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

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Michael Smith, ESAC

PN Monitoring

Palermo, April 2007

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Michael Smith, ESAC

Hot Pixels

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Michael Smith, ESAC

Noisy Pixels

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

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Michael Smith, ESAC

Offset Median

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Michael Smith, ESAC

Offset VarianceFirst Observations per Revolution

Eclipse Season Boundaries

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Michael Smith, ESAC

Offset Maps

Normal Variance Excessive Variance

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Michael Smith, ESAC

Mean Row Offset vs RAWYNormal Variance

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Michael Smith, ESAC

Mean Row Offset vs RAWYExcessive Q0 & Q2 Variance

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Michael Smith, ESAC

Mean Row Offset vs RAWYExcessive Q1 & Q3 Variance

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Michael Smith, ESAC

CalClosed Line Widths vs Offset Map Variance (I)

Quadrant 0 Quadrant 1

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Michael Smith, ESAC

CalClosed Line Centres vs Offset Map Variance (II)

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Michael Smith, ESAC

CalClosed Line Centres vs Offset Map Variance (III)

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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

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Michael Smith, ESAC

Relative Line Centres v Mean Row

slight Row Number – Line-Centre correlation

Correlation perhaps due to a slight

CTI over-correction

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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

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Michael Smith, ESAC

Line width trend is stable

~0.5 ADU/year increase at Mn

(Result of SAS 7.0 Processing)

M. Kirsch

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Michael Smith, ESAC

MOS Monitoring

Palermo, April 2007

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Michael Smith, ESAC

MOS1 Bad Pixels MOS2

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Michael Smith, ESAC

20Michael Smith, ESAC

XMM

EPIC MOS Monitoring

CAL/OPS Meeting

Palermo 11.04.2007

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MOS CTI monitoring

Using new public ADUCONV/CTI CCFs (03.04.2007)

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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

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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

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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

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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

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Michael Smith, ESAC

MOS line monitoring

Using new public ADUCONV/CTI CCFs (03.04.2007)

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Michael Smith, ESAC

EPIC MOS line monitoring: public CCFs

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Michael Smith, ESAC

EPIC MOS line monitoring: public CCFs

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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.

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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

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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

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Monitoring of the “meteorite” column in MOS1 CCD1

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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.

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Michael Smith, ESAC

EPIC telemetry monitoring

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Michael Smith, ESAC

Required telemetry of EPIC instruments

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Required EPIC telemetry revs. 1175-1333

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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),

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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.