All Figures

$\begin{figure} \par\includegraphics[width=15.3cm,clip]{2187fig01Adobe.eps} \end{figure}$ Figure 1: Diffuse and patchy emission as well as new filamentary structures are detected in the observed fields. The known supernova remnant G 116.5+1.1 is located to the lower-right, where the 1400 MHz contour marks the remnant's actual location and size. The circle seen to the upper-left part of the figure encompasses the new filamentary structures which may be part of a new candidate remnant. The filaments seen in the middle-bottom part of the figure constitute the upper portion of the well-known remnant CTB 1. The long rectangles mark the slit projections on the sky and are numbered from I through VIII. The line segments seen near over-exposed stars in this figure and the next figures are due to the blooming effect. The shadings run linearly from 0 to 32 $\times$ 10^-17 erg s^-1 cm^-2 arcsec^-2.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{2187fig02.ps} \end{figure}$ Figure 2: The field of the remnant seen through the sulfur filter. The shadings run linearly from 0 to 9 $\times$ 10^-17 erg s^-1 cm^-2 arcsec^-2, while the 60 $\mu$ m contours scale linearly from 11 to 16.4 MJy sr^-1, every 1.8 MJy sr^-1. It may be possible that cool dust is associated with the two filaments extending to the north-east around $\alpha$ $\simeq$ 00 $^{\rm h}$ 01 $^{\rm m}$ 30 $^{\rm s}$ , and $\delta$ $\simeq$ 63 $^\circ$ 26 $^\prime$ ; short segments of infrared emission also overlap optical emission around pos. IV (cf. Fig. 1). The intensity of these dust structures is typically 10 $\sigma$ above the local IR background.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2187fig03.ps} \end{figure}$ Figure 3: Long slit spectra from individual frames extracted from the listed positions in the area of G 116.5+1.1 and its surrounding area. More details can be found in Sect. 4 and Table 3.
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{2187fig04.eps} \end{figure}$ Figure 4: The HI emission in the range of LSR velocities -70 to -31 km s^-1 has been split into eight narrower velocity intervals. The radio contours at 1400 MHz scale, every 0.22 K, from 5.7 to 6.8 K brightness temperature. The data are plotted in galactic coordinates and more details are given in Sect. 5.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{2187fig05.eps} \end{figure}$ Figure 5: The left figure shows the optical emission in the south of G 116.5+1.1 along with high resolution MSX data at 8.28 $\mu$ m. The IR emission is nicely anticorrelated with the H $\alpha +[$ N II] emission. Note that the central IR emission is a factor of $\sim$ 15 stronger than the emission of the tail extending to the north-east. The right figure shows the HI emission in a wider area and in the range of LSR velocities -45 to -41 km s^-1, while the overlaid contours outline the 60 $\mu$ m IR data ( $1\hbox {$^\prime $ }\times 1\hbox {$.\mkern -4mu^\prime $ }7$ resolution; Cao et al. 1997) and is seen that the infrared emission also extends to the north-east.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2187fig03.ps} \end{figure}$	Figure 3: Long slit spectra from individual frames extracted from the listed positions in the area of G 116.5+1.1 and its surrounding area. More details can be found in Sect. 4 and Table 3.
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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{2187fig04.eps} \end{figure}$	Figure 4: The HI emission in the range of LSR velocities -70 to -31 km s^-1 has been split into eight narrower velocity intervals. The radio contours at 1400 MHz scale, every 0.22 K, from 5.7 to 6.8 K brightness temperature. The data are plotted in galactic coordinates and more details are given in Sect. 5.
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