Astronomy & Astrophysics

All Figures

$\begin{figure} \par\psfig{figure=ms3723f1.ps,width=8.5cm,clip}\end{figure}$ Figure 1: Thermal equilibrium curve for the standard AGN spectrum in Cloudy (see Woods et al.1996).
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In the text

$\begin{figure} \par\psfig{figure=ms3723f2.ps,width=16.5cm,clip} \end{figure}$ Figure 2: The evolution of a SNR expanding into a stationary environment of density $n = 10^{6}~{\rm cm}^{-3}$ . Shown are logarithmic plots of the density with a scale from $2.4 \times 10^{4}~{\rm cm}^{-3}$ (white) to $3.1 \times 10^{8} ~{\rm cm}^{-3}$ (black). The age of the remnant is shown in the upper left corner of each plot. Note the change in the axis scaling between the plots. The unit of length in these and subsequent plots is $1.1 \times 10^{16}~{\rm cm}$ (0.0036 pc), and the ionization parameter of the surrounding medium, $\Xi \approx 150$ , unless explicitly stated otherwise.
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In the text

$\begin{figure} \par\psfig{figure=ms3723f3.ps,width=16.2cm,clip} \end{figure}$ Figure 3: As Fig. 2 but showing logarithmic plots of the temperature with a scale from $10^{6}~{\rm K}$ (white) to $1.58 \times 10^{8}~{\rm K}$ (black). Note the creation, evolution, and destruction of cool gas ( $T < 10^{6}~{\rm K}$ ) within the remnant.
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In the text

$\begin{figure} \par\psfig{figure=ms3723f4.ps,width=16.5cm,clip} \end{figure}$ Figure 4: The morphology of a SNR expanding into stationary surroundings with $n = 10^{5} ~{\rm cm}^{-3}$ at $t = 30~{\rm yr}$ . Left: logarithmic density (grayscale from $4.7 \times 10^{4} ~{\rm cm}^{-3}$ (white) to $1.8 \times 10^{7} ~{\rm cm}^{-3}$ (black)). Right: logarithmic temperature (grayscale from $10^{6}~{\rm K}$ (white) to $1.58 \times 10^{8}~{\rm K}$ (black)). The unit of length is $2.24 \times 10^{16}~{\rm cm}$ (0.0073 pc).
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In the text

$\begin{figure} \par\psfig{figure=ms3723f5.ps,width=16.3cm,clip} \end{figure}$ Figure 5: The evolution of a SNR expanding into an AGN wind with $n = 10^{6}~{\rm cm}^{-3}$ and $v = 3000~{\rm km}~{\rm s}^{-1}$ . In this figure the AGN wind propagates down the page and the explosion site is at position (0, 0). The top row shows logarithmic plots of the density with a scale from $2.4 \times 10^{4}~{\rm cm}^{-3}$ (white) to $3.1~ \times~ 10^{8} ~{\rm cm}^{-3}$ (black), while the bottom row shows logarithmic plots of the temperature with a scale from $10^{6}~{\rm K}$ (white) to $1.58~ \times~ 10^{8}~{\rm K}$ (black). The age of the remnant is shown in the upper left corner of each plot. Note the change in the axis scaling between the plots.
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In the text

$\begin{figure} \par\psfig{figure=ms3723f6.ps,width=16.5cm,clip} \end{figure}$ Figure 6: The density and temperature structure of individual bowshocks and cool clumps. The top panels show the structure existing at $t = 10~{\rm yr}$ when a remnant expands into an ambient density $n = 10^{6}~{\rm cm}^{-3}$ . The bottom panels show the structure existing at $t = 30~{\rm yr}$ when a remnant expands into an ambient density $n = 10^{5} ~{\rm cm}^{-3}$ . The left panels display density gray-scales, contours, and flow vectors, while the right panels display temperature gray-scales and contours.
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In the text

$\begin{figure} \par\psfig{figure=ms3723f7.ps,width=13.5cm,clip} \end{figure}$ Figure 7: The evolution of cool gas in remnants expanding into a surrounding medium with $n = 10^{6}~{\rm cm}^{-3}$ . The mass of cool gas with an ionization parameter below $\Xi$ is shown as a function of t for flow speeds of $v = 0,\;3000,\;5000,\;7000~{\rm km}~{\rm s}^{-1}$ .
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In the text

$\begin{figure} \par\psfig{figure=ms3723f8a.ps,width=8.2cm,clip}\vspace*{6mm} \par\psfig{figure=ms3723f8b.ps,width=8.2cm,clip} \end{figure}$ Figure 8: The evolution of the mass of cool clouds in remnants expanding into a surrounding medium with $n = 10^{5} ~{\rm cm}^{-3}$ ( top) and $n = 10^{6}~{\rm cm}^{-3}$ ( bottom). In each panel the mass of cool gas is shown as a function of t for flow speeds of $v = 0,\;3000,\;5000,\;7000~{\rm km}~{\rm s}^{-1}$ .
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In the text

