All Figures

$\begin{figure} \mbox{ \includegraphics[bb = 40 150 560 600,width=5.5cm,clip]{g6... ...ludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g69.7.c74.ps} } \end{figure}$ Figure 1: Total power images at 1420 MHz ( first and third row) and 408 MHz ( second and fourth row) of the supernova remnants G65.1+0.6, G65.7+1.2 (DA 495), G67.7+1.8, G68.6-1.2, G69.0+2.7 (CTB 80), and G69.7+1.0.
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In the text

$\begin{figure} {\includegraphics[bb = 10 10 1635 1285,height=13cm,clip]{spec1.ps} } \end{figure}$ Figure 7: The radio continuum spectra of the SNRs G65.1+0.6, G65.7+1.2 (DA 495), G67.7+1.8, G69.0+2.7 (CTB 80), G69.7+1.0, G73.9+0.9, G74.9+1.2 (CTB 87), G76.9+1.0, and G78.2+2.1 (DR 4, $\gamma$ Cygni). The CGPS flux densities are represented by triangles.
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In the text

$\begin{figure} \includegraphics[bb = 55 45 540 510,width=8.5cm,clip]{histo.ps} \end{figure}$ Figure 11: Distribution of the spectral index $\alpha _{\rm all}$ (see Table 3) of all supernova remnants listed in this publication.
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In the text

$\begin{figure} \mbox{\includegraphics[bb = 42 55 575 510,width=5.5cm,clip]{pi65... ...\includegraphics[bb = 42 55 575 510,width=5.5cm,clip]{pi106.3.ps} } \end{figure}$ Figure 12: Images of polarized intensity at 1420 MHz of the supernova remnants 65.7+1.2 (DA 495), G67.7+1.8, G69.0+2.7 (CTB 80), G73.9+0.9, G74.9+1.2 (CTB 87), G76.9+1.0, G89.0+4.7 (HB 21), G93.7-0.2 (CTB 104A, DA 551), and G106.3+2.7. The contours indicate the total power emission.
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In the text

$\begin{figure} \mbox{\includegraphics[bb = 42 55 575 510,width=5.5cm,clip]{pi10... ...\includegraphics[bb = 42 55 575 510,width=5.5cm,clip]{pi166.0.ps} } \end{figure}$ Figure 13: Images of polarized intensity at 1420 MHz of the supernova remnants G107.5-1.5, G109.1-1.0 (CTB 109), G113.0+2.0, G116.5+1.1, G120.1+1.4 (Tycho, 3C 10, SN 1572), G127.1+0.5, G130.7+3.1 (3C 58, SN 1181), G160.9+2.6 (HB 9), and G166.0+4.3 (VRO 42.05.01). The contours indicate the total power emission.
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In the text

$\begin{figure} \mbox{\includegraphics[bb = 40 150 560 600,width=5.5cm,clip]{g73... ...cludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g83.0.c74.ps} } \end{figure}$ Figure 2: Total power images at 1420 MHz ( first and third row) and at 408 MHz ( second and fourth row) of the supernova remnants G73.9+0.9, G74.9+1.2 (CTB 87), G76.9.3+1.0, G78.2+2.1 (DR 4, $\gamma$ -Cygni), G82.2+5.3 (W 63), and G83.0-0.3.
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In the text

$\begin{figure} \mbox{\includegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g84.... ...cludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g93.3.c74.ps} } \end{figure}$ Figure 3: Total power images at 1420 MHz ( first and third row) and 408 MHz ( second and fourth row) of the supernova remnants G84.2-0.8, G84.9+0.5, G85.4+0.7, G85.9-0.6, G89.0+4.7 (HB 21), and G93.3+6.9 (DA 530).
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In the text

$\begin{figure} \mbox{\includegraphics[bb = 40 150 560 600,width=5.5cm,clip]{g93... ...ludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g109.1.c74.ps} } \end{figure}$ Figure 4: Total power images at 1420 MHz ( first and third row) and 408 MHz ( second and fourth row) of the supernova remnants G93.7-0.2 (CTB 104A), G94.0+1.0 (3C 434.1), G96.0+2.0, G106.3+2.7, G107.5-1.5, and G109.1-1.0 (CTB 109).
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In the text

$\begin{figure} \mbox{\includegraphics[bb = 40 150 560 600,width=5.5cm,clip]{g11... ...ludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g126.2.c74.ps} } \end{figure}$ Figure 5: Total power images at 1420 MHz ( first and third row) and 408 MHz ( second and fourth row) of the supernova remnants G113.0+0.1, G114.3+0.3, G116.5+1.1, G116.9+0.2 (CTB 1), G120.1+1.4 (Tycho's SNR), and G126.2+1.6.
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In the text

