... camera[*]
Based on observations with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA).
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... layer[*]
As you will see later, most of the K$_{\alpha }$ and K$_{\beta }$ lines of the mentioned atoms appear as fluorescence lines in the calibration spectra in Fig. 6.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... operational[*]
Observation is of course not possible, instrument data are not processed, but the detectors are still running. Extended instrument recovery times are avoided.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... monitor[*]
The low energy proton flare was still ongoing after the drop in count rate after 2.7 104 s, but the camera was automatically switched off and the filter wheel closed because of the high number of counts.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
© ESO 2001