1 / 16

Statistics of Galaxy Groups in UltraDeep XMM Surveys: Challenges and Strategies

This study delves into the statistical analysis of galaxy groups within UltraDeep XMM surveys, highlighting challenges such as incomplete candidate lists and false detections. Proper threshold ratios for point versus extended sources and AGN flux removal are essential for accurate results. The benefits of Chandra coverage for verification are also discussed. Various X-ray scaling relations and weak lensing techniques are utilized for cluster detection and evolution analysis, emphasizing evidence for no evolution in Lx function. Survey strategies and high-z cluster detection tactics are outlined, including insights from the UKIDSS Ultra-Deep Survey. Deep surveys reveal non-evolving luminosity functions and the potential of X-ray spectroscopy, weak lensing, and clustering for mass estimation. Deep X-ray surveys spanning over a square degree provide valuable insights into cosmological parameters at z=1.5.

francesca-gould
Download Presentation

Statistics of Galaxy Groups in UltraDeep XMM Surveys: Challenges and Strategies

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related