Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=4.2cm,clip]{2198f01a.ps}\includegraphi... ...s}\includegraphics[width=4.2cm,clip]{2198f01j.ps}\hspace*{4.2cm}} \end{figure}$ Figure 1: Reduced R-band images of the ten sample galaxies with the boundaries of the analysed square SBF fields indicated. The field-of-view is $2.5 \times 2.5$ arcmin. North is up, East to the left.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2198f02.ps} \end{figure}$ Figure 2: After subtracting the best-fitting model of the global light distribution a well developed 4-armed spiral structure and traces of dust in the central region become visible in the residual image of NGC 4150. These findings confirm the morphological type of S0/Sa for this galaxy.
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In the text

$\begin{figure} \par\includegraphics[height=6.9cm,width=10.9cm,clip]{2198f03l.ps}... ...*{3mm} \includegraphics[height=6.9cm,width=4.7cm,clip]{2198f03r.ps} \end{figure}$ Figure 3: Left: five fields were selected for the SBF analysis in UGC 1703. The signal-to-noise in the power spectra is generally high. The power spectra of the SBF fields (filled circles) are well fitted by the sum (solid line) of a scaled version of the power spectrum of the PSF and a constant (dashed lines). The wavenumbers 1-4 were not considered for the fit. Right: the fluctuation magnitudes $\overline {m}_R$ and (B-R) colours were measured for the five fields to derive the distance of UGC 1703. A shift by 28.11 mag yields the best fit of the data to the calibration diagram.
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In the text

$\begin{figure} \par\includegraphics[height=6.9cm,width=10.9cm,clip]{2198f04l.ps}... ...*{3mm} \includegraphics[height=6.9cm,width=4.7cm,clip]{2198f04r.ps} \end{figure}$ Figure 4: Left: six fields were selected for the SBF analysis in KDG 61. The power spectra of the SBF fields (filled circles) are well fitted by the sum (solid line) of a scaled version of the power spectrum of the PSF and a constant (dashed lines). The wavenumbers 1-4 were not considered for the fit. Right: the fluctuation magnitudes $\overline {m}_R$ and (B-R) colours were measured for the six fields to derive the distance of KDG 61. A shift by 27.80 mag yields the best fit of the data to the calibration diagram.
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In the text

$\begin{figure} \par\includegraphics[height=6.9cm,width=10.9cm,clip]{2198f05l.ps}... ...*{3mm} \includegraphics[height=6.9cm,width=4.7cm,clip]{2198f05r.ps} \end{figure}$ Figure 5: Left: five fields were selected for the SBF analysis in UGCA 200. The power spectra of the SBF fields (filled circles) are well fitted by the sum (solid line) of a scaled version of the power spectrum of the PSF and a constant (dashed lines). The wavenumbers 1-4 were not considered for the fit. Right: the fluctuation magnitudes $\overline {m}_R$ and (B-R) colours were measured for the five fields to derive the distance of UGCA 200. A shift by 29.01 mag yields the best fit of the data to the linear branch of the calibration diagram.
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In the text

$\begin{figure} \par\includegraphics[height=6.9cm,width=10.9cm,clip]{2198f06l.ps}... ...*{3mm} \includegraphics[height=6.9cm,width=4.7cm,clip]{2198f06r.ps} \end{figure}$ Figure 6: Left: six fields were selected for the SBF analysis in UGC 5442. The power spectra of the SBF fields (filled circles) are well fitted by the sum (solid line) of a scaled version of the power spectrum of the PSF and a constant (dashed lines). The wavenumbers 1-4 were not considered for the fit. Right: six fields were analysed to derive the distance of UGC 5442. A shift by 27.74 mag yields the best fit of the data to the calibration diagram.
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In the text

$\begin{figure} \par\includegraphics[height=6.9cm,width=10.9cm,clip]{2198f07l.ps}... ...*{3mm} \includegraphics[height=6.9cm,width=4.7cm,clip]{2198f07r.ps} \end{figure}$ Figure 7: Left: five fields were selected for the SBF analysis in UGC 5944. The signal-to-noise in the power spectra is not as high as measured in the other galaxies due to the larger distance of the galaxy at 11.1 Mpc. Nevertheless, the power spectra of the SBF fields (filled circles) are well fitted by the sum (solid line) of a scaled version of the power spectrum of the PSF and a constant (dashed lines). The wavenumbers 1-4 were not considered for the fit. Right: five fields were analysed to derive the distance of UGC 5944. A shift by 30.22 mag yields the best fit of the data to the calibration diagram.
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In the text

