Astronomy & Astrophysics

All Figures

$\begin{figure} \par {\includegraphics[width=8.3cm,clip]{2675f1.eps} } \end{figure}$ Figure 1: The radial distribution of satellite galaxies. The solid circles are the distribution of the 11 inner satellites observed in the Milky Way (Mateo 1998; Kroupa et al. 2004); the Poisson error is indicated for each data point. The thick solid line is the dark matter profile and the thin solid line is for the substructures. The dotted line with triangles is for the satellite galaxies (brighter than M_V=-12) in galactic halos predicted by the semi-analytical model of Kang et al. (2004), and the dashed line is for the sample selected by mass at accretion (see text). Here the radius is normalized to the virial radius and the virial radius of the Milky Way is taken to be 250 kpc.
Open with DEXTER

In the text

$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{2675f2.eps} } \end{figure}$ Figure 2: The distribution of the rms of the scale height from a plane defined by satellite galaxies obtained through many Monte Carlo realizations. The four panels are for four different galactic-sized halos. The histograms without symbols show the result expected if the satellite galaxies follow the dark matter distribution while the histograms with symbols show those if satellites follow the subhalo distribution. The thick solid histograms are for 11 satellite galaxies, while the thin solid histograms are for 22 satellite galaxies. The horizontal bar in the top left panel shows the range of $\Delta /R_{\rm cut}$ for the observed satellites when different numbers of satellite galaxies are used (see Table 1 in Kroupa et al. 2004).
Open with DEXTER

In the text

$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{2675f3.eps} } \end{figure}$ Figure 3: The distribution of the rms of the angle (in degrees) between the plane defined by satellite galaxies and the plane defined by the major and medium axes in the triaxial halo model (see text). The dashed line is the prediction if the angle between the satellite plane and the minor axis of the halo is randomly distributed on the sky. The other line symbols are the same as in Fig. 2. In each panel we label the ratio of the minor, medium and maximum axes. In parentheses we indicate the angle between the angular momentum vector and the minor axis of the triaxial model.
Open with DEXTER

In the text

$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{2675f4.eps} } \end{figure}$ Figure 4: A scatter plot of $\theta$ vs. $\Delta /R_{\rm cut}$ for the satellites selected from the dark matter particles. $\theta$ is the same as that in Fig. 3.
Open with DEXTER

In the text

$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{2675f4.eps} } \end{figure}$	Figure 4: A scatter plot of $\theta$ vs. $\Delta /R_{\rm cut}$ for the satellites selected from the dark matter particles. $\theta$ is the same as that in Fig. 3.
Open with DEXTER