Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0729f01.eps}\end{figure}$ Figure 1: The difference lightcurve $\Delta m$ between quasar images A and B measured in different wavelength bands. For clarity we shift the curves along the vertical direction. The binned OGLE observations with 181 data points measured in the V-band (Udalski et al. 2006). From our 39-epoch spectrophotometric monitoring, we compute the difference lightcurves of the continuum integrated in the six bands defined in Table 2.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0729f02.eps}\end{figure}$ Figure 2: Examples of six simulated lightcurves fitting the observed OGLE difference lightcurve $\Delta m$ between quasar images A and B.
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In the text

$\begin{figure} \par\includegraphics[width=5.4cm,clip]{0729f03.eps}\hspace*{3mm} ... ...04.eps}\hspace*{3mm} \includegraphics[width=5.4cm,clip]{0729f05.eps}\end{figure}$ Figure 3: Left: the probability distributions for the FWHM $\hat{R}_{\rm s}$ of the source, based on the OGLE data. We consider two cases, one with and another without the prior on the velocity. Center: same as left panel, but for the effective transverse velocity $\hat{V}$ . Right: the probability distributions for the ratio $\hat{R}_{\rm s}/\hat{V}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0729f06.eps}\hspace*{0.6cm... ....eps}\hspace*{0.6cm} \includegraphics[width=7.6cm,clip]{0729f09.eps}\end{figure}$ Figure 4: Top: the source FWHM ratio $R_{i}/R_{\rm ref}=\hat{R}_{i}/\hat{R}_{\rm ref}$ as a function of the wavelength ratio $\lambda _i/\lambda _{\rm ref}$ obtained from the trajectories in the library having $\hat{R}_{\rm s}=0.1~r_{\rm E}=10$ pixels ( left) and $\hat{R}_{\rm s}=1~r_{\rm E}=100$ pixels ( right). The reference wavelength is $\lambda _{\rm ref}=2125$ Å measured in the source frame. The error bars give the $1\sigma$ uncertainties. The solid line indicates the linear regression across the points. The dashed line shows the relation expected for the standard $R\propto \lambda ^{4/3}$ scaling. Bottom: the corresponding probability distributions of the scaled source sizes $\hat{R}_i$ obtained in the six bands i=1,2,..., 6, and using the same color code as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0729f10.eps}\hspace*{0.5cm} \includegraphics[width=7.6cm,clip]{0729f11.eps}\end{figure}$ Figure 5: Left: the final energy profile obtained from the whole ensemble of source trajectories, including the prior on the velocity. The reference wavelength is $\lambda _{\rm ref}=2125$ Å measured in the source frame. The error bars give the $1\sigma$ uncertainties. The solid line indicates the linear regression across the points. The dashed line shows the relation expected for the standard $R\propto \lambda ^{4/3}$ scaling. Right: the corresponding probability distributions of the R_i values obtained in the six bands i=1,2,..., 6, and using the same color code as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0729f12.eps}\end{figure}$ Figure 6: The power-law index $\zeta$ of the energy profile $R\propto \lambda ^{\zeta }$ as a function of the scaled FWHM $\hat{R}_{\rm s}$ of the source. The points are obtained from the subsamples of trajectories with given $\hat{R}_{\rm s}$ fitting the OGLE data and including the prior on the velocity. The horizontal solid red lines indicate the index $\zeta$ and its $1\sigma$ deviation obtained by considering the whole library of trajectories and including the velocity prior. The dashed lines show the expected indices for the three indicated accretion-disk models.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0729f02.eps}\end{figure}$	Figure 2: Examples of six simulated lightcurves fitting the observed OGLE difference lightcurve $\Delta m$ between quasar images A and B.
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$\begin{figure} \par\includegraphics[width=5.4cm,clip]{0729f03.eps}\hspace{3mm} ... ...04.eps}\hspace{3mm} \includegraphics[width=5.4cm,clip]{0729f05.eps}\end{figure}$	Figure 3: Left: the probability distributions for the FWHM $\hat{R}_{\rm s}$ of the source, based on the OGLE data. We consider two cases, one with and another without the prior on the velocity. Center: same as left panel, but for the effective transverse velocity $\hat{V}$ . Right: the probability distributions for the ratio $\hat{R}_{\rm s}/\hat{V}$ .
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