All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.35cm,clip]{6051f1a.ps}\vspace*{5mm} \includegraphics[angle=-90,width=7.1cm,clip]{6051f1b.ps}\end{figure}$ Figure 1: Top: color diagram of stars in the field of BFS6. The curve represents the unreddened main sequence while the line is the reddening vector for a B3 star up to Av = 5 mag. Bottom: distribution of stars above the reddening vector versus the distance.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.1cm,clip]{6051f2.ps}\end{figure}$ Figure 2: New stellar distance of the complexes (filled symbols) versus old distance. The old distance is either the old stellar distance (squares) or the kinematic distance (circles). The Sun is represented by the large star symbol and the arms by the continuous lines. The curves are the fitted spiral arms from Russeil (2003).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{6051f3.ps}\end{figure}$ Figure 3: Computed rotation curve (dashed line) compared with the Brand & Blitz (1993) curve (solid line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.75cm,clip]{6051f4.ps}\end{figure}$ Figure 4: Fitted spiral structure. The symbol size is proportional to the excitation parameter (see Russeil 2003). The Sun position is given by the large star symbol. 1: Sagittarius-Carina arm, 2: Scutum-Crux arm, 1': Norma-Cygnus arm and 2': Perseus arm. The local arm feature (long dashed line), the bar (dashed-dot-dot line, from Englmaier & Gerhard 1999), the expected departure from the logarithmic spiral observed for the Sagittarius-Carina arm (short dashed line) and a feature probably linked to the 3-kpc arm (solid line) are sketched.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.2cm,clip]{6051f5.ps}\end{figure}$ Figure 5: Position of the complexes respectively to the fitted arms. Every arm is represented by three curves (central position and and width, $\pm$ 0.7 kpc, extension of the arm). Up is the cygnus arm, down is the Perseus arm. The triangle symbols are the complexes with kinematic distance only.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{6051f6.ps}\end{figure}$ Figure 6: Velocity difference versus longitude for the Perseus arm (circular symbol) and the Cygnus arm (square symbols).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{6051f7.ps}\end{figure}$ Figure 7: Circular velocity difference versus galactocentric distance (the symbols are the same as in Fig. 6). The linear regression gives a slope of 8.74 $\pm$ 1.10 and a constant term of -111.09 $\pm$ 13.34.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af1.ps}\par\includegraphics[width=8.3cm,clip]{6051af2.ps}\end{figure}$ Figure A.1: DSS images of BFS8 ( top), image size 14.7' $\times$ 12.6' and DA568 ( bottom) with radio contours, image size 26.2' $\times$ 26.1'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af3.ps}\end{figure}$ Figure A.2: DSS images of BFS6, image size 14.4' $\times$ 14.2' with radio contours.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af4.ps}\par\includegraphics[width=8.3cm,clip]{6051af5.ps}\end{figure}$ Figure A.3: DSS images of S138. Top: red image and MSX Band A contours (image size 13.3' $\times$ 13.1'). Bottom: blue image which allows us to better identify the star (image size 4.6' $\times$ 4.4').

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af6.ps}\par\includegraphics[width=8.3cm,clip]{6051af7.ps}\end{figure}$ Figure A.4: DSS images of BFS10 ( top), image size 9.8' $\times$ 8.4' and S141 ( bottom) with overlaid MSX Band A contours, image size 8.5' $\times$ 8.3'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af8.ps}\par\includegraphics[width=8.3cm,clip]{6051af9.ps}\end{figure}$ Figure A.5: Top: DSS image with radio contours of S144 ( top), image size 11' $\times$ 11'. Botton: DSS image with MSX Band A contours of S152/S153, image size 12.8' $\times$ 12.4'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af10.ps} \includegraphics[width=8.3cm,clip]{6051af11.ps}\end{figure}$ Figure A.6: Top: DSS image of S156 with MSX Band A contours (14.9' $\times$ 14.8' size). Bottom: our V-band image (6' $\times$ 6' size).

