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XMM­Newton CCF Release Note
XMM­CCF­REL­28
EPIC PN Spectral Response Distribution
D Lumb
October 13, 2000
1 CCF components
Name of CCF VALDATE List of Blocks
changed
CAL VERSION XSCS flag
EPN REDIST 0005 2000 01 01T00:00:00 EBINS NO
2 Changes
Editorial change ­ units changed from keV to eV
3 Scientific Impact of this Update
Necessary to make the response generation for PN coherent with other data files.
4 Estimated Scientific Quality
A combination of reconciling with theoretical models, and measurement of spectral residuals in­orbit
has been undertaken, such that for some targets, spectral discrepancies at less than the 10% level
have been obtained. Progress is being made for pathological cases of soft and hard sources, and in
understanding the consequences of pile­up.
As ever, progress in improving the spectral response knowledge will continue to develop with
more widespread use of data sets of different quality and characteristics. In the mean time users
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XMM­Newton CCF Release XMM­CCF­REL­28 Page: 2
should be aware not to over­interpret spectral features near instrument absorption edges, and at
the extremes of energy range, nor at count rates inappropriate to the readout mode of use. Namely
energies џ300eV, around C K (280ev) O K (540eV), ALk (1.55keV), Si K (1.84keV) and Au M
(2.3keV) edges, and at energies –8keV.
5 Expected Updates
The mode dependencies of the EPIC cameras is uncertain yet with respect to the spectral response.
While it is hoped that the gain dependencies cover all aspects of mode changes, it is possible that
at least in timing mode, the 1­d clocking scheme causes events to be merged, and so the response
distributions may ALSO be different