Astrometry and EPIC flux crosscalibration in 2XMMp2XMM

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Astrometry and EPIC flux cross-calibration in
2XMMp/2XMM
Silvia Mateos R. Saxton, S. Sembay and the
XMM-Newton Survey Science Centre
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2XMMp astrometry
SDSS-DR5 spectroscopic BLAGN sample (600 objects)
syserr0.3
blue stellar fx/foptgt -1
SDSS-DR5 statistically identified BLAGN
syserr0.3
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Statistical evaluation of 2XMMp/2XMM fluxes

• 2XMMp (and 2XMM) ECFs obtained with
• spectral model ?1.7 NH3x1020 cm-2
• One set of M1/M2 rmfs (from rev 534)
• Selected good quality sources
• gt250 cts per camera and energy bad
• (avoid Eddington bias)
• fluxeslt6x10-12 erg cm-2 s-1 per camera and
  energy band
• (avoid pile up effects)

• Evaluation of EPIC flux cross-calibration from
  observed
• distributions of flux differences (normalised)
  between cameras
• for each energy band
• different M1 off-axis angle
• revolution (time dependence)

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M2-M1
E1
E2
E4
E3
5
M2-M1
E5
Flux calibration differences between M1 and
M2 cameras lt5 level in all energy bands
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pn-M1
E1
E2
E3
E4
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pn-M1
E5
pn-MOS flux differences 10 for energy bands 1-4
and 15 for energy band 5
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on-axis lt5 arcmin (M1 central chip)off-axis
gt5 arcmin
pn-M1
M2-M1
9
pn-M1
M2-M1
10
Time dependence of 2XMMp/2XMM flux
cross-calibration
pn-M1
M2-M1
29-250
250-750
gt750
29-250
250-750
gt750
Small dependence with time of EPIC flux
cross-calibration Largest differences observed
for M2-M1 energy band 1 (0.2-0.5 keV)
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Summary

• Statistical analysis of EPIC flux
  cross-calibration in agreement with results from
  bright calibration objects
• M2-M1 flux differences 5 for all energy bands
• pn-MOS differences 10 for energy bands 1-4 and
  15 for energy band 5 (4.5-12 keV)
• See dependence of EPIC flux cross-calibration
  with off-axis sources
• Small time dependence of EPIC flux
  cross-calibration
• except for M2-M1 energy band 1

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pn-M1
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pn-M1