1. XMM-Newton 1 Michael Smith, ESAC PN Monitoring Palermo, April 2007

2. XMM-Newton 2 Michael Smith, ESAC Hot Pixels

3. XMM-Newton 3 Michael Smith, ESAC Noisy Pixels Due to Noisy Pixels in Column 64 Most of these to be blanked in upcoming Bad Pixel Table upload

4. XMM-Newton 4 Michael Smith, ESAC Offset Median

5. XMM-Newton 5 Michael Smith, ESAC Offset Variance First Observations per Revolution Eclipse Season Boundaries

6. XMM-Newton 6 Michael Smith, ESAC Offset Maps Normal Variance Excessive Variance

7. XMM-Newton 7 Michael Smith, ESAC Mean Row Offset vs RAWY Normal Variance

8. XMM-Newton 8 Michael Smith, ESAC Mean Row Offset vs RAWY Excessive Q0 & Q2 Variance

9. XMM-Newton 9 Michael Smith, ESAC Mean Row Offset vs RAWY Excessive Q1 & Q3 Variance

10. XMM-Newton 10 Michael Smith, ESAC CalClosed Line Widths vs Offset Map Variance (I) Quadrant 0Quadrant 1

11. XMM-Newton 11 Michael Smith, ESAC CalClosed Line Centres vs Offset Map Variance (II)

12. XMM-Newton 12 Michael Smith, ESAC CalClosed Line Centres vs Offset Map Variance (III)

13. XMM-Newton 13 Michael Smith, ESAC  Slight Offset – Line-Centre correlation  Slopes of the order of ~ 0.1 eV / ADU in stead of the ~ 5 eV / ADU one would expect for a simple offset shift  Probably nothing to do with relative offset shifts… Relative Line Centres v Relative Offsets

14. XMM-Newton 14 Michael Smith, ESAC Relative Line Centres v Mean Row  slight Row Number – Line-Centre correlation  Correlation perhaps due to a slight CTI over-correction

15. XMM-Newton 15 Michael Smith, ESAC Energy Scale vs Time very good, esp. for FF mode. Slight over-correction for EFF mode. SW mode under- correction, esp. at Mn (Result of SAS 7.0 Processing) M. Kirsch

16. XMM-Newton 16 Michael Smith, ESAC Line width trend is stable ~0.5 ADU/year increase at Mn (Result of SAS 7.0 Processing) M. Kirsch

17. XMM-Newton 17 Michael Smith, ESAC MOS Monitoring Palermo, April 2007

18. XMM-Newton 18 Michael Smith, ESAC MOS1 Bad Pixels MOS2

19. XMM-Newton 19 Michael Smith, ESAC

20. XMM 20 EPIC MOS Monitoring CAL/OPS Meeting Palermo 11.04.2007

21. XMM-Newton 21 Michael Smith, ESAC MOS CTI monitoring Using new public ADUCONV/CTI CCFs (03.04.2007)

22. XMM-Newton 22 Michael Smith, ESAC EPIC MOS CTI monitoring: public CCFs Parallel CTI MOS1 AlParallel CTI MOS2 Al CCD1 CCD2 CCD3 CCD4 CCD5 CCD6 CCD7 0.06 0.00

23. XMM-Newton 23 Michael Smith, ESAC EPIC MOS CTI monitoring: public CCFs Parallel CTI MOS1 MnParallel CTI MOS2 Mn CCD1 CCD2 CCD3 CCD4 CCD5 CCD6 CCD7 0.00 0.06

24. XMM-Newton 24 Michael Smith, ESAC EPIC MOS CTI monitoring: public CCFs Serial CTI MOS1 AlSerial CTI MOS2 Al CCD1 CCD2 CCD3 CCD4 CCD5 CCD6 CCD7 -0.01 0.04

25. XMM-Newton 25 Michael Smith, ESAC EPIC MOS CTI monitoring: public CCFs Serial CTI MOS1 MnSerial CTI MOS2 Mn CCD1 CCD2 CCD3 CCD4 CCD5 CCD6 CCD7 -0.01 0.04

26. XMM-Newton 26 Michael Smith, ESAC MOS line monitoring Using new public ADUCONV/CTI CCFs (03.04.2007)

27. XMM-Newton 27 Michael Smith, ESAC EPIC MOS line monitoring: public CCFs

28. XMM-Newton 28 Michael Smith, ESAC EPIC MOS line monitoring: public CCFs

29. XMM-Newton 29 Michael Smith, ESAC EPIC MOS line monitoring: public CCFs Line resolution The column dependent MOS CTI CCFs can improve the line resolution because: The spectral deviation of all individual columns is minimised. The correction leads to an increase of the number of counts in the line centroid. Will mainly affect extended sources.

30. XMM-Newton 30 Michael Smith, ESAC EPIC MOS line monitoring: public CCFs Improvement of FWHM due to column dependent CTI CCFs: Al (mean post-cooling values) MOS1: 4.4% old: 80 eV  new: 76 eV MOS2: 4.2% old: 79 eV  new: 75 eV

31. XMM-Newton 31 Michael Smith, ESAC EPIC MOS line monitoring: public CCFs Improvement of FWHM due to column dependent CTI CCFs : Mn (mean post-cooling values) MOS1: 3.4% old: 145 eV  new: 140 eV MOS2: 3.4% old: 142 eV  new: 137 eV

32. XMM-Newton 32 Michael Smith, ESAC Monitoring of the “meteorite” column in MOS1 CCD1

33. XMM-Newton 33 Michael Smith, ESAC Disappeared for imaging modes Column was off since change of on-board offset June 2005. Re-appeared in rev. 1100-1115: Diagnostic shows column offset to be 130 ADU (instead of 123 ADU). At lower level or disappeared in rev. 1116-1122: Diagnostics show column offset back on expected level. During and after eclipse phase rev.1123-1135 column sometimes is hot and sometimes normal. No hot column from rev. 1136-1148. Column present in single exposures from 1149-1156. No hot column since rev. 1157 (-1333) in imaging modes (except 3x3), but in timing modes.

34. XMM-Newton 34 Michael Smith, ESAC EPIC telemetry monitoring

35. XMM-Newton 35 Michael Smith, ESAC Required telemetry of EPIC instruments

36. XMM-Newton 36 Michael Smith, ESAC Required EPIC telemetry revs. 1175-1333

37. XMM-Newton 37 Michael Smith, ESAC Critical observations of revs. 1175-1333 In total 650 MOS1 and 653 MOS2 exposures. 56 FF, 3 LW and 3 SW observations were affected by counting modes, most due to high radiation. 21 MOS1 TI observations were affected by counting modes, all with rates higher than 1/300 sec. Only 3 of these (Crab) have MOS2 counterparts. Due to hot “meteorite” column. 3 MOS2 TI observation exceeded the 12 kbits/sec and were not affected by counting modes (2x XB 1254-690 + Mkn 421),

38. XMM-Newton 38 Michael Smith, ESAC Conclusion Line energies within 5 eV. Line widths (FWHM) stable since cooling: ~76 eV at Al energy and ~140 eV at Mn energy. CTIs are still very stable since cooling. MOS1 “meteorite” column did not appear again in imaging modes, but in several timing mode exposures. New BRAT restricted only few MOS observations between revs. 1175- 1333 (not affected by high radiation). Low energy noise still present. Reason still unknown.