All Figures

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{1122fig1.ps}} \end{figure}$ Figure 1: The position of the innermost 11 MW satellites (Table 1) as viewed from a point located at infinity and $l=167^{\rm\circ }.91$ . The MW disk is indicated by the horizontal line $-25 \le X/{\rm pc} \le 25$ , and the centre of the coordinate system lies at the Galactic centre. The dashed line marks the fitted plane for N=11 seen edge-on in this projection.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{1122fig2.ps}} \end{figure}$ Figure 2: As Fig. 1 but viewed from $l=77\hbox{$.\!\!^\circ$ }91$ . The fitted plane is here seen face-on.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{1122fig3.ps}} \end{figure}$ Figure 3: The position on the Galactic sky of the poles of the planes fitted to the dwarves of Table 1. Plotted are $b_{\rm P}=-b_{\rm P}'$ and $l_{\rm P}=l_{\rm P}'+180^{\rm\circ }$ and the number of dwarves used for the fit ranges from N=16 down to N=3 (Table 1). The cases for N=3,4,5 are indicated with numbers. The others cluster very tightly around $l_{\rm P}\approx 168^{\rm\circ }, b_{\rm P}\approx -16^{\rm\circ }$ . The likely position of the orbital poles of the LMC, SMC, Draco and UMi are indicated by the solid curves (from Fig. 3 in Palma et al. 2002).
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{1122fig4.ps}} \end{figure}$ Figure 4: The probability, $P_{{\rm cos}\omega }$ , that the observed dwarf sample stems from a parent isotropic radial power-law density distribution with index p. The number of innermost dwarves in the sample (Table 1) is indicated by the numbers. Thus 11, for example, means that the innermost N=11 dwarves (out to and including LeoI) are compared with the isotropic power-law distribution. The thin curves (and numbers in parentheses) are probabilities calculated by excluding SMC and UMi from the data; here N=(9) incorporates all dwarves except SMC and UMi out to and including LeoI (Table 1). The increase of $P_{\cos~\omega}$ with decreasing N and (N) is a result of weakening confidence as the number of observed data is reduced. The decrease of $P_{\cos~\omega}$ for p>2.4 comes from the theoretical distribution being increasingly concentrated towards the Galactic centre while the plane lies off-centre ( $D_{\rm P}>0$ ).
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{1122fig1.ps}} \end{figure}$	Figure 1: The position of the innermost 11 MW satellites (Table 1) as viewed from a point located at infinity and $l=167^{\rm\circ }.91$ . The MW disk is indicated by the horizontal line $-25 \le X/{\rm pc} \le 25$ , and the centre of the coordinate system lies at the Galactic centre. The dashed line marks the fitted plane for N=11 seen edge-on in this projection.
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$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{1122fig2.ps}} \end{figure}$	Figure 2: As Fig. 1 but viewed from $l=77\hbox{$.\!\!^\circ$ }91$ . The fitted plane is here seen face-on.
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