Perhaps the principal practical use is for assessment of the background that often accounts for the majority of detected events over the whole instrument and which must therefore be explicitly quantified. The background is made up of several contributions and is usually weak enough to cause few problems: RGS spectra are photon limited more than 80% of the time. However, solar flares and other particle events can cause significant or in rare cases even overwhelming contamination. Rapid variability is also common so that only part of an observation may be affected so that it is possible to generate supplementary GTIs in order to exclude periods of unacceptably high background. Fig. 38 shows the background light curve generated using:
(CCDNR = 9) && ((MLAMBDA,XDSP_CORR) IN \ REGION(P0136540101R2S002SRCLI_0000.FIT:RGS2_BACKGROUND))
What constitutes unacceptably high background is often a matter of
personal judgment depending on the type of analysis
undertaken. High-contrast features like strong emission lines can
often tolerate higher background levels than smooth continuum spectra
and the overall source brightness is clearly a consideration. It is
best to experiment. As a rule of thumb, data with CCD9 background
rates above 1 count/s might be considered suspect and be excluded by
GTI mechanism to flag periods of low background.
tabgtigen table=RGS2.background.FITS gtiset=RGS2.background.GTI.FITS \ expression='(RATE<1)'