X-ray properties of distant SHARC X-ray properties of distant SHARC clusters and cosmological implicationsclusters and cosmological implications

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XMM XMM -Project-Project

Collaborators :

D.H. Lumb, J.G. Bartlett (PI), A.K. Romer, A. Blanchard, D.J. Burke, C.A. Collins, R.C. Nichol, M. Giard, P. Marty, J. Nevalainen, R. Sadat, and S.C. Vauclair (me!).

+ http://webast.ast.obs-mip.fr/bax (X-ray cluster data base)

XMM observation of XMM observation of RXJ1120 RXJ1120

Z Z 0.6 0.6 TTxx=5.45 =5.45 0.3 keV 0.3 keV LLbolbol=14.4 10=14.4 104444 erg s erg s-1-1

PalermoPalermo 2003Arnaud et al, 2002Lumb et al., 2003, coming soon

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8 clusters with accurate 8 clusters with accurate Lx, Tx, Rc, Lx, Tx, Rc, z...z...significant fraction of thesignificant fraction of the high-z SHARC clusters z > 0.45high-z SHARC clusters z > 0.45Goal : L-T relation at high-z, Goal : L-T relation at high-z, a key ingredient in the number counts a key ingredient in the number counts

calculation.calculation.

GT GT observations:observations:

D.Lumb et al., 2003

XMM Lx-Tx evolutionXMM Lx-Tx evolution

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+ localXMM* Chandra

Lx/Tx)Lx/Tx)zz = Lx/Tx) = Lx/Tx)

z = 0z = 0(1+z)(1+z)withwith = 0.65 = 0.65

0.280.28in full agreement with Chandra (Vikhlinin et al, 2002), in full agreement with Chandra (Vikhlinin et al, 2002), and ASCA (Sadat et al., 1998; Novicki et al., 2003....)and ASCA (Sadat et al., 1998; Novicki et al., 2003....)

mm

FFrom X-ray Clustersrom X-ray Clusters

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Number counts:Number counts:

Vauclair et al, 2003,submitted

=> Lx-Tx relation

=> M-Tx relation + mass function

Local NormalizationLocal Normalization

50-60 ROSAT clusters => “Convergence” : Markevitch (1998), Blanchard et al. (2000), Pierpaoli al (2001, 2002), Ikebe et al (2002), Novicki et al (2002)

Need redshift evolution study to break the degeneracy between m and 8u

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5 different flux limited surveys: 5 different flux limited surveys:

EMSS, RDCS, B-SHARC, 160 degEMSS, RDCS, B-SHARC, 160 deg22, MACS, MACS

Modelling with Modelling with a)a) high high no free parameters no free parameters b) Concordance model (b) Concordance model (=0.7, =0.7, mm=0.3)=0.3)

[models normalized to local counts][models normalized to local counts]

Surveys used:Surveys used:

275 clusters with z > 0.3275 clusters with z > 0.3

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RDCS: 50 deg²fx 3. 10-14 erg/s/cm²

MACS: 22 000 deg²fx 10-12 erg/s/cm²

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160deg² down to z=0160deg² down to z=0with fwith fxx>2.10>2.10-13-13 erg/s/cm² erg/s/cm²

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●L-TL-T evolution with redshift evolution with redshift confirmed by XMMconfirmed by XMM

●SStrongtrong E Evolution in the abundance of x-ray volution in the abundance of x-ray clusters clusters appears from all existing surveys in a fully appears from all existing surveys in a fully consistentconsistent wayway

●IInsensitivensensitive to systematics (L-T, M-T, mass function…)to systematics (L-T, M-T, mass function…)

●TThis provides a strong argument in favor of a high his provides a strong argument in favor of a high matter density universe.matter density universe.

●RRelaxing this conclusion will require a major revision of elaxing this conclusion will require a major revision of

standard scaling of standard scaling of M-T (z)M-T (z) for instance i.e. for instance i.e. Tx Tx GM/rGM/r

Conclusions:Conclusions:

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