Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=10cm,clip]{0368fig1.ps} \end{figure}$ Figure 1: Upper four: morphological evolution of the stellar envelope of the dE,N projected onto the x-z plane (i.e., edge-on view) for the fiducial model. For comparison, the M 31 disk and bulge components are shown in the upper left panel and the disk size is indicated by a solid line in other three panels. The orbit of the dE,N with $R_{\rm apo}$ = 80 kpc and $e_{\rm } = 0.62$ is indicated by a dotted line in the upper left panel. The time T (in units of Gyr) indicated in the upper left corner of each frame represents the time elapsed since the simulation starts. Each frame is 164 kpc on a side. Lower four: morphological evolution of the stellar envelope and the nucleus of the dE,N projected onto the x-y plane (i.e., face-on view) for the fiducial model. Each frame is 20 kpc on a side.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{0368fig2.eps} \end{figure}$ Figure 2: The projected surface density profiles for the dark matter ( solid line), the stellar envelope ( dotted line), the nucleus ( short-dashed line), and all these components ( long-dashed line) at T = 0 Gyr ( upper panel) and 4.8 Gyr ( lower panel) in the fiducial model.
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In the text

$\begin{figure} \par\includegraphics[height=11cm,angle=-90]{0368fig3.eps} \end{figure}$ Figure 3: The final B-band surface brightness $\mu _{B}$ (mag arcsec^-2) distribution projected onto the x-y plane for substructures/tails of M 31's stellar halo developed from tidal destruction of the dE,N in the fiducial model. For comparison with observations by Ferguson et al. (2002), the scale is given in units of degree.
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In the text

$\begin{figure} \par\includegraphics[width=13cm]{0368fig4.eps} \end{figure}$ Figure 4: Final mass distributions projected onto the x-y plane at T = 4.8 Gyr for the fiducial model ( upper left), the smaller $e_{\rm p}$ one with $e_{\rm p} = 0.18$ ( upper right), the smaller $R_{\rm apo}$ with $R_{\rm apo} = 40$ kpc ( lower left), and the more compact dark matter model with $a_{\rm dm}=0.25a_{\rm dm,0}$ ( lower right). Each frame is 240 kpc on a side.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{0368fig2.eps} \end{figure}$	Figure 2: The projected surface density profiles for the dark matter ( solid line), the stellar envelope ( dotted line), the nucleus ( short-dashed line), and all these components ( long-dashed line) at T = 0 Gyr ( upper panel) and 4.8 Gyr ( lower panel) in the fiducial model.
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$\begin{figure} \par\includegraphics[height=11cm,angle=-90]{0368fig3.eps} \end{figure}$	Figure 3: The final B-band surface brightness $\mu _{B}$ (mag arcsec^-2) distribution projected onto the x-y plane for substructures/tails of M 31's stellar halo developed from tidal destruction of the dE,N in the fiducial model. For comparison with observations by Ferguson et al. (2002), the scale is given in units of degree.
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$\begin{figure} \par\includegraphics[width=13cm]{0368fig4.eps} \end{figure}$	Figure 4: Final mass distributions projected onto the x-y plane at T = 4.8 Gyr for the fiducial model ( upper left), the smaller $e_{\rm p}$ one with $e_{\rm p} = 0.18$ ( upper right), the smaller $R_{\rm apo}$ with $R_{\rm apo} = 40$ kpc ( lower left), and the more compact dark matter model with $a_{\rm dm}=0.25a_{\rm dm,0}$ ( lower right). Each frame is 240 kpc on a side.
Open with DEXTER