evolution of the thermodynamical and chemical properties ... · surface brightness analysis: csb+t...
TRANSCRIPT
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Paolo Tozzi Trieste
Evolution of the Thermodynamicaland Chemical properties of the
IntraCluster Medium
with I. Balestra, S. Ettori, P. Rosati, S. Borgani, J. Santos, A. Bignamini,
V. Mainieri, C. Norman
Granada, May 2008The X-ray Universe
XM
M2235: z=
1.39 180 ks w
ith C
han
dra, PI C
hris M
ullis
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Fe line is detected in most of the z>1 X-ray clusters
P. Rosati et al. 2004
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We select from the Chandra archive 56 clusters at z>0.3 (among them 7 clusters at z>1)
Distribution of temperature and z of the Chandra high-zsample
Balestra et al. 2007
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Iron abundance vs redshift
Balestra et al. 2007See also Maughan et al. 2008
Small effect of cooling cores.When does mostof the evolution occur?Use of XMM datafor 0.2<z<0.8
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Calura Matteucci & Tozzi 2007
Fe abundance evolution and S0 fraction evolution
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Cora et al. 2008
Dynamical origin of the Fe abundance evolution
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Santos et al. 2008
Investigating the Cool Core fraction in the distant Cluster population
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8
Characterization of a CC Cluster
– Central temperature decrease: Tcentral ~ 1/3 Taverage
– Central Surface Brightness (SB) excess
– Cooling time, tcool: shorter than Hubble Time
t cool∝C SB−0 .93
Santos et al. 2008
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Santos et al. 2008
Searching for cool cores in high-z clusters
LOW-z Strong CC
Mod CC - - -
NCC
HIGH-z Mod CC - - -
NCC
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X-ray properties of distant optically selected clusters (RCS)
Bignamini et al. 2008
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Santos et al. 2008
No cool cores in RCS (optically selected) Clusters
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The future of X-ray surveys
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WFXTpsf 5''FOV 1 sq deg
C. Norman, R. Giacconi, A. Ptak, P. Rosati, R. Gilli, S. Borgani, M. Paolillo, P.T., S. Allen +...
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Summary
Evidence of evolution in the average Fe abundance, a factor of 2 from z~0.5 to z=0. ICM was already substantially enriched at z>1. This evolution can be explained by the sink of low entropy, high-metallicity gas associated with small halos and/or galaxies.
Surface Brightness analysis: CSB+tcool
stacked SB profiles indicate
a significant fraction of moderate CC @ z=[0.7-1.4] Absence of pronounced CC at high-z Absence of pronounced CC in optical selected high-z cluster.
To capitalize what we have learned so far with Chandra and XMM we must have soon a mission devoted to a wide area deep survey with a good spatial resolution ~ 5'' like WFXT. The technological challenge for the mirrors is crucial.