All Figures

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=8.8cm,clip]{9642fig1a.... ....ps} \includegraphics[angle=-90,width=8.8cm,clip=]{9642fig1d.ps} } \end{figure}$ Figure 1: EPIC spectra of supernova remnants in the SMC. From top left to bottom right: a) SNR B0039-7353 = HFPK 530, b) SNR B0050-72.8, c) SNR B0058-71.8 and d) the candidate SNR HFPK 334. The best fits using a single-temperature NEI model are plotted as histograms (black: PN, red: MOS1, green: MOS2).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9642fig2a.eps}\h... ...*{2mm} \includegraphics[angle=-90,width=8.4cm,clip]{9642fig2b.eps} \end{figure}$ Figure 2: A composite optical image (RGB = H $_{\alpha }$ , [S II] and [O III], respectively, all continuum-subtracted) of SMC SNR DEM S5 overlaid with (A) XMM-Newton broad-band contours and (B) ATCA 6-cm contours. The X-ray contours are 15, 20, 25, 30, 35, 40, and 50 $~\times~10^{-6}$ ct s^-1 pix^-1, and the radio-continuum contours are 2, 3, 5, 7, 10, 15, 20 and 25 mJy/beam. Note that the [O III] emission is brightest at the outside of the shell, closest to the expanding SNR shock, with H $_{\alpha }$ , [S II] lagging behind where the post-shock gas has cooled somewhat. The prominent bluish object at the upper right (north-west - centred at RA(J2000 $)=\rm00^h40^m02.6^s$ and Dec(J2000)=-73 $^\circ$ 33 $^\prime$ 53 $^{\prime \prime }$ ), with faint [O III] inside and H $_{\alpha }$ around much of the ill-defined periphery, is a photo-ionised region. Another, much fainter region of [O III] emission is just south-east of DEM S5 (RA(J2000 $)=\rm00^h41^m32.7^s$ and Dec(J2000)=-73 $^\circ$ 38 $^\prime$ 22 $^{\prime \prime }$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9642fig3a.eps}\h... ...*{2mm} \includegraphics[angle=-90,width=8.4cm,clip]{9642fig3b.eps} \end{figure}$ Figure 3: A composite optical image (RGB - H $_{\alpha }$ , [S II] and [O III]) of SMC SNR B0050-72.8 overlaid with (A) XMM-Newton broad-band contours and (B) ATCA 6-cm contour map. X-ray contours are 15, 20, 25, 30, 35, and 40 $~\times~10^{-6}$ ct s^-1 pix^-1. Radio-continuum contours are from 1 to 5 mJy/beam in steps of 0.25 mJy/beam. The red circle indicates the position and extent of the remnant. The bright object in the lower left corner is the compact H II region DEM S69.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9642fig4a.eps} \... ...4b.eps} \includegraphics[angle=-90,width=8.4cm,clip]{9642fig4c.eps} \end{figure}$ Figure 4: A composite optical image (RGB - H $_{\alpha }$ , [S II] and [O III]) of SMC SNR B0058-71.8 overlaid with (A) XMM-Newton broad-band contours, showing the entire DEM S108 shell. An inset showing just the remnant overlaid with (B) XMM-Newton broad-band contours and (C) ATCA 6-cm contours. X-ray contours are 30, 35, 40, 45, 50, 70, and 150 $~\times~10^{-6}$ ct s^-1 pix^-1. Radio-continuum contours are 0.5, 1, 1.5, 2, 2.5, 3, 3.5, 4, and 5 mJy/beam. The bright object in the lower left corner is the compact H II region DEM S109.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{9642fig5a.eps}\p... ...egraphics[angle=-90,width=6.5cm,clip]{9642fig5b.eps}\hspace*{9mm}} \end{figure}$ Figure 5: (A) A composite XMM-Newton image (RGB - soft (0.2-1.0 keV), medium (1.0-2.0 keV) and hard (2.0-4.5 keV)) of the SMC SNR HFPK 334 overlaid with ATCA 6-cm contour map. (B) ATCA 3-cm image overlaid with ATCA 6-cm contour map. The black circle represents the 3-cm beam size of $12 \times 11\hbox {$^{\prime \prime }$ }$ . The radio-continuum contours at 6-cm are from 0.27 to 3.0 mJy/beam in 0.13 mJy/beam steps.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{9642fig6.eps} \end{figure}$ Figure 6: A diameter distribution of the SMC SNRs and SNR candidates. We assume a distance to the SMC of 60 kpc.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=8.8cm,clip]{9642fig1a.... ....ps} \includegraphics[angle=-90,width=8.8cm,clip=]{9642fig1d.ps} } \end{figure}$	Figure 1: EPIC spectra of supernova remnants in the SMC. From top left to bottom right: a) SNR B0039-7353 = HFPK 530, b) SNR B0050-72.8, c) SNR B0058-71.8 and d) the candidate SNR HFPK 334. The best fits using a single-temperature NEI model are plotted as histograms (black: PN, red: MOS1, green: MOS2).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{9642fig6.eps} \end{figure}$	Figure 6: A diameter distribution of the SMC SNRs and SNR candidates. We assume a distance to the SMC of 60 kpc.
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