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XMM­Newton CCF Release Note
XMM­CCF­REL­249
Support to FF mode special gain correction
F. Haberl, M. Guainazzi, M. Freyberg
May 7, 2009
1 CCF components
Name of CCF VALDATE List of Blocks
changed
Change in CAL HB
EPN CTI 0021 2000­01­01T00:00:00 CTI­
HIGH ADD PAR
YES
2 Changes
A new column (FF PAR) has been added to the CTI­HIGH ADD PAR extension of the EPIC­pn CTI
CCF. This column contains the 16 parameters of a special gain correction function to be applied
to pn exposures in Full Frame Mode. The function is analogous to that used to parameterize the
special gain correction function in Small Window and Large Window modes. The CTI losses in
the EPIC­pn window modes originate during two phases, the first in the fast­shift from the image
to the frame­store area, and the second in the (normal) slow­shift during read­out to the CAMEX
(XMM­SOC­CAL­TN­0081, Sect.4).
The fast­shift CTI losses are modeled as energy­dependent fraction of the slow­shift CTI losses.
This correction function is
f(E) = #â # a 0 - a 11 â exp # - # E - a 12
a 13
# 2 ## â # b 0 - b 11 â exp # - # E - b 12
b 13
# 2 ## â
# c 0 - c 11 â exp # - # E - c 12
c 13
# 2 ## â # d 0 - d 11 â exp # - # E - d 12
d 13
# 2 ## (1)
where the coe#cients a, b, c, and d are stored in the CCF, and # is a mode­dependent factor. This
structure had been implemented in July 2002.
1

XMM­Newton CCF Release XMM­CCF­REL­249 Page: 2
Special gain correction functions for modes others than Full Frame are defined relatively to the
Full Frame mode. The new extension is required to allow for changes in the Full Frame gain, without
simultaneously changing the special gain correction functions for the other modes.
3 Scientific impact of this update
In EPN CTI 0021 the parameters in the FF PAR extension are set to dummy values, which yield no
correction.
4 Estimated scientific quality
See Section above.
5 Test procedure and results
SASv9.0 and earlier versions do not support this correction. The new extension is transparent to the
users. This has been proven on a pn Full Frame exposure of MS 0737.9+7441 (Obs.#0123100201) 1 .
Spectra extracted from event lists reduced with SASv8.0 using CCF#20 and #21 yield indistin­
guishable results, as expected.
6 Expected Updates
The new extension will be filled with calibrated numbers once the calibration is completed.
1 This source was chosen, because it is one of the brightest pile­up free sources (0.35--10 keV count rate: 4.719 ±
0.017 s -1 ) in 2XMM. It could be therefore chosen as a testbed when the real correction is implemented.