All Figures

$\begin{figure} \par\epsfxsize=13.6cm \epsfbox{1993fig1.eps}\end{figure}$ Figure 1: Normalized spectra of our sample of central stars of planetary nebulae (from above displaced vertically: NGC 1360, EGB 5, LSS 1362, Abell 36).
Open with DEXTER

In the text

$\begin{figure} {\psfig{figure=1993fig2.eps,width=16.4cm} } \end{figure}$ Figure 2: Circular polarization (V/I) in the four observation blocks of of the central star of NGC 1360 in the vicinity of the strong spectral lines H $\delta +$ He II, H $\gamma +$ He II, He II 4686, H $\beta +$ He II compared to the prediction by the low-field approximation (Eq. (2)) using a longitudinal magnetic field of -1343 G, 1708 G, 2832 G, and 194 G, respectively.
Open with DEXTER

In the text

$\begin{figure} {\psfig{figure=1993fig3.eps,width=16.4cm} } \end{figure}$ Figure 3: Circular polarization (V/I) observed in the central stars of LSS 1362, Abell 36, and EGB 5 in the vicinity of the strong spectral lines H $\delta +$ He II, H $\gamma +$ He II, He II 4686, H $\beta +$ He II compared to the prediction by the low-field approximation (Eq. (2)) using a longitudinal magnetic field of 1891 G, 1169 G, and 1992 G. In the lower level we show an example for a fit to one of the artificial spectra with a noise level of 0.0005 and an assumed magnetic field of 1500 G. The fit results in B=1763 G.
Open with DEXTER

In the text

$\begin{figure} \par\epsfxsize=8.3cm \epsfbox{1993fig4.eps}\end{figure}$ Figure 4: Result of the fits with simulated data having the same noise level as the observations of NGC 1360 for input magnetic fields between 0 and 3000 G, in steps of 500 G. From center line to outside: mean fit result, 1 $\sigma$ error range, 99% confidence level, and smallest and largest fit result during the 1000 simulations which were performed for each predescribed magnetic field.
Open with DEXTER

In the text

$\begin{figure} \par\epsfxsize=13.6cm \epsfbox{1993fig1.eps}\end{figure}$	Figure 1: Normalized spectra of our sample of central stars of planetary nebulae (from above displaced vertically: NGC 1360, EGB 5, LSS 1362, Abell 36).
Open with DEXTER

$\begin{figure} {\psfig{figure=1993fig2.eps,width=16.4cm} } \end{figure}$	Figure 2: Circular polarization (V/I) in the four observation blocks of of the central star of NGC 1360 in the vicinity of the strong spectral lines H $\delta +$ He II, H $\gamma +$ He II, He II 4686, H $\beta +$ He II compared to the prediction by the low-field approximation (Eq. (2)) using a longitudinal magnetic field of -1343 G, 1708 G, 2832 G, and 194 G, respectively.
Open with DEXTER

$\begin{figure} \par\epsfxsize=8.3cm \epsfbox{1993fig4.eps}\end{figure}$	Figure 4: Result of the fits with simulated data having the same noise level as the observations of NGC 1360 for input magnetic fields between 0 and 3000 G, in steps of 500 G. From center line to outside: mean fit result, 1 $\sigma$ error range, 99% confidence level, and smallest and largest fit result during the 1000 simulations which were performed for each predescribed magnetic field.
Open with DEXTER