Astronomy & Astrophysics

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$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...}}% \put(371,225){\makebox(0,0)[r]{ 0}}% \end{picture}% \endgroup\end{figure}$ Figure 1: Luminosity function in the V band in the solar neighbourhood. Crosses with Poisson errors: Jahreiss determination from the revised Catalogue of Nearby Stars; Lines: model LF assuming an IMF slope of $\alpha =1.7$ (solid line) and 1.6 (dashed line) at m<1 $M_{\odot }$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip=,angle=-90]{3188f2.eps} \end{figure}$ Figure 2: Circular velocity of the self-consistent model. Crosses are observational constraints from Caldwell & Ostriker (1981). Contributions from main Galactic components are also given.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip=,angle=0]{3188f3.eps}\end{figure}$ Figure 3: Star counts in K along a DENIS strip in counts per 0.8 $^\circ$ bin in declination (this strip crosses the plane at $l=266.1^\circ$ ). Data are in solid lines, models in dashed lines. Top panel: flat disc. Middle panel: warped disc. Bottom panel: warped and flaring disc.
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In the text

$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...ut(320,240){\makebox(0,0)[r]{ 0.1}}% \end{picture}% \endgroup\par\end{figure}$ Figure 4: Star count predictions in the V band at the Galactic pole. Solid line: total with a spheroid IMF slope of $\alpha =0.5$ , long dashed: disc, short dashed: thick disc, dotted: spheroid, dotted dashed: total with a spheroid IMF slope of $\alpha =2$ . Various observed counts are indicated as crosses (error bars are the Poisson noise) from Simbad data base, Gilmore et al. (1985), Bok & Basinski (1964), Chiu (1980), Yoshii et al. (1987) and Crézé et al., in preparation.
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In the text

$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...40){\makebox(0,0)[r]{ 0.01}}% \end{picture}% \endgroup \small\par\end{figure}$ Figure 5: Star count predictions (stars per magnitude and per square degree) in the V band at $l=0^\circ$ , for latitudes 10 $^\circ$ to 90 $^\circ$ from top to bottom (20 $^\circ$ , 45 $^\circ$ and 90 $^\circ$ with solid lines, 10 $^\circ$ , 30 $^\circ$ , 60 $^\circ$ with dashed lines). Data are from Ojha et al. (1994a) and Yoshii & Rodgers (1989).
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In the text

$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...t(360,240){\makebox(0,0)[r]{ 0.01}}% \end{picture}% \endgroup\par\end{figure}$ Figure 6: Star count predictions (stars per magnitude and per square degree) in the V band at $l=90^\circ$ or 270 $^\circ$ , for latitudes 10 $^\circ$ to 90 $^\circ$ from top to bottom (0 $^\circ$ , 20 $^\circ$ , 45 $^\circ$ and 90 $^\circ$ with solid lines, 10 $^\circ$ , 30 $^\circ$ , 60 $^\circ$ with dashed lines). For each latitude the bifurcation is due to the warp, the highest part being for l=90, b>0 or l=270, b<0. Data are from Ojha et al. (1996), the DMS survey Hall et al. (1996) and in the Chandra Deep Field South from Groenewegen et al. (2002) (longitudes and latitudes of the data are in parentheses).
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In the text

$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...t(360,240){\makebox(0,0)[r]{ 0.01}}% \end{picture}% \endgroup\par\end{figure}$ Figure 7: Same as figure 5 but for l=180. Data are from Ojha et al. (1994b), Borra & Lepage (1986) and Chiu (1980) in indicated directions.
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In the text

$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...ut(360,240){\makebox(0,0)[r]{ 0.1}}% \end{picture}% \endgroup\par\end{figure}$ Figure 8: Star count predictions in the K band (2.15 $\mu$ m) at $l=0^\circ$ , for latitudes 10 $^\circ$ to 90 $^\circ$ from top to bottom (20 $^\circ$ , 45 $^\circ$ and 90 $^\circ$ with solid lines, 10 $^\circ$ , 30 $^\circ$ , 60 $^\circ$ with dashed lines). Data are from the DENIS point source catalogue in indicated directions.
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In the text

$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...ut(360,240){\makebox(0,0)[r]{ 0.1}}% \end{picture}% \endgroup\par\end{figure}$ Figure 9: Star count predictions in the K band (2.15 $\mu$ m) at $l=90^\circ$ or 270 $^\circ$ , for latitudes 0 $^\circ$ to 90 $^\circ$ from top to bottom (0 $^\circ$ , 20 $^\circ$ , 45 $^\circ$ and 90 $^\circ$ with solid lines, 10 $^\circ$ , 30 $^\circ$ , 60 $^\circ$ with dashed lines). For each latitude the bifurcation is due to the warp, the highest part being for l=90, b>0 or l=270, b<0. Data are from the DENIS point source catalogue in indicated directions, and from Kümmel & Wagner (2001) towards the North Ecliptic Pole.
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In the text

