XMM-Newton 1 Michael Smith, ESAC PN Monitoring Palermo, April 2007.
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Transcript of XMM-Newton 1 Michael Smith, ESAC PN Monitoring Palermo, April 2007.
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XMM-Newton
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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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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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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
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20Michael Smith, ESAC
XMM
EPIC MOS Monitoring
CAL/OPS Meeting
Palermo 11.04.2007
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Michael Smith, ESAC
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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Michael Smith, ESAC
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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Michael Smith, ESAC
Required EPIC telemetry revs. 1175-1333
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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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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.