$\begin{figure} \par\psfig{figure=ms3723f9.ps,width=16.8cm,clip} \end{figure}$ Figure 9: The evolution of a SNR expanding into a stationary environment with $n = 10^{6}~{\rm cm}^{-3}$ and $\Xi \approx 1500$ . The top panels show logarithmic plots of the density, while the bottom panels show logarithmic plots of the temperature (same scaling as in Figs. 2 and 3). Note that cool clouds do not form in this case.
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In the text

$\begin{figure} \par\psfig{figure=ms3723f10.ps,width=14.3cm,clip} \end{figure}$ Figure 10: Line profiles from cool gas formed in a SNR expanding into an AGN environment with $\Xi \approx 150$ and integrated over many lines of sight ( i.e. it is assumed that there is a spherical distribution of remnants in an isotropic medium and radiation field). The left and middle columns are for stationary environments with $n = 10^{5} ~{\rm cm}^{-3}$ and $n = 10^{6}~{\rm cm}^{-3}$ , respectively. The right column is for an environment with $n = 10^{6}~{\rm cm}^{-3}$ and $v = 3000~{\rm km}~{\rm s}^{-1}$ . In the top two rows the line profile at specific remnant ages is displayed, with the age of the remnant (in years) marked next to each profile. The solid line in the top row corresponds to $t = 20~{\rm yr}$ for $n = 10^{5} ~{\rm cm}^{-3}$ , and $t = 5~{\rm yr}$ for $n = 10^{6}~{\rm cm}^{-3}$ . The remaining profiles in the top and middle rows correspond to the subsequent entries in Table 2, with the line width decreasing with remnant age. In the bottom row the average line profile integrated over the age of the remnant is displayed. Note the difference in the scaling of the intensity axis.
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In the text

$\begin{figure} \par\psfig{figure=ms3723f11.ps,width=16cm,clip} \end{figure}$ Figure 11: Line profiles from cool gas formed in a SNR expanding into an AGN wind with $n = 10^{6}~{\rm cm}^{-3}$ , $\Xi \approx 150$ , and v = 3000, 5000, or $7000~{\rm km}~{\rm s}^{-1}$ . The line-of-sight is specified by $\theta = 135^{\circ }$ ( i.e. there is a component of the AGN wind moving towards the observer) and the profiles are from remnants of age $t = 5~{\rm yr}$ (top row), $t = 10~{\rm yr}$ , $t=15~{\rm yr}$ , and $t = 20~{\rm yr}$ . In the bottom row the age integrated profiles are shown.
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In the text

$\begin{figure} \par\psfig{figure=ms3723f1.ps,width=8.5cm,clip}\end{figure}$	Figure 1: Thermal equilibrium curve for the standard AGN spectrum in Cloudy (see Woods et al.1996).
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$\begin{figure} \par\psfig{figure=ms3723f3.ps,width=16.2cm,clip} \end{figure}$	Figure 3: As Fig. 2 but showing logarithmic plots of the temperature with a scale from $10^{6}~{\rm K}$ (white) to $1.58 \times 10^{8}~{\rm K}$ (black). Note the creation, evolution, and destruction of cool gas ( $T < 10^{6}~{\rm K}$ ) within the remnant.
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$\begin{figure} \par\psfig{figure=ms3723f7.ps,width=13.5cm,clip} \end{figure}$	Figure 7: The evolution of cool gas in remnants expanding into a surrounding medium with $n = 10^{6}~{\rm cm}^{-3}$ . The mass of cool gas with an ionization parameter below $\Xi$ is shown as a function of t for flow speeds of $v = 0,\;3000,\;5000,\;7000~{\rm km}~{\rm s}^{-1}$ .
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$\begin{figure} \par\psfig{figure=ms3723f8a.ps,width=8.2cm,clip}\vspace*{6mm} \par\psfig{figure=ms3723f8b.ps,width=8.2cm,clip} \end{figure}$	Figure 8: The evolution of the mass of cool clouds in remnants expanding into a surrounding medium with $n = 10^{5} ~{\rm cm}^{-3}$ ( top) and $n = 10^{6}~{\rm cm}^{-3}$ ( bottom). In each panel the mass of cool gas is shown as a function of t for flow speeds of $v = 0,\;3000,\;5000,\;7000~{\rm km}~{\rm s}^{-1}$ .
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$\begin{figure} \par\psfig{figure=ms3723f9.ps,width=16.8cm,clip} \end{figure}$	Figure 9: The evolution of a SNR expanding into a stationary environment with $n = 10^{6}~{\rm cm}^{-3}$ and $\Xi \approx 1500$ . The top panels show logarithmic plots of the density, while the bottom panels show logarithmic plots of the temperature (same scaling as in Figs. 2 and 3). Note that cool clouds do not form in this case.
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