$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...t(360,240){\makebox(0,0)[r]{ 0.01}}% \end{picture}% \endgroup\par\end{figure}$ Figure 11: Star count predictions (stars per magnitude and per square degree) in the V band at $l=90^\circ$ and $b=45^\circ$ and contributions of the different luminosity classes. All: solid line, class II: long dashed, class III: short dashed, class IV: dotted, class V: dashed-dotted upper curve, white dwarfs: dashed-dotted lower curve. The giants dominate at V<11, main sequence stars at V>14 in this direction. The rise of the white dwarf curve at V>27 is due to the dark halo white dwarf population normalized here to 2% of the dark halo.
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In the text

$\begin{figure} \par\hbox{\hspace{0cm} \begingroup % \makeatletter% \providecomma... ...25){\makebox(0,0)[r]{-10}}% \end{picture}% \endgroup \hfill }\par\end{figure}$ Figure 12: B-V versus proper motion $\mu _l$ diagrams towards $l=44^\circ$ , $b=474^\circ$ , for stars with 12<V<18. a) Observations from Ojha et al. (1996). b) Simulation.
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In the text

$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...}}% \put(371,225){\makebox(0,0)[r]{ 0}}% \end{picture}% \endgroup\end{figure}$	Figure 1: Luminosity function in the V band in the solar neighbourhood. Crosses with Poisson errors: Jahreiss determination from the revised Catalogue of Nearby Stars; Lines: model LF assuming an IMF slope of $\alpha =1.7$ (solid line) and 1.6 (dashed line) at m<1 $M_{\odot }$ .
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$\begin{figure} \par\includegraphics[width=7cm,clip=,angle=-90]{3188f2.eps} \end{figure}$	Figure 2: Circular velocity of the self-consistent model. Crosses are observational constraints from Caldwell & Ostriker (1981). Contributions from main Galactic components are also given.
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$\begin{figure} \par\includegraphics[width=12cm,clip=,angle=0]{3188f3.eps}\end{figure}$	Figure 3: Star counts in K along a DENIS strip in counts per 0.8 $^\circ$ bin in declination (this strip crosses the plane at $l=266.1^\circ$ ). Data are in solid lines, models in dashed lines. Top panel: flat disc. Middle panel: warped disc. Bottom panel: warped and flaring disc.
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$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...40){\makebox(0,0)[r]{ 0.01}}% \end{picture}% \endgroup \small\par\end{figure}$	Figure 5: Star count predictions (stars per magnitude and per square degree) in the V band at $l=0^\circ$ , for latitudes 10 $^\circ$ to 90 $^\circ$ from top to bottom (20 $^\circ$ , 45 $^\circ$ and 90 $^\circ$ with solid lines, 10 $^\circ$ , 30 $^\circ$ , 60 $^\circ$ with dashed lines). Data are from Ojha et al. (1994a) and Yoshii & Rodgers (1989).
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$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...t(360,240){\makebox(0,0)[r]{ 0.01}}% \end{picture}% \endgroup\par\end{figure}$	Figure 7: Same as figure 5 but for l=180. Data are from Ojha et al. (1994b), Borra & Lepage (1986) and Chiu (1980) in indicated directions.
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$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...ut(360,240){\makebox(0,0)[r]{ 0.1}}% \end{picture}% \endgroup\par\end{figure}$	Figure 8: Star count predictions in the K band (2.15 $\mu$ m) at $l=0^\circ$ , for latitudes 10 $^\circ$ to 90 $^\circ$ from top to bottom (20 $^\circ$ , 45 $^\circ$ and 90 $^\circ$ with solid lines, 10 $^\circ$ , 30 $^\circ$ , 60 $^\circ$ with dashed lines). Data are from the DENIS point source catalogue in indicated directions.
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$\begin{figure} \par\begingroup % \makeatletter% \providecommand{\GNUPLOTspecial}... ...ut(360,240){\makebox(0,0)[r]{ 0.1}}% \end{picture}% \endgroup\par\end{figure}$	Figure 10: Same as figure 8 but at $l=180^\circ$ .
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$\begin{figure} \par\hbox{\hspace{0cm} \begingroup % \makeatletter% \providecomma... ...25){\makebox(0,0)[r]{-10}}% \end{picture}% \endgroup \hfill }\par\end{figure}$	Figure 12: B-V versus proper motion $\mu _l$ diagrams towards $l=44^\circ$ , $b=474^\circ$ , for stars with 12<V<18. a) Observations from Ojha et al. (1996). b) Simulation.
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