$\begin{figure} \mbox{\includegraphics[bb = 40 150 560 600,width=5.5cm,clip]{g12... ...ludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g166.0.c74.ps} } \end{figure}$ Figure 6: Total power images at 1420 MHz ( first and third row) and 408 MHz ( second and fourth row) of the supernova remnants G127.1+0.5, G130.7+3.1 (3C 58), G132.7+1.3 (HB 3), G156.2+5.7, G160.9+2.6 (HB 9), and G166.0+4.3 (VRO 42.05.01).
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In the text

$\begin{figure} {\includegraphics[bb = 10 10 1658 1285,height=13cm,clip]{spec2.ps} } \end{figure}$ Figure 8: The radio continuum spectra of the SNRs G82.2+5.3 (W 63), G83.0-0.3, G84.2-0.8, G84.9+0.5, G85.4+0.7, G85.9-0.6, G89.0+4.7 (HB 21), G93.3+6.9 (DA 530), and G93.7-0.2 (CTB 104A, DA 551). The CGPS flux densities are represented by triangles.
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In the text

$\begin{figure} {\includegraphics[bb = 10 10 1635 1285,height=13cm,clip]{spec3.ps} } \end{figure}$ Figure 9: The radio continuum spectra of the SNRs G94.0+1.0, G96.0+2.0, G106.3+2.7, G107.5-1.5, G109.1-1.0 (CTB 109), G114.3+0.3, G116.5+1.1, G116.9+0.2 (CTB 1), and G120.1+1.4 (Tycho, 3C 10, SN 1572). The CGPS flux densities are represented by triangles.
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In the text

$\begin{figure} {\includegraphics[bb = 10 10 1635 1285,height=13cm,clip]{spec4.ps} } \end{figure}$ Figure 10: The radio continuum spectra of the SNRs G126.2+1.6, G127.1+0.5 (R 5), G130.7+3.1 (3C 58, SN 1181) G132.7+1.3 (HB 3), G156.2+5.7, G160.9+2.6 (HB 9), and G166.0+4.3 (VRO 42.05.01). The CGPS flux densities are represented by triangles.
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In the text

