fit model scaled to the observations to illustrate the similarity in line profiles. This scaling is performed only for the IRAM and JCMT data (see text for more details). The rest frame of the velocity scale is the local standard of rest (LSR) velocity.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{9312fig11.ps}\end{figure}$ Figure 11: Dependence of the mean of the scattered wavelength-integrated intensity of the circumstellar CO vibration-rotation lines on the angular distance on the sky, $\beta$ . The full black line represents a $\beta ^{-1.75}$ power law, the dashed line a $\beta ^{-3}$ power law.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{9312fig12.ps}\end{figure}$ Figure 12: Decline of the theoretically predicted integrated intensity (in erg s^-1 cm^-2 arcsec^-2) of the circumstellar CO vibration-rotation emission as a function of angular distance $\beta$ from the star. The full black line represents the GASTRoNOoM-predictions, the dashed black line represents the best-fit power law ( $I \propto \beta ^{a}$ ), with the exponent a specified in each panel. Upper panel: adopting a constant mass-loss rate, with same parameters as in Fig. 10. Lower panel: the best-fit model having a variable mass-loss rate with parameters as listed in Table 3. The grey line represents the decline of the overall mean of the data, the triangles show the behaviour in the NE-direction, and the diamonds that in the NW-direction.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{9312fig13.ps}\end{figure}$ Figure 13: Upper: estimated temperature profile, middle: estimated velocity structure, and bottom: estimated mass-loss rate $\dot{M}$ (r) for R Hya as a function of radial distance to the star (black line). The shading region in the bottom panel displays the confidence intervals of the estimated mass-loss parameters. The dashed line indicates $R_{\rm {inner}}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16cm,clip]{9312fig14.ps}\par\end{figure}$ Figure 14: The CO vibra-rotational R(1), R(2), R(3) lines observed at different angular distance from the star (black) are compared with the theoretical model predictions (red) for the best-fit model with parameters as specified in Table 3. The displayed off-star data are for data set 128 (EW-slit N1 E2.5).
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In the text

$\begin{figure} \par\mbox{\subfigure[The CO~emission lines of data set~112, being... ...ludegraphics[width=7cm,height=4.6cm,angle=0]{9312figA1d.eps} }} \par\end{figure}$ Figure A.1: The CO vibration-rotation emission lines north of R Hydrae, integrated over the slit.
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In the text

$\begin{figure} \par\mbox{\subfigure[The CO~emission lines of data set~116, being... ...ludegraphics[width=7cm,height=4.6cm,angle=0]{9312figA2d.eps} }} \par\end{figure}$ Figure A.2: The CO vibration-rotation emission lines south of R Hydrae, integrated over the slit.
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In the text

$\begin{figure} \par\mbox{\subfigure[The CO~emission lines of data set~141, being... ...\includegraphics[width=7cm,height=4.6cm,angle=0]{9312figA3d.eps} }} \end{figure}$ Figure A.3: The CO vibration-rotation emission lines east of R Hydrae, integrated over the slit.
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In the text

$\begin{figure} \par\mbox{\subfigure[The CO~emission lines of data set~149, being... ...ludegraphics[width=7cm,height=4.6cm,angle=0]{9312figA4d.eps} }} \par\end{figure}$ Figure A.4: The CO vibration-rotation emission lines west of R Hydrae, integrated over the slit.
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In the text

$\begin{figure} \par\mbox{\subfigure{\includegraphics[width=8cm,clip]{9312figA5a.... ...5cm} \subfigure{\includegraphics[width=8cm,clip]{9312figA5b.eps} }} \end{figure}$ Figure A.5: Decline of the intensity of the circumstellar emission as a function of angular distance $\beta$ in the four slits positioned 1 $^{\prime \prime }$ to the south of R Hya. Left: the decline of the intensity of the four data sets 116, 117, 123, and 124. Right: mean (and standard deviation) of the intensity decline of the four south-east (SE) and south-west (SW) scans.
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In the text

$\begin{figure} \par\mbox{\subfigure{\includegraphics[width=8cm,clip]{9312figA6a.... ...5cm} \subfigure{\includegraphics[width=8cm,clip]{9312figA6b.eps} }} \end{figure}$ Figure A.6: Decline of the intensity of the circumstellar emission as a function of angular distance $\beta$ in the four slits positioned 1 $^{\prime \prime }$ to the east of R Hya. Left: the decline of the intensity of the four data sets 141, 142, 158, and 161. Right: mean (and standard deviation) of the intensity decline of the four east-north (EN) and east-south (ES) scans.
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In the text