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af12.ps}\par\includegraphics[width=8.3cm,clip]{6051af13.ps}\end{figure}$ Figure A.7: DSS images of S158. Top: red image and MSX band A contours (14.7' $\times$ 12.6' size). Bottom: blue image with star identification (13.3' $\times$ 13.1' size).

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af14.ps}\par\includegraphics[width=8.3cm,clip]{6051af15.ps}\end{figure}$ Figure A.8: DSS images with MSX band A contours of s159 ( top), image size 14.7' $\times$ 12.6' and S163 stars 1 to 4 ( bottom), image size 10.3' $\times$ 9.8'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af16.ps}\par\includegraphics[width=8.3cm,clip]{6051af17.ps}\end{figure}$ Figure A.9: DSS images with MSX band A contours of S163 ( top), image size 14.3' $\times$ 14' and S170 ( bottom), image size 15.3' $\times$ 15.3'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af18.ps}\par\includegraphics[width=8.3cm,clip]{6051af19.ps}\end{figure}$ Figure A.10: DSS image with MSX band A contours of S173 ( top), image size 27.8' $\times$ 25.1'. The labels "star 1'' to "star 4'' refer to the stars observed in this paper. The labels "1'' to "4'' refer to the stars from the literature discussed in the text: 1) ALS6156, 2) ALS6151, 3) ALS6145 and 4) ALS6155. Bottom: DSS image with MSX band A contours of S175, image size 13.2' $\times$ 13.1'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af20.ps}\par\includegraphics[width=8.3cm,clip]{6051af21.ps}\end{figure}$ Figure A.11: DSS images with MSX band A contours of S182 ( top), image size 13.1' $\times$ 12.6' and S187 ( bottom), image size 19.4' $\times$ 16.9'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af22.ps}\par\includegraphics[width=8.3cm,clip]{6051af23.ps}\end{figure}$ Figure A.12: DSS image with MSX band A contours of S192 and S193 ( top), image size 12.8' $\times$ 12.1'. Bottom: DSS image of the exciting star of G137.8-1.0, image size 9.7' $\times$ 8.7'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af24.ps}\par\includegraphics[width=8.3cm,clip]{6051af25.ps}\end{figure}$ Figure A.13: Top: DSS image of S203 with radio contours (image size 1.5 $^\circ$ $\times$ 1.5 $^\circ$ ). For the two locations noted A and B we give detailed images. Bottom: smaller scale image (location A) with the identified exciting star (image size 15' $\times$ 14.7'). The cross indicates the radio source GB6 B0316+5439.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af26.ps}\end{figure}$ Figure A.14: Smaller scale image of S203 (location B) with the stars 1 and 2 (image size 12.7' $\times$ 11.8').

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af27.ps}\par\includegraphics[width=8.3cm,clip]{6051af28.ps}\end{figure}$ Figure A.15: DSS images with MSX band A contours of S196 ( top), image size 13.8' $\times$ 13.9' and BFS31 ( bottom), image size 13.4' $\times$ 13.1'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af29.ps}\par\includegraphics[width=8.3cm,clip]{6051af30.ps}\end{figure}$ Figure A.16: DSS image with MSX band A contours of for S217 ( top), image size 14.9' $\times$ 14.2'. Bottom: DSS image of S204 (image size 58' $\times$ 57.2') with radio contours overlaid. The stars discussed in the text are 1) ALS7811, 2) ALS7833, 3) ALS7829, 4) ALS7816, 5) ALS7815 and 6) BD+56$^$866.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af31.ps}\par\includegraphics[width=8.3cm,clip]{6051af32.ps}\end{figure}$ Figure A.17: DSS images with MSX band A contours of S219 ( top), image size 10.1' $\times$ 7.8' and S256 ( bottom), image size 16.5' $\times$ 13.1'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af33.ps}\par\includegraphics[width=8.3cm,clip]{6051af34.ps}\end{figure}$ Figure A.18: DSS images with MSX band A contours of S258 ( top), image size 14' $\times$ 13.8' and S283 ( bottom), image size 9.9' $\times$ 9.8'.