Dealing with EPIC Out-of-Time (OoT) events

Procedure

The OoT events correction is a "two-step" process:

1. generation of an OoT event list (together with a standard observation event list)
2. removal of OoT events from an image or spectrum

These two steps are described below. In the following example, it will be assumed that a user intends to remove OoT events from a pn exposure, taken in Full Frame Mode.

Generation of an OoT event list

1. Run epchain to generate an OoT event list (PiiiiiijjkkPNblllOOEVLInmmm.FIT)
   
      epchain runbackground=N keepintermediate=raw withoutoftime=Y
    
2. Run epchain to generate an observation event list (PiiiiiijjkkPNblllPIEVLInmmm.FIT)
   
      epchain runatthkgen=N runepframes=N runbadpixfind=N runbadpix=N
    

In order to save some time, one does not have to re-create the attitude history file, or re-run epframes, badpixfind and badpix. epchain will create an output event file with the name PiiiiiijjkkPNblllPIEVLInmmm.FIT (the standard epchain name for a calibrated EPIC-pn Imaging event list).

Removal of OoT events from an image

1. Generate an image from the OoT event list,
   
      evselect table=PiiiiiijjkkPNblllOOEVLInmmm.FIT imagebinning=binSize \
        imageset=PN_OoT_image.fits withimageset=yes xcolumn=X ycolumn=Y \
        ximagebinsize=80 yimagebinsize=80
    
2. Generate an image from the observation event list,
   
      evselect table=PiiiiiijjkkPNblllPIEVLInmmm.FIT imagebinning=binSize \
        imageset=PN_observation_image.fits withimageset=yes xcolumn=X ycolumn=Y \
        ximagebinsize=80 yimagebinsize=80
    
3. Rescale the OoT image to the expected fraction of OoT events (6.3% for pn in Full Frame Mode; the user is referred to the EPIC chapter, section EPIC out-of-time events of the XMM-Newton Users Handbook for more details). The FTOOLS farith can be used for this purpose,
   
      farith PN_OoT_image.fits 0.063 PN_OoT_image_rescaled.fits MUL
   
   where, MUL indicates multiply.
    
4. Subtract the rescaled OoT image from the observation image,
   
      farith PN_observation_image.fits PN_OoT_image_rescaled.fits \
        PN_observation_clean_image.fits SUB
   
   where, SUB indicates subtract.
    

The image PN_observation_clean_image.fits is cleared from OoT events. Figure 1 illustrates the effect of OoT events on images and the results of cleaning an image with the method just described.

Figure 1; Effect of OoT events on images: The upper left panel contains a 2-10 keV band image of a pn observation of a bright source in full frame mode with the OoT-events visible as a strip running from the source towards the top of the image (in detector coordinates). The upper right panel depicts the modelled (see SAS task epframes) OoT event distribution. In the lower left panel these modelled events have been subtracted from the original image. The lower right panel is cleaned for the soft 0.2-2 keV band for comparison.

Removing OoT events from a spectrum

1. Extract a source spectrum (PN_source_spectrum.fits) from the observation image,
   
      evselect table=PiiiiiijjkkPNblllPIEVLInmmm.FIT withspectrumset=yes \
        spectrumset=PN_source_spectrum.fits energycolumn=PI spectralbinsize=5 \
        withspecranges=yes specchannelmin=0 specchannelmax=20479 \
        expression='(FLAG==0) && (PATTERN<=4) && ((X,Y) IN circle(Xc,Yc,R))'
   
   where ((X,Y) IN circle(Xc,Yc,R)) should contain the centroid position and radius in sky coordinates (X/Y).
    
2. Extract a spectrum from the OoT events,
   
      evselect table=PiiiiiijjkkPNblllOOEVLInmmm.FIT withspectrumset=yes \
        spectrumset=PN_oot_spectrum.fits energycolumn=PI spectralbinsize=5 \
        withspecranges=yes specchannelmin=0 specchannelmax=20479 \
        expression='(FLAG==0) && (PATTERN<=4) && ((X,Y) IN circle(Xc,Yc,R))'
   
   where ((X,Y) IN circle(Xc,Yc,R)) should contain the centroid position and radius in sky coordinates (X/Y).
    
3. Change the name of the COUNTS column in the OoT event spectrum to CTS_OOT,
   
      fparkey value=CTS_OOT fitsfile=PN_oot_spectrum.fits+1 keyword=TTYPE2
    
4. Copy the CTS_OOT column of the OoT event spectrum into the source spectrum,
   
      faddcol infile=PN_source_spectrum.fits+1 colfile=PN_oot_spectrum.fits+1 \
        colname=CTS_OOT
    
5. Multiply the values in the column CTS_OOT by 0.063 (6.3% for pn in Full Frame Mode; the user is referred to the EPIC chapter, section EPIC out-of-time events of the XMM-Newton Users Handbook for more details). As the PN_source_spectrum.fits file will be modified in the next two steps, the user may wish to create a backup first,
   
      fcalc clobber=yes infile=PN_source_spectrum.fits+1 outfile=PN_source_spectrum.fits \
        clname=CTS_OOT expr=CTS_OOT*0.063
    
6. Subtract the rescaled values of the CTS_OOT from the COUNTS column of the source spectrum,
   
      fcalc clobber=yes infile=PN_source_spectrum.fits+1 outfile=PN_source_spectrum.fits \
        clname=COUNTS expr=COUNTS-CTS_OOT

          Figure 2 illustrates the effect of OoT events on spectra.

Figure 2; Effect of spectral broadening due to OoT events: the upper panel shows a spectrum extracted from a pn CalClosed full frame mode observation (black) together with the spectrum corrected for OoT events (green). In the lower panel the spectrum of the simulated OoT events over the whole FoV is plotted.