All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,height=5.2cm,clip]{4081fig1.ps} \end{figure}$ Figure 1: The distribution pulsars in the Manchester et al. (2005) catalog. Filled squares and open circles are pulsars with Galactocentric distances between 1 and 5 kpc, and 5 and 10 kpc respectively. Open triangles are pulsars at $R_{\rm GC}\ge 10$ kpc.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,height=10cm,clip]{4081fig2.ps}\end{figure}$ Figure 2: The upper 4 panels display a Besançon $1^{\circ }$ square area simulated color-magnitude diagram around CMa ( $l,b)=(240^{\circ },-7^{\circ })$ . These show the expected different contributions of stars as a function of their distance. The lowest panel displays data from 2MASS between $238^{\circ}\le~l~\le242^{\circ}$ and $-8^{\circ}\le~b~\le-6^{\circ}$ . The outlined vertical boxes mark 4 distance intervals as selected from the red clump distribution in simulated diagrams. The 3 oblique boxes trace 3 samples of red giant stars extracted at three different heliocentric distances. The thick line is the Majewski et al. calibration of the Sagittarius dwarf RGB, shifted to 2.8, 7.3 and 16.6 kpc.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,height=8.2cm,clip]{4081fig3.ps} \end{figure}$ Figure 3: A schematic view (from Drimmel & Spergel 2001) of the Milky Way as seen from its North pole showing the 4 spiral arms as mapped by H II regions and dust (see also Vallée 2005; and Russeil 2003). The Galactic center, the Sun and the names of the spiral arms are plotted. Note the presence of the Local arm (Orion-Cygnus) close to the Sun's position and the outer arm that is also called Norma-Cygnus. The 3 heliocentric circles define the regions at fixed $R_{\odot }$ where we extract RGB samples to trace the Galactic warp and flare. The direction of the warp phase angle $\phi$ , and longitude directions are also plotted. We have also added the Galactic bar at an orientation angle of $14^{\circ }$ (following Freudenreich 1998) with length 3 kpc (following Vallée 2005). Note however that a recent Galactic Legacy Mid-Plane Survey Extraordinaire (GLIMPSE) study by Benjamin et al. (2005) report on a linear Galactic bar with half-length of $4.4\pm 0.5$ kpc.
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In the text

$\begin{figure} \par\hspace*{2mm}\includegraphics[width=7.2cm,height=4.8cm,clip]{... ...{2mm} \includegraphics[width=7.5cm,height=8.1cm,clip]{4081fig5.ps} \end{figure}$ Figure 4: The upper panels display two examples of the derivation of best warp angles and their relative error by means of a reduced $\chi ^2$ . The lower panels show the latitude profiles for a third field: (i) assuming no warp ( upper panel) and; (ii) having derived the best warp angle ( lower panel). The dashed and solid lines refer to the Northern and Southern latitude profiles, respectively. All panels refer to the RGB sample at $R_{\odot }=7.3$ kpc.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,height=5.2cm]{4081fig6.ps}\end{figure}$ Figure 5: An example of deriving the scale height ( $Z_{\rm h}$ ) from the RGB sample at $R_{\odot }=16.6$ kpc. The filled circles show the Northern hemisphere latitude profile while the open circles show the Southern profile. Vertical lines delimit the region where we apply a linear fit (dotted line) to the data.
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In the text

$\begin{figure} \includegraphics[width=8.3cm,height=8.2cm,clip]{4081fig7.ps} \end{figure}$ Figure 6: The relative luminosity contribution of the three stellar populations in the J band ( upper panel) and K band ( middle panel). The lower figure shows the cumulative distributions of the distances of RGB stars without any luminosity-weighting along the line of sight (dark line). The grey line shows instead the distance-weighted distribution.
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In the text

$\begin{figure} \includegraphics[width=8cm,height=8.2cm,clip]{4081fig8.ps}\end{figure}$ Figure 7: The stellar warp as derived from RC stars at $R_{\odot }\le 2$ kpc (filled squares). The results are compared with the latitude of peak brightness obtained from DIRBE at wavelengths 1.2, 3.5 and 240 $\mu$ m by Freudenreich et al. (1994, grey open triangles).
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In the text

