Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[angle=270,width=17.8cm,clip]{8750fig1.eps} \end{figure}$ Figure 1: The differential photometry obtained at each observatory (DE - open circles, OSN - squares, APT - filled circles) normalized to zero. The solid line is a least squares fit of two frequencies, which were revealed from subsequently prewhitened amplitude Fourier spectra of the combined data.
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In the text

$\begin{figure} \resizebox{8.8cm}{!} {\rotatebox{270}{\includegraphics{8750fig2.eps} }} \end{figure}$ Figure 2: Strömgren y-filter Fourier spectra: a) 15 And relative to HD 220575; b) 15 And relative to 10 Lac; c) HD 220575 relative to 10 Lac.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{8750fig3.eps}} \end{figure}$ Figure 3: Fourier amplitude spectrum of the combined data in the V and y filters. Some prewhitening steps are indicated.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=17.8cm,clip]{8750fig1.eps} \end{figure}$	Figure 1: The differential photometry obtained at each observatory (DE - open circles, OSN - squares, APT - filled circles) normalized to zero. The solid line is a least squares fit of two frequencies, which were revealed from subsequently prewhitened amplitude Fourier spectra of the combined data.
Open with DEXTER

$\begin{figure} \resizebox{8.8cm}{!} {\rotatebox{270}{\includegraphics{8750fig2.eps} }} \end{figure}$	Figure 2: Strömgren y-filter Fourier spectra: a) 15 And relative to HD 220575; b) 15 And relative to 10 Lac; c) HD 220575 relative to 10 Lac.
Open with DEXTER

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{8750fig3.eps}} \end{figure}$	Figure 3: Fourier amplitude spectrum of the combined data in the V and y filters. Some prewhitening steps are indicated.
Open with DEXTER