$\begin{figure} \par\includegraphics[height=6.9cm,width=10.9cm,clip]{2198f08l.ps}... ...*{3mm} \includegraphics[height=6.9cm,width=4.7cm,clip]{2198f08r.ps} \end{figure}$ Figure 8: Left: six fields were selected for the SBF analysis in NGC 4150. The signal-to-noise in the power spectra is not as high as measured in the other galaxies, as it is more distant. Nevertheless, the power spectra of the SBF fields (filled circles) are well fitted by the sum (solid line) of a scaled version of the power spectrum of the PSF and a constant (dashed lines). The wavenumbers 1-4 were not considered for the fit. Right: six fields were analysed to derive the distance of NGC 4150. A shift by 30.79 mag yields the best fit of the data to the calibration diagram.
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In the text

$\begin{figure} \par\includegraphics[height=6.9cm,width=10.9cm,clip]{2198f09l.ps}... ...*{3mm} \includegraphics[height=6.9cm,width=4.7cm,clip]{2198f09r.ps} \end{figure}$ Figure 9: Left: six fields were selected for the SBF analysis in BTS 128. The power spectra of the SBF fields (filled circles) are well fitted by the sum (solid line) of a scaled version of the power spectrum of the PSF and a constant (dashed lines). The wavenumbers 1-4 were not considered for the fit. Right: six fields were analysed to derive the distance of BTS 128. A shift by 31.02 mag yields the best fit of the data to the calibration diagram.
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In the text

$\begin{figure} \par\includegraphics[width=6.0cm,clip]{2198f10.ps} \end{figure}$ Figure 10: Residual R-band image of UGC 7639 with the eight SBF fields indicated.
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In the text

$\begin{figure} \par\includegraphics[height=6.9cm,width=7.6cm,clip]{2198f11l.ps}\... ...*{3mm} \includegraphics[height=6.9cm,width=4.7cm,clip]{2198f11r.ps} \end{figure}$ Figure 11: Left: eight fields were selected for the SBF analysis in UGC 7639. The signal-to-noise in the power spectra is high. The power spectra of the SBF fields (filled circles) are well fitted by the sum (solid line) of a scaled version of the power spectrum of the PSF and a constant (dashed lines). The wavenumbers 1-4 were not considered for the fit. Right: eight fields were analysed to derive the distance of UGC 7639. A shift by 29.27 mag yields the best fit of the data to the calibration diagram.
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In the text

$\begin{figure} \par\includegraphics[height=5.8cm,width=9.1cm,clip]{2198f12l.ps}\... ...12m.ps}\includegraphics[height=5.8cm,width=4.0cm,clip]{2198f12r.ps} \end{figure}$ Figure 12: Left: six fields were selected for the SBF analysis in UGC 8799. The signal-to-noise in the power spectra is not as high as measured in the other galaxies due to the larger distance of the galaxy at $\sim$ 13.2 Mpc. Nevertheless, the power spectra of the SBF fields (filled circles) are reasonably well fitted by the sum (solid line) of a scaled version of the power spectrum of the PSF and a constant (dashed lines). The wavenumbers 1-4 were not considered for the fit. Right: six fields were analysed to derive the distance of UGC 8799. A shift by 30.19 mag or 30.61 mag yields the best fit of the data to the calibration diagram.
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In the text

$\begin{figure} \par\includegraphics[height=6.9cm,width=7.5cm,clip]{2198f13l.ps}\... ...*{3mm} \includegraphics[height=6.9cm,width=4.7cm,clip]{2198f13r.ps} \end{figure}$ Figure 13: Left: eight fields were selected for the SBF analysis in UGC 8882. The signal-to-noise in the power spectra is not as high as measured in the other galaxies due to the larger distance of the galaxy at 14.4 Mpc. Nevertheless, the power spectra of the SBF fields (filled circles) are well fitted by the sum (solid line) of a scaled version of the power spectrum of the PSF and a constant (dashed lines). The wavenumbers 1-4 were not considered for the fit. Right: eight fields were analysed to derive the distance of UGC 8882. A shift by 29.60 mag yields the best fit of the data to the calibration diagram.
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In the text

$\begin{figure} \par\includegraphics[width=4.2cm,clip]{2198f01a.ps}\includegraphi... ...s}\includegraphics[width=4.2cm,clip]{2198f01j.ps}\hspace*{4.2cm}} \end{figure}$	Figure 1: Reduced R-band images of the ten sample galaxies with the boundaries of the analysed square SBF fields indicated. The field-of-view is $2.5 \times 2.5$ arcmin. North is up, East to the left.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{2198f02.ps} \end{figure}$	Figure 2: After subtracting the best-fitting model of the global light distribution a well developed 4-armed spiral structure and traces of dust in the central region become visible in the residual image of NGC 4150. These findings confirm the morphological type of S0/Sa for this galaxy.
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$\begin{figure} \par\includegraphics[width=6.0cm,clip]{2198f10.ps} \end{figure}$	Figure 10: Residual R-band image of UGC 7639 with the eight SBF fields indicated.
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