Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[angle=270,width=17cm,clip]{etasax2_3band.ps}\end{figure}$ Figure 1: The BeppoSAX MECS images of the $\eta$ Car region on 2000 June 21-23, in three energy bands: (from left to right) 2-5.5 keV (softer), 6-7.5 keV (iron line), and 7.5-10 keV (harder). North is up and east to the left; the size of the image field is 54 arcmin. The second brightest source to the west of $\eta$ Car is the W-R star HD 93162 (WR25).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.15cm,clip]{etasax2_fig2.ps}\end{figure}$ Figure 2: The BeppoSAX MECS background-subtracted count rates (in s^-1 keV^-1) of $\eta$ Car in June 2000 compared with the local nebular background spectrum.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.15cm,clip]{etasax2_fig3.ps}\end{figure}$ Figure 3: Upper panel: results of the fit of the June 2000 BeppoSAX MECS background-subtracted spectrum with a one-temperature (5.51 keV) MEKAL model. The spectral model is extrapolated to the PDS energy range to show the high energy flux excess. The residuals are plotted in the lower panel.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.15cm,clip]{etasax2_fig4.ps}\end{figure}$ Figure 4: Upper panel: results of the fit of the BeppoSAX MECS and PDS (2-150 keV) spectrum of $\eta$ Car in June 2000 with a two-temperature (5.5 keV and 14 keV) MEKAL model. The residuals are plotted in the lower panel.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{etasax2_fig5.ps}\end{figure}$ Figure 5: The BeppoSAX MECS and PDS (2-150 keV) spectrum of $\eta$ Car fitted with a 5.70 keV thermal bremsstrahlung plus a power law spectrum with photon index 2.42, and a Gaussian line centred at 6.70 keV.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{etasax2_fig6.ps}\end{figure}$ Figure 6: Plot of the BeppoSAX MECS23 spectra of $\eta$ Car during December 1996-June 2000. The phases of the 5.53 yr cycle are indicated. Note the larger flux of the iron line in March 1998 ( $\Phi = 1.05$ ) when the spectrum was strongly absorbed. At energies >7 keV the four spectra overlap.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=17cm,clip]{etasax2_3band.ps}\end{figure}$	Figure 1: The BeppoSAX MECS images of the $\eta$ Car region on 2000 June 21-23, in three energy bands: (from left to right) 2-5.5 keV (softer), 6-7.5 keV (iron line), and 7.5-10 keV (harder). North is up and east to the left; the size of the image field is 54 arcmin. The second brightest source to the west of $\eta$ Car is the W-R star HD 93162 (WR25).
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$\begin{figure} \par\includegraphics[angle=270,width=8.15cm,clip]{etasax2_fig2.ps}\end{figure}$	Figure 2: The BeppoSAX MECS background-subtracted count rates (in s^-1 keV^-1) of $\eta$ Car in June 2000 compared with the local nebular background spectrum.
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$\begin{figure} \par\includegraphics[angle=270,width=8.15cm,clip]{etasax2_fig3.ps}\end{figure}$	Figure 3: Upper panel: results of the fit of the June 2000 BeppoSAX MECS background-subtracted spectrum with a one-temperature (5.51 keV) MEKAL model. The spectral model is extrapolated to the PDS energy range to show the high energy flux excess. The residuals are plotted in the lower panel.
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$\begin{figure} \par\includegraphics[angle=270,width=8.15cm,clip]{etasax2_fig4.ps}\end{figure}$	Figure 4: Upper panel: results of the fit of the BeppoSAX MECS and PDS (2-150 keV) spectrum of $\eta$ Car in June 2000 with a two-temperature (5.5 keV and 14 keV) MEKAL model. The residuals are plotted in the lower panel.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{etasax2_fig5.ps}\end{figure}$	Figure 5: The BeppoSAX MECS and PDS (2-150 keV) spectrum of $\eta$ Car fitted with a 5.70 keV thermal bremsstrahlung plus a power law spectrum with photon index 2.42, and a Gaussian line centred at 6.70 keV.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{etasax2_fig6.ps}\end{figure}$	Figure 6: Plot of the BeppoSAX MECS23 spectra of $\eta$ Car during December 1996-June 2000. The phases of the 5.53 yr cycle are indicated. Note the larger flux of the iron line in March 1998 ( $\Phi = 1.05$ ) when the spectrum was strongly absorbed. At energies >7 keV the four spectra overlap.
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