Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{ms3537f14.ps} \end{figure}$ Figure 2: The parameters of the best-fitting Sérsic model, central surface brightness ( $\mu _0$ ), scale length (r₀), and shape indicator (n), plotted versus absolute magnitude for different galaxy types. All data are in the B-band. Es and S0s are from Caon et al. (1993), Local Group dSphs are from Jerjen et al. (2000) and dE, (N)s/dS0, (N)s are from this study. Added as well is the large photographic sample of Virgo early-type dwarfs from Binggeli & Jerjen (1998), shown as dots.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{ms3537f15.ps} \end{figure}$ Figure 3: Effective surface brightness in R plotted versus the mean, absolute residual between profile observed and model-profile (see text for details). The error bars represent the mean error of the profile in the corresponding range.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{ms3537f16.ps} \end{figure}$ Figure 4: Comparison of our total apparent magnitude in B (filled circles) and R(open circles) (upper panel) and of the central surface brightness from the Sérsic fit in B (filled circles) and R (open circles) (lower panel) to data from the literature.
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{ms3537f17.ps} \end{figure}$ Figure 5: Isophotal contours of the R-band images. The galaxy name is given in the upper left corner. The surface brightness of the innermost isophote is indicated in the upper right corner, the interval is 0.25 mag. The images are $1 \hbox {$.\mkern -4mu^\prime $ }7$ on a side, corresponding to $\sim$ 8 kpc.
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{ms3537f18.ps} \end{figure}$ Figure 5: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{ms3537f19.ps} \end{figure}$ Figure 6: Ellipticity versus shape parameter represented as a₄/a*100 for dE, (N)s (solid circles) and dS0, (N)s (open circles). The lines are the same like in Fig. 1 of Bender et al. (1989) and indicate the distribution of giant ellipticals. Shown are also the $1 \sigma$ errors of the averaging.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{ms3537f20.ps} \end{figure}$ Figure 7: The logarithm of the nuclear offset versus the effective surface brightness in R. The dashed line indicates our lower detection limit of $0.2 \hbox {$^{\prime \prime }$ }$ , i.e. offsets above this line are real and, in fact, lower limits of the true displacements. The error bars are the $1 \sigma$ errors of the averaging. The meaning of the symbols is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms3537f21.ps} \end{figure}$ Figure 8: The logarithm of the nuclear offset versus the residual effective surface brightness, calculated with respect to the mean relation between effective surface brightness and absolute magnitude (in R), for dE, N galaxies only. Dashed line as in Fig. 7.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms3537f22.ps} \end{figure}$ Figure 9: Isophotal twist, $\Delta \rm PA$ , versus ellipticity. The meaning of the symbols is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{ms3537f23.ps} \end{figure}$ Figure 10: Isophotal twist, $\Delta \rm PA$ , versus the corresponding change of ellipticity, $\Delta \epsilon$ , for galaxies with $\epsilon < 0.3$ . (Two plot symbols strongly overlap at $\Delta \epsilon \approx 0$ , $\Delta \rm PA \approx 29$ .)
