XMM-Newton EPIC Response Files Update Page

Updates of the EPIC Canned Response Files

Update 2023-08-16

After the release of EPIC response files for SAS v21.0 (Update 2023-05-10), a new epoch has been added to pn canned response matrices, making a total of four epochs. Also, four new epochs have been added to MOS, hence, canned response matrices are available now for 19 different epochs and, as before, two energy resolutions, 5eV and 15eV.

Update 2023-05-10

EPIC response files have been made available for the new SAS v21.0, released on the 19th April 2023. As in the previous release (Update 2021-12-09), pn canned response matrices are available for 3 different epochs. A new epoch has been added to MOS, hence, canned response matrices have been created for 15 different epochs and two energy resolutions, 5eV and 15eV.

Update 2021-12-09

EPIC response files have been made available for the new SAS v20.0, released on the 9th December 2021. As in the previous release (Update 2020-10-28), pn canned response matrices are available for 3 different epochs. MOS canned response matrices have been created for 14 different epochs and two energy resolutions, 5eV and 15eV.

Update 2020-10-28

EPIC response files have been made available for the new SAS v19.0, released on the 28^th Oct 2020. As in the previous release (Update 2019-07-31), pn canned response matrices are available for 3 different epochs. MOS canned response matrices have been created for 14 different epochs and two energy resolutions, 5eV and 15eV.

Update 2019-07-31

EPIC response files have been made available for the new SAS v18.0, released on the 10^th June 2019. As in the previous release (Update 2018-08-08), pn canned response matrices are available for 3 different epochs. MOS canned response matrices have been created for 14 different epochs and two energy resolutions, 5eV and 15eV.

Update 2018-08-08

EPIC response files have been made available for the new SAS v17.0, released on the 22^nd June 2018. As in the previous release (Update 2017-03-22), pn canned response matrices are available for 3 different epochs. MOS canned response matrices have been created for 14 different epochs and two energy resolutions, 5eV and 15eV.

Update 2017-03-22

EPIC response files have been made available for the new SAS v16.0, released on the 12^th January 2017. As in the previous release (Update 2016-04-26), pn canned response matrices are available for 3 different epochs. MOS canned response matrices have been created for 14 different epochs and two energy resolutions, 5eVand 15eV.

Update 2016-04-26

EPIC response files have been made available for the new SAS v15.0, released on the 4th February 2016. As in the previous release (Update 2014-11-24), pn canned response matrices are available for 3 different epochs. MOS canned response matrices have been created for 14 different epochs and two energy resolutions, 5eV and 15eV.

Update 2014-11-24

EPIC response files have been made available for the new SAS v14.0, released on the 13th November 2014. SAS v14.0 supports the use of PN response matrices generated at different epochs. Hence, three sets of canned response files are provided. The three epochs compensate for the gradual widening of the EPIC-pn redistribution function over the course of the mission as seen in both calibration and science data (CAL-SRN-0308-1-1.ps.gz). As in the previous release (Update 2014-01-31), MOS canned response matrices have been created for 14 different epochs and two energy resolutions, 5eV and 15eV.

Update 2014-01-31

EPIC response files have been made available for the new SAS v13.5.0, released on the 11th December 2013. SAS v13.5.0 fully supports the use of MOS response matrices generated at 5eV energy resolution. Hence, two sets of canned response files are provided, one set for 5eV and one for 15eV energy resolution. As in the previous release (Update 2013-08-06), canned response matrices have been created for 14 different epochs for EPIC-MOS and both energy resolutions.

Update 2013-08-06

EPIC response files have been made available for the new SAS v13.0.0, released on the 9th May 2013. As in the previous release (Update 2012-06-29), canned response matrices have been created for 13 different epochs for EPIC-MOS.

Update 2012-06-29

EPIC response files have been made available for the new SAS v12.0.1, released on the 25th June 2012. As in the previous release (Update 2011-04-12), canned response matrices have been created for 13 different epochs for EPIC-MOS.

Update 2011-04-12

EPIC response files have been made available for the new SAS v11.0.0 release on the 28th February 2011. The EPIC-MOS matrices have been substantially revised and now produce a fit which is more in agreement with the EPIC-pn and RGS cameras, especially at energies below 700 eV (see CCF release notes CAL-SRN-0272 and CAL-SRN-0273 for more information). The EPIC-MOS redistribution continues to evolve with time and canned response matrices have been created for 13 different epochs during the mission, and at three different positions on the detector.
 

Update 2010-10-26

EPIC response files have been made available for the new SAS v10.0.0 release on the 23th April 2010. The updated files make use of the new pn and MOS redistribution matrices (see CCF release notes XMM-CCF-REL-266 and XMM-CCF-REL-267 for more information on the new redistribution matrices for pn and MOS respectively).

Update 2009-07-07

EPIC response files have been made available as a tool for the feasibility study of AO-9 proposals. The new SAS v9.0.0 release on the 18th June 2009 does not affect the generation of the Canned Response Matrices, hence those generated with SAS 8.0.0 are still valid for AO-9 (see Update 2008-09-24 for more info).

Update 2008-09-24

The following EPIC response files have been made available as a tool for the feasibility study of AO-8 proposals.

EPIC Status of Calibration and Data Analysis document.

Update 2007-07-17

The following EPIC response files have been made available as a tool for the feasibility study of AO-7 proposals.

EPIC Status of Calibration and Data Analysis document.

Update 2006-02-16

A link to all of the most recent response matrices has been made in the pipeline directory. This allows users of source spectra, produced directly by the pipeline, to access the canned matrices which are referenced in the header of these spectra.

