All Figures

$\begin{figure} \par {\includegraphics[width=12cm,clip]{ms3949.f01} } \end{figure}$ Figure 1: Diffuse and patchy emission dominates the field of G 78.2+2.1. The shadings run linearly from 0 to $280 \times 10^{-17}$ erg s^-1 cm^-2 arcsec^-2, while the 1400 MHz contours scale also linearly from 5 to 90 K brightness temperature in steps of 9.3 K (Taylor et al. 2003). The long rectangles in the east and north-west mark the slit projections on the sky. The line segments seen near over-exposed stars in this figure and the next figures are due to the blooming effect. North is up, East is to the left and the coordinates given in this figure and the next figures refer to epoch J2000.
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In the text

$\begin{figure} \par {\includegraphics[width=12cm,clip]{ms3949.f02} } \end{figure}$ Figure 2: The same field as in Fig. 1 but now seen through the sulfur filter. The shadings run linearly from 0 to $25 \times 10^{-17}$ erg s^-1 cm^-2 arcsec^-2, while the infrared emission at 8.28 $\mu$ m is shown in contours scaling from $8\times 10^{-7}$ to $8\times 10^{-6}$ W m^-2 sr^-1. Evidence for shock-heated gas are not present in areas of strong IR emission.
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In the text

$\begin{figure} \par {\includegraphics[width=12cm,clip]{ms3949.f03} } \end{figure}$ Figure 3: The emission in the medium ionization line of [O III] 5007 Å is shown in this figure. The dashed lines mark the detected small scale structures in the east and north-west. The shadings run linearly from 0 to $20 \times 10^{-17}$ erg s^-1 cm^-2 arcsec^-2.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{ms3949.f04} } \end{figure}$ Figure 4: The total molecular CO emission in the field of G 78.2+2.1 with contours of the radio emission at 1400 MHz. Weak CO emission is mainly seen in the north-east, the west and towards the central areas of G 78.2+2.1. The strongest molecular emission seems to be projected to the south-east of $\gamma$ Cygni. The CO data were interpolated to produce a smoother image.
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In the text

$\begin{figure} \par {\includegraphics[width=12cm,clip]{ms3949.f02} } \end{figure}$	Figure 2: The same field as in Fig. 1 but now seen through the sulfur filter. The shadings run linearly from 0 to $25 \times 10^{-17}$ erg s^-1 cm^-2 arcsec^-2, while the infrared emission at 8.28 $\mu$ m is shown in contours scaling from $8\times 10^{-7}$ to $8\times 10^{-6}$ W m^-2 sr^-1. Evidence for shock-heated gas are not present in areas of strong IR emission.
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$\begin{figure} \par {\includegraphics[width=12cm,clip]{ms3949.f03} } \end{figure}$	Figure 3: The emission in the medium ionization line of [O III] 5007 Å is shown in this figure. The dashed lines mark the detected small scale structures in the east and north-west. The shadings run linearly from 0 to $20 \times 10^{-17}$ erg s^-1 cm^-2 arcsec^-2.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{ms3949.f04} } \end{figure}$	Figure 4: The total molecular CO emission in the field of G 78.2+2.1 with contours of the radio emission at 1400 MHz. Weak CO emission is mainly seen in the north-east, the west and towards the central areas of G 78.2+2.1. The strongest molecular emission seems to be projected to the south-east of $\gamma$ Cygni. The CO data were interpolated to produce a smoother image.
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