$\begin{figure} \par\mbox{\subfigure{\includegraphics[width=8cm,clip]{9312figA7a.... ...5cm} \subfigure{\includegraphics[width=8cm,clip]{9312figA7b.eps} }} \end{figure}$ Figure A.7: Decline of the intensity of the circumstellar emission as a function of angular distance $\beta$ in the four slits positioned 1 $^{\prime \prime }$ to the west of R Hya. Left: the decline of the intensity of the four data sets 149, 150, 159, and 160. Right: mean (and standard deviation) of the intensity decline of the four west-north (WN) and west-south (WS) scans.
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In the text

$\begin{figure} \par\mbox{\subfigure{\includegraphics[width=8cm,clip]{9312figA8a.... ...5cm} \subfigure{\includegraphics[width=8cm,clip]{9312figA8b.eps} }} \end{figure}$ Figure A.8: Decline of the intensity of the circumstellar CO emission in the south-west and west-south directions of R Hya. Left: mean of the (116, 117, 123, 124) and (149, 150, 159, 160) data sets is displayed. At the cross-over points around 1.4 $^{\prime \prime }$ from the star, the west-south data are significantly higher than for the south-west scan, due to the higher intensity values of the (149, 150) data sets. Right: data sets (149, 150) are omitted. At the cross-over point, the south-west and west-south scans coincides nicely.
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In the text

