statistics of galaxy groups in ultradeep xmm surveys alexis finoguenov max-planck institut fuer...
Post on 19-Dec-2015
216 views
TRANSCRIPT
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 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
Alexis Finoguenov Statistics of galaxy groups 9
COSMOS: scaling using weak lensing
Credit: Alexie Leauthaud + COSMOS weak lensing team
Alexis Finoguenov Statistics of galaxy groups 10
Group statistics:Group statistics: COSMOSCOSMOS & & CDFSCDFS
Self-consistent evidence for no evolution in Lx function!Self-consistent evidence for no evolution in Lx function!
Alexis Finoguenov Statistics of galaxy groups 11
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
Alexis Finoguenov 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
Alexis Finoguenov 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