All Figures

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0283fig1.ps}\end{figure}$ Figure 1: The reduced FORS1 I ( top), V ( middle), and N ( bottom, moved downward by 1% for clarity) spectra of NGC 2244-334. The Si II lines at $\lambda \lambda$ 4128-4130 are visible, and the numerous Fe II lines around 5200 Å that contribute to the absorption detected by Maitzen's $\Delta a$ photometry are prominent. A strong Zeeman signature is also seen in the three very strong lines of multiplet 42 of Fe II at 4923, 5018 and 5169 Å.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0283fig2.ps}\end{figure}$ Figure 2: The correlation diagram of V/I versus $({\rm d}I/{\rm d}\lambda )/I$ , from which the value of $\langle B_z \rangle$ is deduced. The points in this diagram are obtained only from the wings of the Balmer lines, using a window that corresponds roughly to the observed width of each line. The windows used range in (full) width from about 50 Å at H $\beta$ to 25 Å at H11 (3770 Å).
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{0283fig3.ps}\end{figure}$ Figure 3: This figure shows the unscaled I FORS1 spectrum of NGC 2244-334 (dotted), the observed V/I spectrum (error bars), and the ${\rm d}I/{\rm d}\lambda$ spectrum derived from the I spectrum by numerical differentiation and scaled by the factor appropriate for $\langle B_z \rangle$ = -9 kG (Eq. (1)).
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{0283fig4.eps}\end{figure}$ Figure 4: Representative synthesis of three 50-Å regions of the UVES spectrum of NGC 2244-334. The actual spectra are the curves with noise in the continuum; fits are smoother. Note that there is no real evidence for missing lines in the synthesis, although not all the lines are well fit. Identification of dominant contributors to the stronger features is given underneath the spectra. Although the ultraviolet spectral regions have relatively low signal-to-noise ratio, they are still rich in information.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0283fig2.ps}\end{figure}$	Figure 2: The correlation diagram of V/I versus $({\rm d}I/{\rm d}\lambda )/I$ , from which the value of $\langle B_z \rangle$ is deduced. The points in this diagram are obtained only from the wings of the Balmer lines, using a window that corresponds roughly to the observed width of each line. The windows used range in (full) width from about 50 Å at H $\beta$ to 25 Å at H11 (3770 Å).
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$\begin{figure} \par\includegraphics[width=13.6cm,clip]{0283fig3.ps}\end{figure}$	Figure 3: This figure shows the unscaled I FORS1 spectrum of NGC 2244-334 (dotted), the observed V/I spectrum (error bars), and the ${\rm d}I/{\rm d}\lambda$ spectrum derived from the I spectrum by numerical differentiation and scaled by the factor appropriate for $\langle B_z \rangle$ = -9 kG (Eq. (1)).
Open with DEXTER