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XMM v Chandra - Cluster Analysis

Explore the systematic discrepancy between Chandra and XMM-Newton EPIC MOS in fitted temperature profiles for higher temperature galaxy clusters. This discrepancy, as much as 2 keV, is unlikely due to the larger XMM-Newton point spread function.

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XMM v Chandra - Cluster Analysis

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  1. XMM v Chandra - Cluster Analysis Steve Snowden NASA/Goddard Space Flight Center EPIC Operations and Calibration Meeting Mallorca 6-7 October 2007

  2. Initial Signs Fitted temperature radial profiles for the cluster of galaxies Abell 1795 Abell 1795 is the poster child for the discrepancy. Chandra data (boxes) and XMM data (other)

  3. Consistent Discrepancy • Comparison of multiple galaxy clusters shows a significant and systematic discrepancy between Chandra and XMM-Newton MOS results. • The higher the temperature, the greater the Chandra temperature is relative to XMM

  4. Not a Question of XMM Consistency • Comparison of fitted profiles from repeated XMM observations shows excellent consistency

  5. Not an Issue with Recent Changes • Comparison of fitted temperatures before and after the recent MOS QE changes. • Changes by Steve Sembay in the MOS QE does not change the situation.

  6. Will Significantly Affect Science • Fundamental science in the radial profiles of clusters

  7. Bottom Line – With all current corrections there is a systematic discrepancy between Chandra and XMM-Newton EPIC MOS fitted temperatures for higher temperature clusters. The higher the fitted temperature the more likely the case that Chandra will find a higher temperature. The difference is significant, as much as 2 keV. This is very unlikely to be due to the larger XMM PSF. –> cross-talk arfgen modification by Richard Saxton –> not affected by using Chandra image for arfgen cross-talk –> most noticeable in flat part of profile

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