Update 2005-12-15

No ready-made MOS redistribution matrices are being provided as of SAS 6.5.

The low energy redistribution function (RMF) of the MOS CCDs has a complex shape, in that the main photopeak has a secondary component (a shoulder) which relatively increases with decreasing energy, until, at the very lowest energies, it is the dominant component. Observations of non- or weakly-varying sources, such as the SNR 1ES0102-72 and the O star Zeta Puppis, have shown that the shape of the in-flight redistribution function changes both spatially across the detector (the change from the on-ground calibration being most pronounced at the boresight) and also temporarily with observation epoch (Read et al. 2005, ESA-SP 604).

The form of this was such that the original shoulder had now evolved into a flatter 'shelf', of lower amplitude, but extending to lower energies. The bulk of the spatial change occurs within 40 arcseconds of the boresight, a region which we refer to as the "patch". A new method of deriving the RMF was constructed to account for this spatial and temporal variation. This has been incorporated into the Science Analysis Software (the SAS), such that as of SAS v6.5.0, there are now three RMF regions on each of the two MOS detectors; a "patch core" region, a "patch wings" region and an "outside patch" region. This, in combination with the 10 temporal epochs now considered in the SAS, gives rise to a total of 60 MOS RMFs in the current calibration files. For a source extracted close to the patch, rmfgen automatically constricts a PSF-(default) or flat-weighted average RMF from the three region-defined RMFs (making use, of course, of the calibration files from the correct epoch).

Since SAS 6.5, rmfgen produces RMF following the above method. No ready-made redistribution matrices are provided as of SAS 6.5 since this would require an infinite number, depending on the actual extraction region.
 

Users should, in general, use the rmf with the revolution number closest to the revolution in which their observation was performed. The revolution 534 matrices are, however, an exception to this rule. In this revolution the MOS detectors were cooled, resulting in a much improved spectral response. Therefore, observations with a revolution number greater than 534 should use the revolution 534 response files but earlier revolutions must use the previous response from e.g. revolution 439.

In timing mode (tu) only supporting pattern 0 is supported.

Update 2005-12-14

PN response files for all modes have been updated for SAS 6.5.0 and latest CCFs.

Update 2004-12-03

PN response files for all modes have been updated

This release improves the agreement between the MOS and PN responses below 1 keV. For further details please refer to XMM-SOC-SRN-0183.

Update 2004-10-15

MOS response files for all modes have been updated

The timing mode response has been much improved below 1 keV where large discrepancies with model fits were previously seen.

The tail of the redistribution function has been adjusted for all modes. This particularly affects very hard sources which previously showed an unnatural deficit at low energies wher e there were no source photons.

The naming convention has changed to include the revolution number. The general description above has been modified to reflect these changes.

Update 2004-07-28

Response files for both MOS and pn have been updated.

• pn: further adjustments of the redistribution parameters in the Partial Event Model at low energies (<600 eV) were done.
• MOS: Observations of calibration targets confirm a significant change in the low energy redistribution characteristics of the MOS cameras with time. This change is probably due to an increase in the surface charge loss property of the CCDs which degrades the low energy resolution. Epoch dependent calibration files have been produced which reflect these changes. For detailed information see XMM-SOC-CAL-SRN-169.

Update 2003-01-29

PN response files for all modes have been updated:

• Quantum efficiency QE (concerns all readout modes)
  New QE function is based on measurements of the thickness of the SiO2 layer on top of the CCD. This improves spectral fits around the O-edge.
   
• Spectral redistribution (concerns all readout modes)
  Data from the isolated neutron star RXJ1856.5-3754 were used to adjust the redistribution parameters in the Partial Event Model at low energies (<600 eV). The parameters were tuned to make the spectral fit parameters of RXJ1856.5-3754 consistent with those obtained by the Chandra LETG in high resolution. In particular the absorption column density agrees now with that obtained by the LETG, while before the pn value was too low.
   
• Charge Transfer Inefficiency (Small Window mode)
  The CTI correction for SW mode was further adjusted at low energies to further improve the spectral fits around the O-edge. At the O-edge the events were CTI-overcorrected before.

For further information please visit the Update Details Page

Update 2002-05-28

PN response files for timing and burst mode have now been added to the repository. Due to the lack of point sources with strong emission lines the energy resolution assumed to produce the RMF files for pn timing and burst mode has not been checked over the whole energy band. Be careful when interpreting derived line widths. Lines in spectra of extended sources are expected to be broadened by CTI correction which assumes a certain position of the source on the detector.

Update 2002-04-29

A set of CCD-only redistribution matrix files (RMF) are available here. These may be used in combination with the SAS task arfgen to provide the full response for the EPIC detectors on and off axis.

They are virtually identical to the files produced by the SAS task rmfgen but can be used to save time.

It is likely that they will be updated from time to time to give the user access to the current best knowledge independently of the SAS release schedule. Changes to the RMF tend to come from improvements to generation algorithms which imply a code change. Conversely, improvements in the knowledge of the instrument effective areas (produced by arfgen) can usually be included in updates to the CCF which avoids the need for a new software release.

The MOS files use the nomenclature ****all**** and *****p0*** which mean patterns 0-12 and pattern 0 only respectively. Pattern 0 is currently the only supported pattern type for timing mode observations. In imaging mode pattern 0 spectra can be selected to improve the spectral resolution for bright sources.

The PN response matrices are available for spectra...
(The corresponding information has been moved to the top of the page, since it is still valid ...)