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{ms3537f24.ps} \end{figure}$ Figure 11: Isophotal twist, $\Delta \rm PA$ , versus the logarithm of $\delta _N$ . The dashed line indicates our lower detection limit of $0 \hbox{$.\!\!^{\prime\prime}$ }2$ . The meaning of the symbols is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f01.ps} \end{figure}$ Figure 1: Plots of the basic parameters for the photometry and the isophotal analysis versus equivalent radius $\sqrt {ab}$ , where a and b are the major- and minor-axis, respectively. For the errors of the photometric parameters (left column) the remaining gradient on the frames after the flat-fielding and the amount of the background subtracted have been taken into account. The fact that in some cases only a quarter of the galaxy light in the outer parts could be integrated is not considered in the error estimates. Error bars are only shown for every other data point. The errors of the isophotal parameters (right column) have been derived by means of a Fourier expansion (for details see Bender & Möllenhoff 1987). Ellipses have only been fitted to isophotes completely present on the frames. The error bars are mostly smaller than the plot symbols. Upper left: surface brightness profiles in B (lower curve, where available) and R (upper curve). Error bars are only shown for the profile in B(or in R, if B is not available). A tick mark indicates the confidence limit of our photometry in R (Table 2, Col. 3), if not present, it roughly corresponds to the right margin of the plot. Middle left: model profile (from a Sérsic fit) minus profile observed in R. Lower left: B-R colour-profile. Upper right: ellipticity profile in R. Middle right: profile of the position angle of the major-axis in R, from top counterclockwise. Lower right: the profile of the isophotal shape parameter a₄ in R expressed as a₄/a*100, where a is the length of the major-axis of the corresponding isophote.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f02.ps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f03.ps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f04.ps} \end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f05.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f06.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f07.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f08.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f09.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f10.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f11.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\par\includegraphics[width=13.6cm,clip]{ms3537f12.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f13.ps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{ms3537f15.ps} \end{figure}$	Figure 3: Effective surface brightness in R plotted versus the mean, absolute residual between profile observed and model-profile (see text for details). The error bars represent the mean error of the profile in the corresponding range.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{ms3537f16.ps} \end{figure}$	Figure 4: Comparison of our total apparent magnitude in B (filled circles) and R(open circles) (upper panel) and of the central surface brightness from the Sérsic fit in B (filled circles) and R (open circles) (lower panel) to data from the literature.
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$\begin{figure} \par\includegraphics[width=16.7cm,clip]{ms3537f17.ps} \end{figure}$	Figure 5: Isophotal contours of the R-band images. The galaxy name is given in the upper left corner. The surface brightness of the innermost isophote is indicated in the upper right corner, the interval is 0.25 mag. The images are $1 \hbox {$.\mkern -4mu^\prime $ }7$ on a side, corresponding to $\sim$ 8 kpc.
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$\begin{figure} \par\includegraphics[width=16.7cm,clip]{ms3537f18.ps} \end{figure}$	Figure 5: continued.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{ms3537f19.ps} \end{figure}$	Figure 6: Ellipticity versus shape parameter represented as a₄/a*100 for dE, (N)s (solid circles) and dS0, (N)s (open circles). The lines are the same like in Fig. 1 of Bender et al. (1989) and indicate the distribution of giant ellipticals. Shown are also the $1 \sigma$ errors of the averaging.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{ms3537f20.ps} \end{figure}$	Figure 7: The logarithm of the nuclear offset versus the effective surface brightness in R. The dashed line indicates our lower detection limit of $0.2 \hbox {$^{\prime \prime }$ }$ , i.e. offsets above this line are real and, in fact, lower limits of the true displacements. The error bars are the $1 \sigma$ errors of the averaging. The meaning of the symbols is indicated.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms3537f21.ps} \end{figure}$	Figure 8: The logarithm of the nuclear offset versus the residual effective surface brightness, calculated with respect to the mean relation between effective surface brightness and absolute magnitude (in R), for dE, N galaxies only. Dashed line as in Fig. 7.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms3537f22.ps} \end{figure}$	Figure 9: Isophotal twist, $\Delta \rm PA$ , versus ellipticity. The meaning of the symbols is indicated.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{ms3537f23.ps} \end{figure}$	Figure 10: Isophotal twist, $\Delta \rm PA$ , versus the corresponding change of ellipticity, $\Delta \epsilon$ , for galaxies with $\epsilon < 0.3$ . (Two plot symbols strongly overlap at $\Delta \epsilon \approx 0$ , $\Delta \rm PA \approx 29$ .)
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{ms3537f24.ps} \end{figure}$	Figure 11: Isophotal twist, $\Delta \rm PA$ , versus the logarithm of $\delta _N$ . The dashed line indicates our lower detection limit of $0 \hbox{$.\!\!^{\prime\prime}$ }2$ . The meaning of the symbols is indicated.
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$\begin{figure} \par\includegraphics[width=13.6cm,clip]{ms3537f02.ps} \end{figure}$	Figure 1: continued.
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