$\begin{figure} \par\includegraphics[width=8.2cm,clip]{Fe052_f1.eps} \end{figure}$ Figure 1: Positions of 1998 SF36 on the sky during photometric observations. Coordinates are given in geocentric ecliptic longitude and latitude.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fe052_f2.eps} \end{figure}$ Figure 2: Sample composite lightcurves of 1998 SF36, taken on (top to bottom): 21-27 Feb., 13-16 Mar., 22-25 Aug. 2001.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fe052_f3.eps} \end{figure}$ Figure 3: Solar phase angle behaviour of 1998 SF36. Diamonds are the phase curve magnitudes in R, and asterisks are those in V, both corrected to reference geometry. The line shows the exponential-linear fit (Kaasalainen et al. 2001).
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In the text

$\begin{figure} \par\includegraphics[width=4.1cm,clip]{Fe052_f5a.eps}\hspace*{4mm... ...}\hspace*{4mm} \includegraphics[width=4.1cm,clip]{Fe052_f5i.eps} \end{figure}$ Figure 5: Selected lightcurves (asterisks) and the corresponding fits (dashed lines) for 1998 SF36. The horizontal axes give the rotational phase in degrees, and the vertical axes brightness in units of relative intensity. The viewing latitude (measured from the pole) is given by $\theta$ , and the illumination latitude by $\theta _0$ . The solar phase angle is given by $\alpha$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{Fe052_f1.eps} \end{figure}$	Figure 1: Positions of 1998 SF36 on the sky during photometric observations. Coordinates are given in geocentric ecliptic longitude and latitude.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fe052_f2.eps} \end{figure}$	Figure 2: Sample composite lightcurves of 1998 SF36, taken on (top to bottom): 21-27 Feb., 13-16 Mar., 22-25 Aug. 2001.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fe052_f3.eps} \end{figure}$	Figure 3: Solar phase angle behaviour of 1998 SF36. Diamonds are the phase curve magnitudes in R, and asterisks are those in V, both corrected to reference geometry. The line shows the exponential-linear fit (Kaasalainen et al. 2001).
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$\begin{figure} \par\mbox{\includegraphics[width=5.6cm,clip]{Fe052_f4a.eps} \incl... ...052_f4b.eps} \includegraphics[width=5.6cm,clip]{Fe052_f4c.eps} } \end{figure}$	Figure 4: Model views of 1998 SF36 (pole-on and equatorial edge-on/end-on).
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$\begin{figure} \par\includegraphics[width=4.1cm,clip]{Fe052_f5a.eps}\hspace{4mm... ...}\hspace{4mm} \includegraphics[width=4.1cm,clip]{Fe052_f5i.eps} \end{figure}$	Figure 5: Selected lightcurves (asterisks) and the corresponding fits (dashed lines) for 1998 SF36. The horizontal axes give the rotational phase in degrees, and the vertical axes brightness in units of relative intensity. The viewing latitude (measured from the pole) is given by $\theta$ , and the illumination latitude by $\theta _0$ . The solar phase angle is given by $\alpha$ .
Open with DEXTER