$\begin{figure} \includegraphics[width=8cm,height=8.2cm,clip]{4081fig9.ps}\end{figure}$ Figure 8: The stellar warp as derived from RC stars for 4 distance intervals (dark filled squares). The results are compared with the latitude of peak brightness obtained from DIRBE at wavelengths 3.5 and 240 $\mu$ m by Freudenreich et al. (1994, grey open triangles).
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In the text

$\begin{figure} \par\includegraphics[width=14cm,height=14cm,clip]{4081fig10.ps}\p... ...{2mm} \includegraphics[width=14.5cm,height=7.5cm,clip]{4081fig11.ps}\end{figure}$ Figure 9: The upper left panel displays the stellar warp as derived from red giants at $R_{\odot }\simeq 7.3$ kpc. In the lower left panel we compare the derived warp with those based on two RC samples between: (i) $6\le~R_{\odot}\le 8$ , and (ii) $0\le~R_{\odot}\le 8$ kpc. The upper right panel over-plots the dust warp as derived from DIRBE at $240~\mu$ m data, whereas the lower right panel over-plots the Galactic warp as derived from neutral H I gas (also from Freudenreich et al. 1994). The lower panel shows the density maps and contours of the $R_{\odot }\simeq 7.3$ RGB sample. One can trace by eye the warp signature (a colored version is more appropriate). Over-plotted is also the location of the mean mid-plane warped disk as a function of longitude.
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In the text

$\begin{figure} \includegraphics[width=8cm,height=8cm,clip]{4081fig12.ps} \end{figure}$ Figure 10: Same as Fig. 9, but for RGB stars at $R_{\odot }\simeq 16.6$ kpc. Note the structure ("swelling'') around $l\sim 160^{\circ }$ and how the the agreement with H I is better with respect to the $R_{\odot }\simeq 7.3$ kpc sample.
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In the text

$\begin{figure} \includegraphics[width=8cm,clip]{4081fig13.ps} \end{figure}$ Figure 11: A comparison of our Galactic stellar disk warp height $Z-{\it warp}$ (kpc), as obtained from the RGB sample at heliocentric distances of 7.3 kpc points with error bars, with models based on stellar tracers lines. Note the excellent agreement between data and models for the Southern warp. The disagreement for the Northern warp is explained in the text.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,height=7.8cm,clip]{4081fig14.ps}\end{figure}$ Figure 12: The Galactic stellar disk warp height as derived from the RGB samples at $R_{\odot }=2.8$ and 7.3 kpc compared with the Yusifov (2004) model.
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In the text

$\begin{figure} \includegraphics[width=7.8cm,height=7.8cm,clip]{4081fig15.ps} \end{figure}$ Figure 13: The Galactic stellar disk warp height as derived from the RGB sample at $R_{\odot }=16.6$ kpc improperly compared with the Yusifov (2004) model (not applicable at these distances). Note that for Galactocentric distances greater than 14 kpc the model imposes a constant Southern stellar warp so as to be consistent with the derived parameters of the gaseous warp.
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In the text

$\begin{figure} \includegraphics[width=8cm,clip]{4081fig16.ps}\end{figure}$ Figure 14: Variation of the scale-height (derived from the $R_{\odot }=2.8$ , 7.3 and 16.6 kpc RGB samples) as a function of Galactocentric distances. We also show a comparison of our results with two models and data-points from Alard (2000).
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In the text

$\begin{figure} \includegraphics[width=7.2cm,height=4.2cm,clip]{4081fig17.ps} \end{figure}$ Figure 15: A comparison of the thickness of the stellar disk, neutral hydrogen gas layer and molecular clouds ensemble for the outer Milky Way. Filled squares show the flaring for the RGB samples at $R_{\odot }=7.3$ and 16.6 kpc, whereas the open squares plot the RGB samples at $R_{\odot }=2.8$ kpc.
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In the text

$\begin{figure} \includegraphics[width=8cm,height=4.8cm,clip]{4081fig18.ps}\end{figure}$ Figure 16: A cut in the YZ plane of the warped and flared Galaxy using the Yusifov warp model in the direction and at the distance of CMa. The thick line marks the mean warped stellar disk whereas the grey dashed lines trace the density at $1\times$ , $2\times$ and $3\times$ the scale-height of the disk.
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In the text

