XMM-Newton 1 M.Stuhlinger, ESAC MOS1 Timing Mode noise echo of the meteorite column Madrid, 23. March 2009
MOS1 Timing Mode noise echo of the meteorite column Madrid, 23. March 2009
Jan 05, 2016
MOS1 Timing Mode noise echo of the meteorite column Madrid, 23. March 2009. Discovery history:. During analyses of MOS1 timing mode exposures. My MOS1 timing mode spectrum of highly absorbed source 1E1740.7-2942 looks very different to MOS2/pn at low energies. - PowerPoint PPT Presentation
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XMM-Newton
1
M.Stuhlinger, ESAC
MOS1 Timing Mode
noise echo
of the meteorite column
Madrid, 23. March 2009
XMM-Newton
2
M.Stuhlinger, ESAC
Discovery history:
• During analyses of MOS1 timing mode exposures.
• My MOS1 timing mode spectrum of highly absorbed source 1E1740.7-2942 looks very different to MOS2/pn at low energies.
• Same spectrum extracted by Carlos Gabriel agrees with MOS2 and does not show low energy features.
XMM-Newton
3
M.Stuhlinger, ESAC
Different spectra extractions cause different appearance
XMM-Newton
4
M.Stuhlinger, ESAC
Discovery history:
• During analyses of MOS1 timing mode exposures.
• My MOS1 timing mode spectrum of highly absorbed source 1E1740.7-2942 looks very different to MOS2/pn at low energies.
• Same spectrum extracted by Carlos Gabriel agrees with MOS2 and does not show low energy features.
• Where do “my” low energy counts come from?Columns 320-327 show noise component shifted to lower energies with increasing RAWX.
XMM-Newton
5
M.Stuhlinger, ESAC
1E1740.7-2942
XMM-Newton
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M.Stuhlinger, ESAC
1E1740.7-2942
RA
WX
320
RA
WX
321
RA
WX
323
RA
WX
324
RA
WX
325
RA
WX
322
XMM-Newton
7
M.Stuhlinger, ESAC
Discovery:
• During analyses of MOS1 timing mode exposures.
• My MOS1 timing mode spectrum of highly absorbed source 1E1740.7-2942 looks very different to MOS2/pn at low energies.
• Same spectrum extracted by Carlos Gabriel agrees with MOS2 and does not show low energy features.
• Where do “my” low energy the counts come from?Columns 322-325 show noise component shifted to lower energies with increasing RAWX.
• Why the difference? We both exclude the hot column RAWX=319.Carlos used RAWX [300:316] (left PSF wing only), I used RAWX [300:317] or [321:330] (both PSF
wings with gap).
XMM-Newton
8
M.Stuhlinger, ESAC
1E1740.7-2942
6 p
ixel
s to
be
ign
ore
d
XMM-Newton
9
M.Stuhlinger, ESAC
MOS1 1E1740.7-2942 (rev.1065): PI versus RAWX
RAWX 323
RAWX 322
RAWX 324
RAWX 325
RAWX 321RA
WX
319
RAWX 320
RAWX
PI
XMM-Newton
10
M.Stuhlinger, ESAC
MOS1 Swift J1753.5-0127 (rev.1152): PI versus RAWX
RAWX 323
RAWX 322
RAWX 324
RAWX 325
RAWX 321
RA
WX
319
RAWX 320
RAWX
PI
XMM-Newton
11
M.Stuhlinger, ESAC
MOS1 4U0142+61 (rev.1300): PI versus RAWX
RAWX 323
RAWX 322
RAWX 324
RAWX 325
RAWX 321
RA
WX
319
RAWX 320
RAWX
PI
XMM-Newton
12
M.Stuhlinger, ESAC
Conclusions:
• Noise echo of meteorite column in RAWX [320:325] is common feature in MOS1 timing modes.
• Most probable noise echo is created within serial readout process.
• For extraction of MOS1 timing mode spectra (Rev.>961):
Better ignore RAWX [318:325]
• Large fraction of the right (higher RAWX values) PSF wing is lost!
• Already recommended: Avoid MOS1 observations in timing mode.
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