XMM-Newton surveys of X-ray galaxy groups Alexis Finoguenov MPE/UMBC+ S.Giodini, V.Allevato, M. Tanaka, A. Leauthaud, O. Ilbert, N.Cappelluti, J.Silverman,

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Presentation transcript:

XMM-Newton surveys of X-ray galaxy groups Alexis Finoguenov MPE/UMBC+ S.Giodini, V.Allevato, M. Tanaka, A. Leauthaud, O. Ilbert, N.Cappelluti, J.Silverman, K. Kovac, V.Smolcic, JP Kneib, H. McCracken, S. Lilly, N.Scoville, G.Hasinger, M. Elvis, A. Comastri, M. Cooper, J. Mulchaey, P.Nandra +COSMOS, CDFS, DEEP2, CFHTLS teams

Why study galaxy groups? Baryonic budget of the Universe Galaxy evolution f(r,M,z) well defined size well defined mass Central galaxy start to dominate the total stellar mass Bridges between clusters and the field Alexis FinoguenovCluster cosmology in Deep Fields2

Groups and their galaxies Alexis FinoguenovCluster cosmology in Deep Fields3 ?

XMM-COSMOS 2deg2: 300cl Flux keV (cgs) CDFN 0.2deg2 30 cl DEEP2 2.6 sq.degs 20 deg2 XMM-LSS (Pierre’ 04) 600 cl SZ-CA (Boehringer’07) 100 deg: XMM-CFHTLS: 60 massive clusters Contiguous X-ray cluster surveys in context Area SXDF 1.1 deg2: 100 cl Lockman Hole, 0.3sq.deg. 30cl 4Cluster cosmology in Deep Fields CDFS 0.3 sq.deg. 50cl Alexis Finoguenov l=1000

Alexis FinoguenovCluster cosmology in Deep Fields5 Groups are not scaled down clusters! Quenched galaxies Mass=>feedback (AGN) quenching Field: mainly dwarf galaxies are quenched by environment Field: mainly dwarf galaxies are quenched by environment Both components are seen in 3.e13 groups Both components are seen in 3.e13 groups Clusters are dominated by environmental quenching Clusters are dominated by environmental quenching

6 Photoz z=0.8 z=0.6 z=0.4 z=0.2 I AB <25 1.4Mio galaxies X-ray contours l=3000 COSMOS Mass calibration Variety of groups Galaxy properties: stellar mass SFR AGN Morphology LSS

7 K.Kovac Groups and LSS zCOSMOS groups

Lx-Mass from weak lensing Leauthaud, AF et al lgM=0.6lgLx+C

9 Less gas More stars Stellar content of galaxy groups Giodini et al. 2010

SFR Alexis Finoguenov10 Herschel results

Increased red [OII] emitters in groups at high redshifts Not only the fraction, but the strengths of [OII] increases as well. groups field Tanaka, AF, et al. submitted. Based on the 30-band photometry (NUV-r from Ilbert et al. 2010), we find these red [OII] emitters are not undergoing active star formation. The [OII] emission is likely due to AGNs.

Resolving LSS with X-ray groups Alexis FinoguenovView on baryons from COSMOS12

Radio AGN HOD: marked mass function Alexis FinoguenovCluster cosmology in Deep Fields13

Next steps: z~1 – DEEP2 Alexis FinoguenovCluster cosmology in Deep Fields14 Erfanianfar, AF, in prep.

CFHTLS Lerchster, …, AF et al. 2011; Mirkazemi, AF, et al. in prep.

Summary Alexis FinoguenovCluster cosmology in Deep Fields16 Survey of groups explore parameter space opened by both X-ray observations and the multiwavelength data Contrary to cosmology goals, in group studies the least massive group is the most treasured Unprecedented XMM coverage of COSMOS and CDFS enabled the study of barionic budget of groups and environmental dependence of SFR to a z~1 Extension of those surveys towards higher-z (DEEP2) and higher mass (CFHTLS) have been achieved Near future of group research is associated with Ultra- VISTA and CANDELS datasets

17 A. Faltenbacher, AF, N. Drory 2010 ApJ Fraction of matter resolved in groups Simulations… Alexis Finoguenov

GSMF – active vs passive Alexis FinoguenovCluster cosmology in Deep Fields18