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Statistics of galaxy Statistics of galaxy groups in ultraDeep groups in ultraDeep
XMM surveys XMM surveys
Alexis FinoguenovAlexis Finoguenov
Max-Planck Institut fuer extraterrestrische PhysikMax-Planck Institut fuer extraterrestrische PhysikUniversity of Maryland, Baltimore CountyUniversity of Maryland, Baltimore County
& COSMOS, eCDFS, UDS/SXDF teams& COSMOS, eCDFS, UDS/SXDF teams
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Alexis Finoguenov Statistics of galaxy groups 2
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COSMOS
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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
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CDF S+N original
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CDF S+N restored
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CDF S+N diffuse
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CDFS: X-ray scaling relations
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COSMOS: scaling using weak lensing
Credit: Alexie Leauthaud + COSMOS weak lensing team
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Group statistics:Group statistics: COSMOSCOSMOS & & CDFSCDFS
Self-consistent evidence for no evolution in Lx function!Self-consistent evidence for no evolution in Lx function!
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Survey strategies to detect evolution
fxrequired
areaLx
z evol
bias@peak
z off survey
1.e-15
>1 2.e43 >1 1.8 1.9UDS/DUXultraVISTA
1.e-14
>10 5.e43 >0.7 2.6 1.4 XMM-LSSXCS
1.e-13
>200 2.e44 >0.2 3.7 1.1 400d
1.e-12
>10k 1.e45 >0 5.8 0.8RASS
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Strategy of high-z cluster detection
1
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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
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U
D
S
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z=1.408 cluster
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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