$\begin{figure} \mbox{ \includegraphics[bb = 40 150 560 600,width=5.5cm,clip]{g6... ...ludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g69.7.c74.ps} } \end{figure}$	Figure 1: Total power images at 1420 MHz ( first and third row) and 408 MHz ( second and fourth row) of the supernova remnants G65.1+0.6, G65.7+1.2 (DA 495), G67.7+1.8, G68.6-1.2, G69.0+2.7 (CTB 80), and G69.7+1.0.
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$\begin{figure} {\includegraphics[bb = 10 10 1635 1285,height=13cm,clip]{spec1.ps} } \end{figure}$	Figure 7: The radio continuum spectra of the SNRs G65.1+0.6, G65.7+1.2 (DA 495), G67.7+1.8, G69.0+2.7 (CTB 80), G69.7+1.0, G73.9+0.9, G74.9+1.2 (CTB 87), G76.9+1.0, and G78.2+2.1 (DR 4, $\gamma$ Cygni). The CGPS flux densities are represented by triangles.
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$\begin{figure} \includegraphics[bb = 55 45 540 510,width=8.5cm,clip]{histo.ps} \end{figure}$	Figure 11: Distribution of the spectral index $\alpha _{\rm all}$ (see Table 3) of all supernova remnants listed in this publication.
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$\begin{figure} \mbox{\includegraphics[bb = 42 55 575 510,width=5.5cm,clip]{pi65... ...\includegraphics[bb = 42 55 575 510,width=5.5cm,clip]{pi106.3.ps} } \end{figure}$	Figure 12: Images of polarized intensity at 1420 MHz of the supernova remnants 65.7+1.2 (DA 495), G67.7+1.8, G69.0+2.7 (CTB 80), G73.9+0.9, G74.9+1.2 (CTB 87), G76.9+1.0, G89.0+4.7 (HB 21), G93.7-0.2 (CTB 104A, DA 551), and G106.3+2.7. The contours indicate the total power emission.
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$\begin{figure} \mbox{\includegraphics[bb = 42 55 575 510,width=5.5cm,clip]{pi10... ...\includegraphics[bb = 42 55 575 510,width=5.5cm,clip]{pi166.0.ps} } \end{figure}$	Figure 13: Images of polarized intensity at 1420 MHz of the supernova remnants G107.5-1.5, G109.1-1.0 (CTB 109), G113.0+2.0, G116.5+1.1, G120.1+1.4 (Tycho, 3C 10, SN 1572), G127.1+0.5, G130.7+3.1 (3C 58, SN 1181), G160.9+2.6 (HB 9), and G166.0+4.3 (VRO 42.05.01). The contours indicate the total power emission.
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$\begin{figure} \mbox{\includegraphics[bb = 40 150 560 600,width=5.5cm,clip]{g73... ...cludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g83.0.c74.ps} } \end{figure}$	Figure 2: Total power images at 1420 MHz ( first and third row) and at 408 MHz ( second and fourth row) of the supernova remnants G73.9+0.9, G74.9+1.2 (CTB 87), G76.9.3+1.0, G78.2+2.1 (DR 4, $\gamma$ -Cygni), G82.2+5.3 (W 63), and G83.0-0.3.
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$\begin{figure} \mbox{\includegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g84.... ...cludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g93.3.c74.ps} } \end{figure}$	Figure 3: Total power images at 1420 MHz ( first and third row) and 408 MHz ( second and fourth row) of the supernova remnants G84.2-0.8, G84.9+0.5, G85.4+0.7, G85.9-0.6, G89.0+4.7 (HB 21), and G93.3+6.9 (DA 530).
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$\begin{figure} \mbox{\includegraphics[bb = 40 150 560 600,width=5.5cm,clip]{g93... ...ludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g109.1.c74.ps} } \end{figure}$	Figure 4: Total power images at 1420 MHz ( first and third row) and 408 MHz ( second and fourth row) of the supernova remnants G93.7-0.2 (CTB 104A), G94.0+1.0 (3C 434.1), G96.0+2.0, G106.3+2.7, G107.5-1.5, and G109.1-1.0 (CTB 109).
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$\begin{figure} \mbox{\includegraphics[bb = 40 150 560 600,width=5.5cm,clip]{g11... ...ludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g126.2.c74.ps} } \end{figure}$	Figure 5: Total power images at 1420 MHz ( first and third row) and 408 MHz ( second and fourth row) of the supernova remnants G113.0+0.1, G114.3+0.3, G116.5+1.1, G116.9+0.2 (CTB 1), G120.1+1.4 (Tycho's SNR), and G126.2+1.6.
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$\begin{figure} \mbox{\includegraphics[bb = 40 150 560 600,width=5.5cm,clip]{g12... ...ludegraphics[bb = 42 52 565 507,width=5.5cm,clip]{g166.0.c74.ps} } \end{figure}$	Figure 6: Total power images at 1420 MHz ( first and third row) and 408 MHz ( second and fourth row) of the supernova remnants G127.1+0.5, G130.7+3.1 (3C 58), G132.7+1.3 (HB 3), G156.2+5.7, G160.9+2.6 (HB 9), and G166.0+4.3 (VRO 42.05.01).
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$\begin{figure} {\includegraphics[bb = 10 10 1658 1285,height=13cm,clip]{spec2.ps} } \end{figure}$	Figure 8: The radio continuum spectra of the SNRs G82.2+5.3 (W 63), G83.0-0.3, G84.2-0.8, G84.9+0.5, G85.4+0.7, G85.9-0.6, G89.0+4.7 (HB 21), G93.3+6.9 (DA 530), and G93.7-0.2 (CTB 104A, DA 551). The CGPS flux densities are represented by triangles.
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$\begin{figure} {\includegraphics[bb = 10 10 1635 1285,height=13cm,clip]{spec3.ps} } \end{figure}$	Figure 9: The radio continuum spectra of the SNRs G94.0+1.0, G96.0+2.0, G106.3+2.7, G107.5-1.5, G109.1-1.0 (CTB 109), G114.3+0.3, G116.5+1.1, G116.9+0.2 (CTB 1), and G120.1+1.4 (Tycho, 3C 10, SN 1572). The CGPS flux densities are represented by triangles.
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$\begin{figure} {\includegraphics[bb = 10 10 1635 1285,height=13cm,clip]{spec4.ps} } \end{figure}$	Figure 10: The radio continuum spectra of the SNRs G126.2+1.6, G127.1+0.5 (R 5), G130.7+3.1 (3C 58, SN 1181) G132.7+1.3 (HB 3), G156.2+5.7, G160.9+2.6 (HB 9), and G166.0+4.3 (VRO 42.05.01). The CGPS flux densities are represented by triangles.
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