Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 1 XMM-Newton ESAC Status of XMM-Newton cross-calibration with SASv6.5 Martin Stuhlinger with inputs/support from whole cross-calibration team

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 2 XMM-Newton ESAC Cross-calibration team  ESAC: (Bruno Altieri), Marcus Kirsch, Leo Metcalfe, Andy Pollock, Richard Saxton, Michael Smith, Martin Stuhlinger, Antonio Talavera  Leicester: Steve Sembay, Andy Read, Darren Baskill  MPE: Frank Haberl, Michael Freyberg, Konrad Dennerl  SRON: Jelle Kaastra, Jan Willem den Herder, Cor de Vries, Jacco Vink  … and many others, including Chandra and Swift

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 3 XMM-Newton ESAC Talk outline  Major changes from SASv6.1 to SASv6.5 (EPIC)  Low-energy improvement: effect of the new pn redistribution (CCFs available since May 2005)  Spectral fitting examples on various sources  Chandra/XMM-Newton cross-calibration  Swift/XMM-Newton cross-calibration  Conclusions and outstanding issues

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 4 XMM-Newton ESAC Changes in SASv6.5 (1) New MOS rmf generation See talk by Andy Read  Time dependent  9 time epochs  Spatial dependent  3 spatial regions  3 spatial regions  18 new CCFs with SASv6.5 WARNING!!! Using SASv6.1, rmfgen could create responses with strange features A. Read MOS patch

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 5 XMM-Newton ESAC Changes in SASv6.5 (2) Improvement of arfgen  MOS flux correction for more than one missing column in sequence MOS SW: FLAG==0 MOS SW: XMMEA_EM

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 6 XMM-Newton ESAC Changes in SASv6.5 (3) Improvement of embadpixfind  New column rejection algorithm prevents erronious identification of bad columns  Emproc now using embadpixfind as well OldNew

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 7 XMM-Newton ESAC pn rmf tuning CCFs public since 14 May 2005 Old CCFs New CCFs Systematic S-shaped residuals … changed to flat residuals B. Altieri

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 8 XMM-Newton ESAC RXJ (1): pn flux stability  Rev  Rev  Rev  SW mode  Thin filter Changes by less than 1%

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 9 XMM-Newton ESAC RXJ (2) SASv6.1  Rev  Thin filter, SW  Great improve- ments in consistency with SASv6.5 SASv6.5

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 10 XMM-Newton ESAC 3C273 (1) SASv6.1  Rev  Medium filter  All EPICs in SW modes

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 11 XMM-Newton ESAC 3C273 (2)  Rev  Medium filter  All EPICs in SW modes SASv6.1

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 12 XMM-Newton ESAC 3C273 (3)  Rev  Medium filter  All EPICs in SW modes SASv6.1

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 13 XMM-Newton ESAC 3C273 (4)  Rev  Medium filter  All EPICs in SW modes SASv6.1

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 14 XMM-Newton ESAC 3C273 (5)  Rev  Medium filter  All EPICs in SW modes SASv6.1

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 15 XMM-Newton ESAC 3C273 (6)  Rev  Medium filter  All EPICs in SW modes

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 16 XMM-Newton ESAC 3C273 (7) Spectral summary:  Good agreement between the EPICs at all epochs  MOS2 bump ~20% at keV  pn bump of ~10% at keV  Above ~5 keV pn is lower than MOS by ~10%  RGS decreased by ~10-20% at lowest energies during the mission

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 17 XMM-Newton ESAC 3C273 (8): Low-energy flux ratios  keV  MOS to pn ratios decrease by less than 5%  RGS ratios decrease by 10-15%  Possible different changes for RGS1 and RGS2? cooling SASv6.1 S.Sembay

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 18 XMM-Newton ESAC 1ES (1) M. Smith  Rev  Thin filter  PN SW, MOS LW  40 lines plus absorbed bremsstrahlung  Line energies fixed to laboratory values  Line widths determined by RGS

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 19 XMM-Newton ESAC 1ES (2) M. Smith  Rev  Thin filter  PN SW, MOS LW  pn response under- estimates redistri- bution, most evident at O-lines  Above 0.6 keV the ageement is good  Backgound subtraction is problematic for pn SW mode

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 20 XMM-Newton ESAC 1ES (3) M. Smith  Rev  Thin filter  All EPICs in LW modes  pn LW mode agrees better than pn SW mode because background sub- traction for pn is less problematic

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 21 XMM-Newton ESAC 1ES (4) M. Smith  Rev  Thick filter  PN SW, MOS LW  Large pn-MOS discrepancies below 0.5 keV  Perhaps a filter issue (C-edge?) rather then redistribution

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 22 XMM-Newton ESAC 1ES (5) M. Smith  Rev  Thin filter  PN SW, MOS LW  Below 0.5 keV RGS flux has decreased  Hence the combined fits are unreliable at low energies.

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 23 XMM-Newton ESAC PKS M. Kirsch  Rev  Thin filter  PN SW, MOS LW  Early epoch, before MOS “patch”  Excellent agreement between all EPIC instruments SASv6.1

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 24 XMM-Newton ESAC PKS M. Kirsch  Rev. 0545, med., SW  MOS “patch” present  Good agreement at lowest and medium energies  MOSes lower by ~15% between keV  pn lower above 5 keV SASv6.1

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 25 XMM-Newton ESAC H  Rev  Medium filter, SW  Discrepancies reduced by ~10% SASv6.1

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 26 XMM-Newton ESAC XMM-Newton versus Chandra LETG M. Smith  PKS  XMM rev  Good agreement above 1 keV  ACIS/LETG has higher normalisation than the EPICs below 1 keV

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 27 XMM-Newton ESAC XMM-Newton versus Chandra HETG M. Smith  H  XMM rev  Very good agreement below 2 keV  Above 2 keV, ACIS/ HEG shows a flatter slope than the EPICs  Above 2 keV, MOS is closer to ACIS/ MEG than pn

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 28 XMM-Newton ESAC XMM-Newton versus Swift XRT  H  XMM rev  Good agreement between ~0.6 keV and ~3.0 keV  XRT measures steeper slope at high energies than the EPICs  Large discrepancies below ~0.6 keV

Martin Stuhlinger X-Ray Universe 2005, Sep.26-30, 2005 European Space Astronomy Centre Page 29 XMM-Newton ESAC Conclusions EPIC low-energy issue about to be solved :EPIC low-energy issue about to be solved : CCF for EPIC-pn available since 2005 MayCCF for EPIC-pn available since 2005 May Mechanisms for time- and spatial-dependent MOS redistribution are in SASv6.5, corresponding new EPIC-MOS CCFs publishedMechanisms for time- and spatial-dependent MOS redistribution are in SASv6.5, corresponding new EPIC-MOS CCFs published RGS :RGS : Low-energy flux difference ~10% at launchLow-energy flux difference ~10% at launch Sensitivity at the longest wavelengths has decreased by ~10-20% over the missionSensitivity at the longest wavelengths has decreased by ~10-20% over the mission Status in SASv6.5: EPIC and RGS are not yet consistent below ~0.7 keVStatus in SASv6.5: EPIC and RGS are not yet consistent below ~0.7 keV Open cross-calibration issues : Open cross-calibration issues : Implement best knowledge of RGS into SAS (see previous talk) Implement best knowledge of RGS into SAS (see previous talk) Which of MOS or pn is right at high energies? Which of MOS or pn is right at high energies? EPIC rmf’s at low energies: still room for improvement EPIC rmf’s at low energies: still room for improvement We keep on cross-calibrating happily…