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Statistics of galaxy groups in ultraDeep XMM surveys Alexis Finoguenov Max-Planck Institut fuer extraterrestrische Physik University of Maryland, Baltimore.

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Presentation on theme: "Statistics of galaxy groups in ultraDeep XMM surveys Alexis Finoguenov Max-Planck Institut fuer extraterrestrische Physik University of Maryland, Baltimore."— 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 Alexis FinoguenovStatistics of galaxy groups2

3 Alexis FinoguenovStatistics of galaxy groups3 COSMOSCOSMOS

4 Alexis FinoguenovStatistics of galaxy groups4 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

5 Alexis FinoguenovStatistics of galaxy groups5 CDF S+N original

6 Alexis FinoguenovStatistics of galaxy groups6 CDF S+N restored

7 Alexis FinoguenovStatistics of galaxy groups7 CDF S+N diffuse

8 Alexis FinoguenovStatistics of galaxy groups8 CDFS: X-ray scaling relations

9 Alexis FinoguenovStatistics of galaxy groups9 COSMOS: scaling using weak lensing Credit: Alexie Leauthaud + COSMOS weak lensing team

10 Alexis FinoguenovStatistics of galaxy groups10 Group statistics: COSMOS & CDFS Self-consistent evidence for no evolution in Lx function!

11 Alexis FinoguenovStatistics of galaxy groups11 Survey strategies to detect evolution fx required area Lxz evol bias @peak z off survey 1.e-15>12.e43>11.81.9 UDS/DUX ultraVISTA 1.e-14>105.e43>0.72.61.4 XMM-LSS XCS 1.e-13>2002.e44>0.23.71.1 400d 1.e-12>10k1.e45>05.80.8RASS

12 Alexis FinoguenovStatistics of galaxy groups12 Strategy of high-z cluster detection 1

13 Alexis FinoguenovStatistics of galaxy groups13 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

14 Alexis FinoguenovStatistics of galaxy groups14 UDSUDS

15 Alexis FinoguenovStatistics of galaxy groups15 z=1.408 cluster

16 Alexis FinoguenovStatistics of galaxy groups16 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

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