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Low energy calibration with the Vela SNR

Low energy calibration with the Vela SNR. EPIC Calibration & Operations Meeting. Mallorca, Spain, 2009 March 31 – April 1. Vela SNR: extended source with bright OVII emission.  excellent calibration source. 2001- 2007: 12 long FF observations,

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Low energy calibration with the Vela SNR

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  1. Low energy calibration with the Vela SNR EPIC Calibration & Operations Meeting Mallorca, Spain, 2009 March 31 – April 1

  2. Vela SNR: extended source with bright OVII emission  excellent calibration source 2001- 2007: 12 long FF observations, several with different pointing coordinates and roll angles  fairly homogeneous illumination of the detector

  3. Monitoring the absolute energy scale @ 0.57 keV with the Vela SNR:

  4. Monitoring the absolute energy scale @ 1.49 keV with the internal calibration source:

  5. Comparison: trends at 0.57 keV and 1.49 keV Vela SNR 0.57 keV internal calibration source 1.49 keV

  6. Comparison: trends at 0.57 keV and 1.49 keV 0.574 keV (Vela SNR) 1.486 keV (Al-K, scaled)

  7. Internal calibration source onboard XMM-Newton / EPIC-pn Al-K Mn-K inhomogeneous irradiation at Mn-K, illumination of quadrant 3 very poor

  8. Superposition of all Vela SNR observations in FF mode 0.40 – 0.74 keV photon map (singles) exposure map maximum: 172 singles/pixel total exposure (after removing times of background flares): ~300 ks exposure corrected map

  9. Spatial properties of the absolute energy scale 0.40 – 0.74 keV photon map (singles)  adaptive binning into subareas of similar signal

  10. Spatial properties of the absolute energy scale vertical binning according to response matrices horizontal binning adaptively, criterion: ~5000 single events within 400 – 740 eV (above background)  422 fields

  11. Preparations for a joint fit removal of periods of enhanced background correction for local energy shifts due to errors in the offset map (epreject) correction for energy shifts between the individual observations correction for out-of-time events

  12. Spectral model used ( E = 0.43 – 0.74 keV ) all line energies and widths coupled to reference line (O VII r) relative line fluxes of O VII triplet fixed continuum approximated by powerlow 8 fit parameters

  13. Spectral model used ( E = 0.43 – 0.74 keV )

  14. result: energy scale spatially homogeneous within ±10 eV however, also evidence for systematic shifts in a ring-like pattern

  15. Checks for stability and reproducibility of the result removal of periods of enhanced background correction for local energy shifts due to errors in the offset map (epreject) correction for energy shifts between the individual observations correction for out-of-time events different binning, different spectral models

  16. EPIC-Cal Meeting, Tübingen, Germany, 2003 Feb 3-5 1.186 keV (Ge-L) 9.874 keV (Ge-K)

  17. EPIC-Cal Meeting, Tübingen, Germany, 2003 Feb 3-5 1.186 keV (Ge-L) 9.874 keV (Ge-K)

  18. Printed Circuit Board

  19. EPIC-Cal Meeting, Tübingen, Germany, 2003 Feb 3-5 1.186 keV (Ge-L) 9.874 keV (Ge-K)

  20. EPIC-Cal Meeting, Tübingen, Germany, 2003 Feb 3-5

  21. EPIC-Cal Meeting, VILSPA, Spain, 2004 Mar 23-24

  22. EPIC-Cal Meeting, Mallorca, Spain, 2009 March 31 – April 1

  23. Comparison with Mn-K

  24. Comparison with Mn-K

  25. Mn-K

  26. EPIC-Cal Meeting, MPE-Garching, Germany, 2006 May 4 20 adu image, rev 546 Correcting spatial inhomogeneities of the absolute energy scale • offsets in the energy scale due to errors in the offset map • column gain variations after launch • CTI changes due to residual light through the ventilation hole

  27. Correcting spatial inhomogeneities of the absolute energy scale • offsets in the energy scale due to errors in the offset map • column gain variations after launch • CTI changes due to residual light through the ventilation hole EPIC-Cal Meeting, Mallorca, Spain, 2007 Nov 6-7

  28. Correcting spatial inhomogeneities of the absolute energy scale • offsets in the energy scale due to errors in the offset map • column gain variations after launch • CTI changes due to residual light through the ventilation hole EPIC-Cal Meeting, Mallorca, Spain, 2007 Nov 6-7

  29. Correcting spatial inhomogeneities of the absolute energy scale • offsets in the energy scale due to errors in the offset map • column gain variations after launch • CTI changes due to residual light through the ventilation hole EPIC-Cal Meeting, Mallorca, Spain, 2009 March 31 – April 1

  30. Low energy calibration with the Vela SNR EPIC Calibration & Operations Meeting Mallorca, Spain, 2009 March 31 – April 1

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