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6051af35.ps}\par\includegraphics[width=8.3cm,clip]{6051af36.ps}\end{figure}$ Figure A.19: DSS images with MSX band A contours of BFS53 ( top), image size 12.9' $\times$ 12.8' and S294 ( bottom), image size 13.3' $\times$ 12.6'.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12.85cm,clip]{6051af37.ps}\vspace*{5mm} \includegraphics[angle=-90,width=12.8cm,clip]{6051af38.ps}\end{figure}$ Figure A.20: Top: 1) S175 star 1; 2) S170 star 1; 3) S163 star 1; 4) S159; 5) S153; 6) S152 star 4; 7) S141; 8) G137.8-1.0; 9) BFS10. Bottom: 1) S173 star 1; 2) S173 star 2; 3) S173 star 3; 4) S187 star 1; 5) S192 star 1; 6) S193 star 3; 7) S193 star 1; 8) S204.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12.5cm,clip]{6051af39.ps}\vspace*{5mm} \includegraphics[angle=-90,width=13cm,clip]{6051af40.ps}\end{figure}$ Figure A.21: Top: 1) S182 star 1; 2) S187 star 3; 3) S219 star 4; 4) S219 star 1; 5) S158 star 2; 6) S158 star 1. Bottom: 1) S156; 2) S138 star 1.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12.4cm,clip]{6051af41.ps}\vspace*{5mm} \includegraphics[angle=-90,width=12.7cm,clip]{6051af42.ps}\end{figure}$ Figure A.22: Top: 1) S258 star 2; 2) S217 star 2; 3) S203 star 3; 4) S219 star 7; 5) S256 star 2; 6) S294 star 1; 7) BFS31; 8) BFS53; 9) S196 star 4. Bottom: 1) S283 star 1; 2) BFS8 star 2; 3) S170 star 5; 4) S170 star 4; 5) S170 star 3; 6) S170 star 2; 7) S163 star 6; 8) S163 star 5; 9) S163 star 7.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12.7cm,clip]{6051af43.ps}\end{figure}$ Figure A.23: 1) DA568 star 2; 2) DA568 star 1; 3) S283 star 5; 4) S283 star 2; 5) S283 star 4.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.35cm,clip]{6051f1a.ps}\vspace*{5mm} \includegraphics[angle=-90,width=7.1cm,clip]{6051f1b.ps}\end{figure}$	Figure 1: Top: color diagram of stars in the field of BFS6. The curve represents the unreddened main sequence while the line is the reddening vector for a B3 star up to Av = 5 mag. Bottom: distribution of stars above the reddening vector versus the distance.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.1cm,clip]{6051f2.ps}\end{figure}$	Figure 2: New stellar distance of the complexes (filled symbols) versus old distance. The old distance is either the old stellar distance (squares) or the kinematic distance (circles). The Sun is represented by the large star symbol and the arms by the continuous lines. The curves are the fitted spiral arms from Russeil (2003).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{6051f3.ps}\end{figure}$	Figure 3: Computed rotation curve (dashed line) compared with the Brand & Blitz (1993) curve (solid line).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.2cm,clip]{6051f5.ps}\end{figure}$	Figure 5: Position of the complexes respectively to the fitted arms. Every arm is represented by three curves (central position and and width, $\pm$ 0.7 kpc, extension of the arm). Up is the cygnus arm, down is the Perseus arm. The triangle symbols are the complexes with kinematic distance only.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.3cm,clip]{6051f6.ps}\end{figure}$	Figure 6: Velocity difference versus longitude for the Perseus arm (circular symbol) and the Cygnus arm (square symbols).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{6051f7.ps}\end{figure}$	Figure 7: Circular velocity difference versus galactocentric distance (the symbols are the same as in Fig. 6). The linear regression gives a slope of 8.74 $\pm$ 1.10 and a constant term of -111.09 $\pm$ 13.34.
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