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Statistics of Galaxy Groups in UltraDeep XMM Surveys

This study by Alexis Finoguenov from Max-Planck Institut für extraterrestrische Physik & University of Maryland, Baltimore County, along with the COSMOS, eCDFS, and UDS/SXDF teams, delves into the challenges faced in analyzing galaxy groups using XMM surveys. The research covers topics such as incomplete candidate lists, verification against Chandra clusters, false detections, proper threshold ratios for point vs. extended sources, AGN flux removal, and benefits of Chandra coverage. It also explores X-ray scaling relations, scaling using weak lensing, and survey strategies for detecting evolution in galaxy groups. The study provides self-consistent evidence for no evolution in the Lx function and emphasizes the importance of deep X-ray surveys to understand cosmological parameters at high redshift clusters.

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Statistics of Galaxy Groups in UltraDeep XMM Surveys

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  1. Statistics of galaxy groups in ultraDeep XMM surveys Alexis Finoguenov Max-Planck Institut fuer extraterrestrische Physik University of Maryland, Baltimore County & COSMOS, eCDFS, UDS/SXDF teams

  2. Statistics of galaxy groups

  3. COSMOS Statistics of galaxy groups

  4. Challenges due to XMM PSF • Incomplete candidate list • Verified against Chandra clusters • False detection • Proper threshold ratio for point vs extended source • AGN flux removal • Profits from having Chandra coverage Statistics of galaxy groups

  5. CDF S+N original Statistics of galaxy groups

  6. CDF S+N restored Statistics of galaxy groups

  7. CDF S+N diffuse Statistics of galaxy groups

  8. CDFS: X-ray scaling relations Statistics of galaxy groups

  9. COSMOS: scaling using weak lensing Credit: Alexie Leauthaud + COSMOS weak lensing team Statistics of galaxy groups

  10. Group statistics:COSMOS & CDFS Self-consistent evidence for no evolution in Lx function! Statistics of galaxy groups

  11. Survey strategies to detect evolution Statistics of galaxy groups

  12. Strategy of high-z cluster detection 1 Statistics of galaxy groups

  13. The UKIDSS Ultra-Deep Survey 0.77 sq degrees K=23, H=24, J=25 (5, Vega, point source) Year 1: K=21.8, J=23.0 (86 hours) EDR: K=20.6, J=21.7 (12 hours) 0.88 deg. Almaini et al. 2006 Statistics of galaxy groups

  14. UDS Statistics of galaxy groups

  15. z=1.408 cluster Statistics of galaxy groups

  16. Conclusions • Deep surveys are dominated by clusters with non-evolving luminosity function • X-ray spectroscopy, stacked weak lensing and clustering could all be used to yield the total mass • Deep X-ray surveys extended over an area >1 square degree access cosmological parameters at z=1.5 Statistics of galaxy groups

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