Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{0571f01.ps} \end{figure}$ Figure 1: The N-E region of the Virgo cluster including galaxies with $m_{\rm p}\leq 19.0$ . The dashed line represents the boundary of the VCC catalog. The rectangles include the studied WFH and WFV areas, covering approximately 26 $\rm deg^2$ . The location of M 87 is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0571f02.ps} \end{figure}$ Figure 2: The luminosity function of E (filled symbols) and dE (open symbols) in the WFS. The completeness limit of the VCC ( $m_{\rm p}=18$ ) is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0571f03.ps}\end{figure}$ Figure 3: Distribution of the seeing in the WFS.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0571f04.ps} \end{figure}$ Figure 4: The effect of the seeing on n ( left) and on $\mu _0$ ( right) as derived from the simulations (lines) for various n. Dots give the distribution of the observed points in the $n-r_{\rm e}/\sigma$ plane.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{0571f05.ps} \end{figure}$ Figure 5: Comparison of B_T from this work with $m_{\rm p}$ from the VCC. The dotted line gives the bisector linear regression. In this and in the following figures (unless otherwhise specified) empty symbols refer to dEs, filled symbols to Es and asterisks to "core'' galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0571f06.ps} \end{figure}$ Figure 6: Comparison among structural parameters derived in this work and by Young & Currie (1998) for 42 common galaxies ( right) and by Binggeli & Jerijn (1998) for 37 common galaxies ( left).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0571f07.ps} \end{figure}$ Figure 7: Comparison among structural parameters derived in this work and by Barazza et al. (2003) for 5 common galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{0571f08a.ps}\par\vspace*{2... ...s}\par\vspace*{2mm} \includegraphics[width=5.5cm,clip]{0571f08c.ps} \end{figure}$ Figure 8: The outer B-I color index ( top); the inner B-I color index ( middle; the two brightest objects are missing in this panel because they are both saturated) and the outer B-I gradient ( bottom) as a function of B_T. In this figure filled dots represent giant Es, empty dots dEs, asterisks Nucleated dEs.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0571f09.ps} \end{figure}$ Figure 9: The dependence of n from B_T. The dashed line gives the bisector linear regression.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{0571f10a.ps}\par\vspace*{2... ...s}\par\vspace*{2mm} \includegraphics[width=6.2cm,clip]{0571f10c.ps} \end{figure}$ Figure 10: Correlations among structural parameters of dE-E galaxies in the Virgo cluster. B_T vs. $\langle \mu\rangle_{\rm e}$ ( top); $\langle \mu\rangle_{\rm e}$ vs. $\log ~ R_{\rm e}$ ( middle); B_T vs. $\log ~ R_{\rm e}$ ( bottom). The position of M 32 (scaled to the distance of Virgo and corrected for B-V=1) as given by Faber et al. (1997) is marked with a cross. The dotted rectangle represents the loci of luminous "core'' galaxies adapted from GG03.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{0571f11.ps} \end{figure}$ Figure 11: Correlation between B_T and $\mu _0$ for dE-E galaxies in the Virgo cluster. The position of M 32 is marked with a cross. The dotted rectangle represents the loci of luminous "core'' galaxies adapted from GG03. The dashed line gives the bisector linear regression.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{0571f12.ps} \end{figure}$ Figure 12: Distribution of C₃₁ versus n. The dashed line gives the bisector linear regression: $C_{31}= 1.49 \times n+1.33$ .
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f13a.eps}\end{figure}$ Figure 13: The 136 individual B-band profiles and their Sersic fit. The vertical dashed line marks the seeing.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f13b.eps}\end{figure}$ Figure 13: continued.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f13c.eps}\end{figure}$ Figure 13: continued.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f13d.eps}\end{figure}$ Figure 13: continued.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f14a.eps}\end{figure}$ Figure 14: The profiles and their Sersic fit for 90 galaxies in the WFV with B and I band imaging and their B-I color profile. I Images are convolved to the seeing of B images, marked by the vertical dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f14b.eps}\end{figure}$ Figure 14: continued.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f14c.eps}\end{figure}$ Figure 14: continued.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f14d.eps}\end{figure}$ Figure 14: continued.
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In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{0571f01.ps} \end{figure}$	Figure 1: The N-E region of the Virgo cluster including galaxies with $m_{\rm p}\leq 19.0$ . The dashed line represents the boundary of the VCC catalog. The rectangles include the studied WFH and WFV areas, covering approximately 26 $\rm deg^2$ . The location of M 87 is indicated.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0571f02.ps} \end{figure}$	Figure 2: The luminosity function of E (filled symbols) and dE (open symbols) in the WFS. The completeness limit of the VCC ( $m_{\rm p}=18$ ) is indicated.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0571f03.ps}\end{figure}$	Figure 3: Distribution of the seeing in the WFS.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0571f04.ps} \end{figure}$	Figure 4: The effect of the seeing on n ( left) and on $\mu _0$ ( right) as derived from the simulations (lines) for various n. Dots give the distribution of the observed points in the $n-r_{\rm e}/\sigma$ plane.
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{0571f05.ps} \end{figure}$	Figure 5: Comparison of B_T from this work with $m_{\rm p}$ from the VCC. The dotted line gives the bisector linear regression. In this and in the following figures (unless otherwhise specified) empty symbols refer to dEs, filled symbols to Es and asterisks to "core'' galaxies.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0571f06.ps} \end{figure}$	Figure 6: Comparison among structural parameters derived in this work and by Young & Currie (1998) for 42 common galaxies ( right) and by Binggeli & Jerijn (1998) for 37 common galaxies ( left).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0571f07.ps} \end{figure}$	Figure 7: Comparison among structural parameters derived in this work and by Barazza et al. (2003) for 5 common galaxies.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{0571f08a.ps}\par\vspace{2... ...s}\par\vspace{2mm} \includegraphics[width=5.5cm,clip]{0571f08c.ps} \end{figure}$	Figure 8: The outer B-I color index ( top); the inner B-I color index ( middle; the two brightest objects are missing in this panel because they are both saturated) and the outer B-I gradient ( bottom) as a function of B_T. In this figure filled dots represent giant Es, empty dots dEs, asterisks Nucleated dEs.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0571f09.ps} \end{figure}$	Figure 9: The dependence of n from B_T. The dashed line gives the bisector linear regression.
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$\begin{figure} \par\includegraphics[width=6.2cm,clip]{0571f11.ps} \end{figure}$	Figure 11: Correlation between B_T and $\mu _0$ for dE-E galaxies in the Virgo cluster. The position of M 32 is marked with a cross. The dotted rectangle represents the loci of luminous "core'' galaxies adapted from GG03. The dashed line gives the bisector linear regression.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{0571f12.ps} \end{figure}$	Figure 12: Distribution of C₃₁ versus n. The dashed line gives the bisector linear regression: $C_{31}= 1.49 \times n+1.33$ .
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$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f13a.eps}\end{figure}$	Figure 13: The 136 individual B-band profiles and their Sersic fit. The vertical dashed line marks the seeing.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f13b.eps}\end{figure}$	Figure 13: continued.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f14a.eps}\end{figure}$	Figure 14: The profiles and their Sersic fit for 90 galaxies in the WFV with B and I band imaging and their B-I color profile. I Images are convolved to the seeing of B images, marked by the vertical dashed line.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{0571f14b.eps}\end{figure}$	Figure 14: continued.
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