XMM-Newton

1

Michael Smith, ESAC

PN Monitoring

Palermo, April 2007

XMM-Newton

2

Michael Smith, ESAC

Hot Pixels

XMM-Newton

3

Michael Smith, ESAC

Noisy Pixels

Due to Noisy Pixels in Column 64Most of these to be blanked in upcoming Bad Pixel Table upload

XMM-Newton

4

Michael Smith, ESAC

Offset Median

XMM-Newton

5

Michael Smith, ESAC

Offset VarianceFirst Observations per Revolution

Eclipse Season Boundaries

XMM-Newton

6

Michael Smith, ESAC

Offset Maps

Normal Variance Excessive Variance

XMM-Newton

7

Michael Smith, ESAC

Mean Row Offset vs RAWYNormal Variance

XMM-Newton

8

Michael Smith, ESAC

Mean Row Offset vs RAWYExcessive Q0 & Q2 Variance

XMM-Newton

9

Michael Smith, ESAC

Mean Row Offset vs RAWYExcessive Q1 & Q3 Variance

XMM-Newton

10

Michael Smith, ESAC

CalClosed Line Widths vs Offset Map Variance (I)

Quadrant 0 Quadrant 1

XMM-Newton

11

Michael Smith, ESAC

CalClosed Line Centres vs Offset Map Variance (II)

XMM-Newton

12

Michael Smith, ESAC

CalClosed Line Centres vs Offset Map Variance (III)

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

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

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

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

XMM-Newton

17

Michael Smith, ESAC

MOS Monitoring

Palermo, April 2007

XMM-Newton

18

Michael Smith, ESAC

MOS1 Bad Pixels MOS2

XMM-Newton

19

Michael Smith, ESAC

20Michael Smith, ESAC

XMM

EPIC MOS Monitoring

CAL/OPS Meeting

Palermo 11.04.2007

XMM-Newton

21

Michael Smith, ESAC

MOS CTI monitoring

Using new public ADUCONV/CTI CCFs (03.04.2007)

XMM-Newton

22

Michael Smith, ESAC

EPIC MOS CTI monitoring: public CCFs

Parallel CTI MOS1 Al Parallel CTI MOS2 Al

CCD1

CCD2

CCD3

CCD4

CCD5

CCD6

CCD7

0.06

0.00

XMM-Newton

23

Michael Smith, ESAC

EPIC MOS CTI monitoring: public CCFs

Parallel CTI MOS1 Mn Parallel CTI MOS2 Mn

CCD1

CCD2

CCD3

CCD4

CCD5

CCD6

CCD7

0.00

0.06

XMM-Newton

24

Michael Smith, ESAC

EPIC MOS CTI monitoring: public CCFs

Serial CTI MOS1 Al Serial CTI MOS2 Al

CCD1

CCD2

CCD3

CCD4

CCD5

CCD6

CCD7

-0.01

0.04

XMM-Newton

25

Michael Smith, ESAC

EPIC MOS CTI monitoring: public CCFs

Serial CTI MOS1 Mn Serial CTI MOS2 Mn

CCD1

CCD2

CCD3

CCD4

CCD5

CCD6

CCD7

-0.01

0.04

XMM-Newton

26

Michael Smith, ESAC

MOS line monitoring

Using new public ADUCONV/CTI CCFs (03.04.2007)

XMM-Newton

27

Michael Smith, ESAC

EPIC MOS line monitoring: public CCFs

XMM-Newton

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Michael Smith, ESAC

EPIC MOS line monitoring: public CCFs

XMM-Newton

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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.

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

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

XMM-Newton

32

Michael Smith, ESAC

Monitoring of the “meteorite” column in MOS1 CCD1

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.

XMM-Newton

34

Michael Smith, ESAC

EPIC telemetry monitoring

XMM-Newton

35

Michael Smith, ESAC

Required telemetry of EPIC instruments

XMM-Newton

36

Michael Smith, ESAC

Required EPIC telemetry revs. 1175-1333

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),

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.