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XMMNewton CCF Release Note
XMMCCFREL11
RGS CCD Properties
C. Erd
October 4, 2000
1 CCF components
Name of CCF VALDATE List of Blocks
changed
CAL VERSION XSCS flag
RGS1 ADUCONV 0004 20000206T16:50:00 ADUCOEFF,
OFFSET GAIN
--- NO
RGS2 ADUCONV 0005 20000125T16:27:00 ADUCOEFF,
OFFSET GAIN
--- NO
RGS1 CTI 0001 19980101T00:00:00 CTI,
CTI EXTENDED,
XCTI, CTIY1,
CTIY2,
CTIY3, CTIY4,
CTIY5, CTIY6,
CTIY7,CTIY8,
CTIY9
--- NO
RGS2 CTI 0001 19980101T00:00:00 CTI,
CTI EXTENDED,
XCTI, CTIY1,
CTIY2,
CTIY3, CTIY4,
CTIY5, CTIY6,
CTIY7,CTIY8,
CTIY9
--- NO
RGS1 REDIST 0003 19990101T00:00:00 EBOUNDS,
CCD REDISTRIBUTION
--- NO
RGS2 REDIST 0003 19990101T00:00:00 EBOUNDS,
CCD REDISTRIBUTION
--- NO
RGS1 BADPIX 0004 20000206T16:50:00 BADPIX --- NO
RGS2 BADPIX 0004 20000125T19:30:00 BADPIX --- NO
RGS1 DARKFRAME 0003 19980101T00:00:00 DARKFRAME --- NO
RGS2 DARKFRAME 0003 19980101T00:00:00 DARKFRAME --- NO
1

XMMNewton CCF Release XMMCCFREL11 Page: 2
2 Changes
Before application of the gain correction the zero level is subtracted from the CCD PHA data.
The dark frame that was measured during preflight calibrations exhibits some higher values closer
to the edges of the CCD's, and additionally higher offsets as a function of distance (time) to the
readout node. These were averaged for all CCD's measured and stored as the nominal dark frame
in RGS DARKFRAME. This dark frame is linearly shifted based on the individual offset values per CCD
(see [1] for details).
The gains for the CCD's were calibrated from inflight data by using the continuum as well as
discrete emission lines with known energies (see [2]). The gain corrections are adjusted such that
the corrected pulse invariant (PI) values match the CCD redistribution function.
The CTI was compared with the parameterizations that were obtained with higher statistics
during preflight calibrations and no significant deviation from preflight conditions were found.
Therefore the preflight CTI calibration data remain applicable.
The CCD redistribution function is described with a phenomenological model [1, 3], whose
parameters are stored in RGS REDIST. The response model operates in pulse invariant (PI) units,
and therefore the CCD have to be gain corrected before. Currently these parameters of the response
model are identical for all CCD's.
The bad pixel tables were updated based on early flight data.
3 Scientific Impact of this Update
First release.
4 Estimated Scientific Quality
It should be noted that the CCD's exhibit poorer CTI along the parallel direction close to their
edges. Insufficient correction of the CTI may produce smaller or higher PI, depending on the kind of
correction, and subsequently more events may be rejected close to these areas by the order selection.
Based on current knowledge, this should not exceed a few percent.
The CCD redistribution model was tested with isolated lines of coronal emission spectra and has
generally proven to correctly describe the CCD data well. Uncertainties become apparent in errors
in the effective area, and are estimated to be less than 1%.

XMMNewton CCF Release XMMCCFREL11 Page: 3
References
[1] Christian Erd, Phillipe Gondoin, David Lumb, Rudi Much, Uwe Lammers, and Giuseppe Va
canti. Calibration Access and Data Handbook. XMMPSGM20, issue 1.0, ESA/SSD, September
2000.
[2] C. de Vries. Inflight CCD PHA model gains. RGSSRONCALME00/cv2, Space Research Or
ganization of the Netherlands, June 2000. http://ws13.sron.nl:8080/xmmdoc/effective area/rgs
sroncalme00 cv2.ps.
[3] C. de Vries. A simple CCD pulse height model function. RGSSRONCAL
ME98/010, Space Research Organization of the Netherlands, November 1998.
http://ws13.sron.nl:8080/xmmdoc/effective area/rgssroncalme98 010.ps.