Astronomy & Astrophysics

All Figures

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{aa3400.f1}}\end{figure}$ Figure 1: The surface brightness distributions in B and V bands obtained from combined data by Neizvestny (1986) and Doroshenko (this work).
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{aa3400.f2}}\end{figure}$ Figure 2: UBV-light curves of Mrk 6 in A=27.5''obtained from observations by Doroshenko (filled circles) and Neizvestny (1987) (open circles).
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In the text

$\begin{figure} \par\resizebox{8.1cm}{!}{\includegraphics[clip]{aa3400.f3}}\end{figure}$ Figure 3: Light curve constructed from photometric data in V-band by Doroshenko - filled circles, by Neizvestny (1987) - open circles and from spectral continuum flux at $\lambda~$ 5170 Å by Doroshenko & Sergeev (2003) - crosses.
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In the text

$\begin{figure} \par\resizebox{8.75cm}{!}{\includegraphics[clip]{aa3400.f4}}\end{figure}$ Figure 4: Two-color diagram of Mrk 6 a) for observed values and b) after subtraction the underlying galaxy contribution. The colors averaged over the intervals $\Delta V=0.1^{\rm m}$ are indicated by the large open circles. The solid line corresponds to the CI for power law spectra ( $I_{\nu }\propto \nu ^{\alpha }$ ) with different $\alpha$ s; the dashed line shows the CI for black bodies with different temperature Tbb.
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In the text

$\begin{figure} \par\resizebox{7.7cm}{!}{\includegraphics[clip]{aa3400.f5}}\end{figure}$ Figure 5: The structure function of Mrk 6: upper panel - in U, middle panel - in B and bottom panel - in V band. The best fit Poisson model is shown by heavy lines. Thin lines mark the uncertainty of the SF ( $\sigma _{SF}(\tau )$ ) obtained from Monte-Carlo simulations for the best fit parameters.
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In the text

$\begin{figure} \par\resizebox{8.2cm}{!}{\includegraphics[clip]{aa3400.f6}}\end{figure}$ Figure 6: Comparison of the SRs for Mrk 6, NGC 4151 and NGC 5548. The observed SFs are shown by open circles. The best fit Poisson models are shown by heavy lines. Dashed-lines indicate uncertainty of the model SFs calculated from Monte-Carlo light curve simulations. The best fit parameters of the models are given in Table 3.
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{aa3400.f1}}\end{figure}$	Figure 1: The surface brightness distributions in B and V bands obtained from combined data by Neizvestny (1986) and Doroshenko (this work).
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$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{aa3400.f2}}\end{figure}$	Figure 2: UBV-light curves of Mrk 6 in A=27.5''obtained from observations by Doroshenko (filled circles) and Neizvestny (1987) (open circles).
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$\begin{figure} \par\resizebox{8.1cm}{!}{\includegraphics[clip]{aa3400.f3}}\end{figure}$	Figure 3: Light curve constructed from photometric data in V-band by Doroshenko - filled circles, by Neizvestny (1987) - open circles and from spectral continuum flux at $\lambda~$ 5170 Å by Doroshenko & Sergeev (2003) - crosses.
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$\begin{figure} \par\resizebox{7.7cm}{!}{\includegraphics[clip]{aa3400.f5}}\end{figure}$	Figure 5: The structure function of Mrk 6: upper panel - in U, middle panel - in B and bottom panel - in V band. The best fit Poisson model is shown by heavy lines. Thin lines mark the uncertainty of the SF ( $\sigma _{SF}(\tau )$ ) obtained from Monte-Carlo simulations for the best fit parameters.
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$\begin{figure} \par\resizebox{8.2cm}{!}{\includegraphics[clip]{aa3400.f6}}\end{figure}$	Figure 6: Comparison of the SRs for Mrk 6, NGC 4151 and NGC 5548. The observed SFs are shown by open circles. The best fit Poisson models are shown by heavy lines. Dashed-lines indicate uncertainty of the model SFs calculated from Monte-Carlo light curve simulations. The best fit parameters of the models are given in Table 3.
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