$\begin{figure} \includegraphics[width=7.5cm,height=7cm,clip]{4081fig19.ps}\par\... ...*{2mm} \includegraphics[width=7.5cm,height=7cm,clip]{4081fig20.ps} \end{figure}$ Figure 17: The same as in Fig. 16 but for fields where positive detections of the Mon. Ring have been reported. For the Sloan detections ( upper three panels) we plot detections at heliocentric distances of 7, 8, 9 and 10 kpc. Similarly, the lower three panels show INT detections (Conn et al. 2005; Ibata et al. 2003) plotted at the distances given in Table 3 of Conn et al.
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In the text

$\begin{figure} \includegraphics[width=10.3cm,height=10.3cm,clip]{4081fig21.ps}\end{figure}$ Figure A.1: Explaining the "peculiar'' $R_{\odot }-V_{\rm rad}$ relation found for CMa stars as due to Galactic differential rotation. The left panel shows a Besançon simulated $R_{\odot }-V_{\rm rad}$ distribution for stars at the CMa center. Grey dots highlight the modeled Thin Disk truncation at $R_{\odot }=7.7$ kpc (marked by a horizontal line). Black dots plot the Thick Disk and Halo stars. Open triangles show the $R_{\odot }-V_{\rm rad}$ distribuition for simulated stars extracted from the synthetic color-magnitude diagram (upper right panel), and falling within a box delimiting the RC region between $5\le R_{\odot } \le 8$ kpc. The open squares are the observed-RC sample from Martin et al. (their Fig. 6). Right middle panel shows the distribution of radial velocities of the Martin et al. observed-RC sample (dashed histogram), and the scaled distribution of simulated-RC stars (continuous histogram). The right lower panel shows the mean $V_{\rm rad}$ of the dwarfs-decontaminated and RC-simulated sample (open triangles) estimated in three distance intervals. The open squares plot the observed mean $V_{\rm rad}$ values for CMa RC stars (see Table 2 of Martin et al.) in the same distance intervals. The error bars are from the same table. The Dashed line is a linear fit to the Martin et al. mean values; which is fully compatible with recent estimates of the A Oort constant being $A=17.23\pm 0.35$ .

In the text

$\begin{figure} \includegraphics[width=7.5cm,height=7.5cm,clip]{4081fig22.ps}\end{figure}$ Figure B.1: A 1 $^{\rm o}$ dereddened color-magnitude diagrams of the core of CMa. Over-plotted is a 6.3 Gyr Z=0.004 ([Fe/H $]\simeq -0.76$ ) isochrone from The Girardi et al. (2002) library. The assumed distance modulus is (m-M)₀=14.5. Each star was dereddened according to its position in the Schlegel et al. (1998) reddening maps. Also plotted are the red clump and blue horizontal branch location of the Sagittarius, as derived by Monaco et al. (2003).