$\begin{figure} \par\mbox{\subfigure{\includegraphics[width=7cm]{9312figA9a.eps} ... ....5cm} \subfigure{\includegraphics[width=7cm]{9312figA9h.eps} }} \par\end{figure}$ Figure A.9: Dependence of the scattered wavelength-integrated intensity of the circumstellar CO vibration-rotation lines as a function of the angular distance on the sky, $\beta$ , for the different scan directions. The straight line represents a $\beta ^{a}$ power law, with the exponent a specified in each panel.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.5cm,clip]{9312fig1.eps}\end{figure}$	Figure 1: Slit positions for the Phoenix off-star observations of R Hya. All off-star slits are positioned at 1 $^{\prime \prime }$ from the star. In the figure, the slits are shifted for reasons of clarity. The number of each data set as used in the logbook (Table A.1) is indicated.
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$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{9312fig2.ps}\end{figure}$	Figure 2: The low-resolution ISO-SWS spectrum ( $R \sim 100$ ) in the 4 to 7 $\mu$ m wavelength range. The width of the box denotes the observed spectral range of the Phoenix spectrometer. The inset shows the full ISO-SWS spectrum between 2.38 and 45.2 $\mu$ m in the ( $\lambda \times F_{\lambda }$ )-space illustrating the absence of the 10 $\mu$ m silicate feature.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{9312fig5.eps}\end{figure}$	Figure 5: Off-star (full line) and on-star (dashed line) spectrum of R Hya. The three off-star CO vibration-rotation emission lines, which are marked R(1), R(2), and R(3), are partly filled in by emission from the circumstellar CO lines compared to the on-star observations. Telluric CO lines are at 2150.86, 2154.60 and 2158.30 cm^-1, telluric H₂O lines at 2152.50 and 2156.50 cm^-1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{9312fig6.eps}\end{figure}$	Figure 6: The resulting circumstellar CO vibration-rotation flux from the wind of R Hya for data set 128, being a EW-slit N1 E2.5. The intensity is integrated over the full slit area.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{9312fig7.eps}\end{figure}$	Figure 7: Set of emission spectra at the east-position from R Hya (data set 142, being a NS-slit E1 S2.5). The spectra are shifted vertically for reasons of clarity. The top spectrum is measured closest to the star, i.e., at $\beta$ = 1 $^{\prime \prime }$ . The subsequent spectra are measured at 1.1 $^{\prime \prime }$ , 1.6 $^{\prime \prime }$ and 2.4 $^{\prime \prime }$ from the star.
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$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{9312fig11.ps}\end{figure}$	Figure 11: Dependence of the mean of the scattered wavelength-integrated intensity of the circumstellar CO vibration-rotation lines on the angular distance on the sky, $\beta$ . The full black line represents a $\beta ^{-1.75}$ power law, the dashed line a $\beta ^{-3}$ power law.
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$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{9312fig13.ps}\end{figure}$	Figure 13: Upper: estimated temperature profile, middle: estimated velocity structure, and bottom: estimated mass-loss rate $\dot{M}$ (r) for R Hya as a function of radial distance to the star (black line). The shading region in the bottom panel displays the confidence intervals of the estimated mass-loss parameters. The dashed line indicates $R_{\rm {inner}}$ .
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$\begin{figure} \par\includegraphics[angle=90,width=16cm,clip]{9312fig14.ps}\par\end{figure}$	Figure 14: The CO vibra-rotational R(1), R(2), R(3) lines observed at different angular distance from the star (black) are compared with the theoretical model predictions (red) for the best-fit model with parameters as specified in Table 3. The displayed off-star data are for data set 128 (EW-slit N1 E2.5).
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$\begin{figure} \par\mbox{\subfigure[The CO~emission lines of data set~112, being... ...ludegraphics[width=7cm,height=4.6cm,angle=0]{9312figA1d.eps} }} \par\end{figure}$	Figure A.1: The CO vibration-rotation emission lines north of R Hydrae, integrated over the slit.
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$\begin{figure} \par\mbox{\subfigure[The CO~emission lines of data set~116, being... ...ludegraphics[width=7cm,height=4.6cm,angle=0]{9312figA2d.eps} }} \par\end{figure}$	Figure A.2: The CO vibration-rotation emission lines south of R Hydrae, integrated over the slit.
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$\begin{figure} \par\mbox{\subfigure[The CO~emission lines of data set~141, being... ...\includegraphics[width=7cm,height=4.6cm,angle=0]{9312figA3d.eps} }} \end{figure}$	Figure A.3: The CO vibration-rotation emission lines east of R Hydrae, integrated over the slit.
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$\begin{figure} \par\mbox{\subfigure[The CO~emission lines of data set~149, being... ...ludegraphics[width=7cm,height=4.6cm,angle=0]{9312figA4d.eps} }} \par\end{figure}$	Figure A.4: The CO vibration-rotation emission lines west of R Hydrae, integrated over the slit.
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$\begin{figure} \par\mbox{\subfigure{\includegraphics[width=8cm,clip]{9312figA5a.... ...5cm} \subfigure{\includegraphics[width=8cm,clip]{9312figA5b.eps} }} \end{figure}$	Figure A.5: Decline of the intensity of the circumstellar emission as a function of angular distance $\beta$ in the four slits positioned 1 $^{\prime \prime }$ to the south of R Hya. Left: the decline of the intensity of the four data sets 116, 117, 123, and 124. Right: mean (and standard deviation) of the intensity decline of the four south-east (SE) and south-west (SW) scans.
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$\begin{figure} \par\mbox{\subfigure{\includegraphics[width=8cm,clip]{9312figA6a.... ...5cm} \subfigure{\includegraphics[width=8cm,clip]{9312figA6b.eps} }} \end{figure}$	Figure A.6: Decline of the intensity of the circumstellar emission as a function of angular distance $\beta$ in the four slits positioned 1 $^{\prime \prime }$ to the east of R Hya. Left: the decline of the intensity of the four data sets 141, 142, 158, and 161. Right: mean (and standard deviation) of the intensity decline of the four east-north (EN) and east-south (ES) scans.
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$\begin{figure} \par\mbox{\subfigure{\includegraphics[width=8cm,clip]{9312figA7a.... ...5cm} \subfigure{\includegraphics[width=8cm,clip]{9312figA7b.eps} }} \end{figure}$	Figure A.7: Decline of the intensity of the circumstellar emission as a function of angular distance $\beta$ in the four slits positioned 1 $^{\prime \prime }$ to the west of R Hya. Left: the decline of the intensity of the four data sets 149, 150, 159, and 160. Right: mean (and standard deviation) of the intensity decline of the four west-north (WN) and west-south (WS) scans.
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$\begin{figure} \par\mbox{\subfigure{\includegraphics[width=7cm]{9312figA9a.eps} ... ....5cm} \subfigure{\includegraphics[width=7cm]{9312figA9h.eps} }} \par\end{figure}$	Figure A.9: Dependence of the scattered wavelength-integrated intensity of the circumstellar CO vibration-rotation lines as a function of the angular distance on the sky, $\beta$ , for the different scan directions. The straight line represents a $\beta ^{a}$ power law, with the exponent a specified in each panel.
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