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

Alexis Finoguenov Statistics of galaxy groups 2

Alexis Finoguenov Statistics of galaxy groups 3

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