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,height=5.2cm,clip]{4081fig1.ps} \end{figure}$	Figure 1: The distribution pulsars in the Manchester et al. (2005) catalog. Filled squares and open circles are pulsars with Galactocentric distances between 1 and 5 kpc, and 5 and 10 kpc respectively. Open triangles are pulsars at $R_{\rm GC}\ge 10$ kpc.
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$\begin{figure} \par\includegraphics[width=7.1cm,height=5.2cm]{4081fig6.ps}\end{figure}$	Figure 5: An example of deriving the scale height ( $Z_{\rm h}$ ) from the RGB sample at $R_{\odot }=16.6$ kpc. The filled circles show the Northern hemisphere latitude profile while the open circles show the Southern profile. Vertical lines delimit the region where we apply a linear fit (dotted line) to the data.
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$\begin{figure} \includegraphics[width=8.3cm,height=8.2cm,clip]{4081fig7.ps} \end{figure}$	Figure 6: The relative luminosity contribution of the three stellar populations in the J band ( upper panel) and K band ( middle panel). The lower figure shows the cumulative distributions of the distances of RGB stars without any luminosity-weighting along the line of sight (dark line). The grey line shows instead the distance-weighted distribution.
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$\begin{figure} \includegraphics[width=8cm,height=8.2cm,clip]{4081fig8.ps}\end{figure}$	Figure 7: The stellar warp as derived from RC stars at $R_{\odot }\le 2$ kpc (filled squares). The results are compared with the latitude of peak brightness obtained from DIRBE at wavelengths 1.2, 3.5 and 240 $\mu$ m by Freudenreich et al. (1994, grey open triangles).
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$\begin{figure} \includegraphics[width=8cm,height=8.2cm,clip]{4081fig9.ps}\end{figure}$	Figure 8: The stellar warp as derived from RC stars for 4 distance intervals (dark filled squares). The results are compared with the latitude of peak brightness obtained from DIRBE at wavelengths 3.5 and 240 $\mu$ m by Freudenreich et al. (1994, grey open triangles).
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$\begin{figure} \includegraphics[width=8cm,height=8cm,clip]{4081fig12.ps} \end{figure}$	Figure 10: Same as Fig. 9, but for RGB stars at $R_{\odot }\simeq 16.6$ kpc. Note the structure ("swelling'') around $l\sim 160^{\circ }$ and how the the agreement with H I is better with respect to the $R_{\odot }\simeq 7.3$ kpc sample.
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$\begin{figure} \includegraphics[width=8cm,clip]{4081fig13.ps} \end{figure}$	Figure 11: A comparison of our Galactic stellar disk warp height $Z-{\it warp}$ (kpc), as obtained from the RGB sample at heliocentric distances of 7.3 kpc points with error bars, with models based on stellar tracers lines. Note the excellent agreement between data and models for the Southern warp. The disagreement for the Northern warp is explained in the text.
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$\begin{figure} \par\includegraphics[width=7.8cm,height=7.8cm,clip]{4081fig14.ps}\end{figure}$	Figure 12: The Galactic stellar disk warp height as derived from the RGB samples at $R_{\odot }=2.8$ and 7.3 kpc compared with the Yusifov (2004) model.
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$\begin{figure} \includegraphics[width=7.8cm,height=7.8cm,clip]{4081fig15.ps} \end{figure}$	Figure 13: The Galactic stellar disk warp height as derived from the RGB sample at $R_{\odot }=16.6$ kpc improperly compared with the Yusifov (2004) model (not applicable at these distances). Note that for Galactocentric distances greater than 14 kpc the model imposes a constant Southern stellar warp so as to be consistent with the derived parameters of the gaseous warp.
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$\begin{figure} \includegraphics[width=8cm,clip]{4081fig16.ps}\end{figure}$	Figure 14: Variation of the scale-height (derived from the $R_{\odot }=2.8$ , 7.3 and 16.6 kpc RGB samples) as a function of Galactocentric distances. We also show a comparison of our results with two models and data-points from Alard (2000).
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$\begin{figure} \includegraphics[width=7.2cm,height=4.2cm,clip]{4081fig17.ps} \end{figure}$	Figure 15: A comparison of the thickness of the stellar disk, neutral hydrogen gas layer and molecular clouds ensemble for the outer Milky Way. Filled squares show the flaring for the RGB samples at $R_{\odot }=7.3$ and 16.6 kpc, whereas the open squares plot the RGB samples at $R_{\odot }=2.8$ kpc.
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$\begin{figure} \includegraphics[width=8cm,height=4.8cm,clip]{4081fig18.ps}\end{figure}$	Figure 16: A cut in the YZ plane of the warped and flared Galaxy using the Yusifov warp model in the direction and at the distance of CMa. The thick line marks the mean warped stellar disk whereas the grey dashed lines trace the density at $1\times$ , $2\times$ and $3\times$ the scale-height of the disk.
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$\begin{figure} \includegraphics[width=7.5cm,height=7cm,clip]{4081fig19.ps}\par\... ...*{2mm} \includegraphics[width=7.5cm,height=7cm,clip]{4081fig20.ps} \end{figure}$	Figure 17: The same as in Fig. 16 but for fields where positive detections of the Mon. Ring have been reported. For the Sloan detections ( upper three panels) we plot detections at heliocentric distances of 7, 8, 9 and 10 kpc. Similarly, the lower three panels show INT detections (Conn et al. 2005; Ibata et al. 2003) plotted at the distances given in Table 3 of Conn et al.
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