i. balestra , p.t., s. ettori, p. rosati, s. borgani, v. mainieri, m. viola, c. norman
DESCRIPTION
Galaxies and Structures through Cosmic Times - Venice, March 2006. Evolution in the chemical enrichment of the intracluster medium. I. Balestra , P.T., S. Ettori, P. Rosati, S. Borgani, V. Mainieri, M. Viola, C. Norman. High redshift (z>0.3) clusters in medium- deep Chandra exposures - PowerPoint PPT PresentationTRANSCRIPT
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I. BalestraI. Balestra, P.T., S. Ettori, P. Rosati, , P.T., S. Ettori, P. Rosati, S. Borgani, V. Mainieri, M. Viola, C. NormanS. Borgani, V. Mainieri, M. Viola, C. Norman
Galaxies and Structures through Cosmic Times - Venice, March 2006
Evolution in the chemical enrichment of the intracluster
medium
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High redshift(z>0.3) clusters in medium-deep Chandraexposures(ACIS-I andACIS-S)
Science:Scaling relations(temperature, luminosity, massentropy)Chemical enrichmentAGN around clustersBaryon fraction and cosmological test
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RXJ1252: detection of the Fe line at z=1.23
Rosati et al. 2004
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Fe Ions concentration as a function of the ICM temperature
Collisionally dominated optically thin coronal plasmaas a function of electron temperature (Mewe 1991)
5 -10 keVFe XXVFe XXVI
The Iron abundance is determined almost uniquely by the K-shell complex at 6.7-6.9 keV rest-frame
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We select from the Chandra archive 56 clusters at z>0.3(among them 7 clusters at z>1)
Distribution with temperature and redshift of the sample
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We samplecentral regionsbetween 0.15and 0.3 R
vir
depending on the redshiftof the cluster
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Temperature vs redshift (56 clusters @ z> 0.3)3 times more objects than in Tozzi et al. 2003
Balestra et al. 2006
Caveat: two differentvalues of solar Fe abundin the literature:
Anders & Grevesse 1989Fe/H = 4.68 × 10-5
Grevesse & Sauval 1998Fe/H = 3.16 × 10-5
ZFeGS
= 1.48 ZFeAG
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Scatter comparable with statistical errorshint ofhigherFe abundanceat low kT<5 keV
Fe abundance-Temperature in different redshift bins
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Iron abundance -Temperature
Weightedaverage
Balestra et al. 2006
An
der
s &
Gre
vess
e 19
89
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Horner 2001 PhDBaumgartner et al. 2005
Local sample 273 clusters observed with ASCAG
reve
sse
& S
auva
l 199
818 local clusters observed with ASCAFinoguenov, Arnaud & David 2001
An
der
s &
Gre
vess
e 19
89XMM-Grating data from cool core cluster Peterson et al. 2003
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Iron abundance versus redshift
Balestra et al. 2006
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Average Iron abundance versus redshift
Balestra et al. 2006
We find an increase of a factor about 2 in Z
Fe
from z=1.2 to z=0.4 in the central 0.2 R
vir of
hot clustersconsistent with Z
Fe = 0.55 (1+z)-1.3
This larger sample showshigher Z
Fe at z<0.5,
implying significant evolution (Tozzi et al. 2003 was still consistentwith no evolution, with weak hints of decrease at less than 2 σ c.l.)
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It is known that locally ZFe
= 0.6 in cold-core clusters and Zfe = 0.2/0.3 in
non cold-core clusters (see De Grandi et al. 2001; 2004).
Is this evolution associated to the evolution of the cold-cores with Iron peak within the central 0.1 R
vir?
First check: Iron abundances are not affected by removal of the lowenergy part of the spectrum, nor by masking of the central 0.1 R
vir
(when possible)
More directly, there is no correlation with the central surface brightness(cooling time)
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Fe Abundance vs central Surface Brightness
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Is the Iron abundance evolution expected?
Ettori 2005
Fe abundance in the ICM from the observed cosmic Star Formation Ratewith different delay times for TyIa Sne
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CONCLUSIONS
Clear detection of the Iron line in the large majority of high-z clusters, up to z~1.3
Correlation in the Iron abundance – Temperature relation at high-z: Iron abundance starts to increase below 5 keV
Fe abundance ~ 0.25 Z⊙ constant for z>0.6
Higher average Fe abundance in the z~0.4-0.6 redshift range
The decrease of the average Iron abundance from ZFe
=0.4 Z⊙(@ z~0.3)to Z
Fe=0.2 Z⊙ (z~1.3), consistent with cosmic star formation rate only
for large TyIa delay times.
Open question: production of diffusion of Fe enriched gas betweenz=1.2 and z=0.4?
A sample of ~56 clusters @ z>0.3 observed with Chandra
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Metallicity profiles for 4 clusters with high S/N
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Temperature and Fe abundance fromChandra+XMM (MOS) combined fit
Rosati et al. 2004
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Redshift measure fromChandra+XMM (MOS) combined fit
Rosati et al. 2004
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Chandra+XMM observation of RXJ1252Rosati et al. 2003
Detection of the Fe line of the most distant X-ray clusters
RXJ1252~1000 net counts180 ks with ACIS-IRosati et al. 2004
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kT < 5 keV
Is it due to cool core with Iron excess?
Simplistic spatialspectroscopy (first 2 rings with reasonable S/N)
Iron-rich clustersdo not necessarily show Iron-richcores
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What is the nature of low temperature, Iron rich clusters?
A typical example: V14156, z=0.4
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Investigating the nature of Fe-rich clusters:Simulated XMM spectrum of V1416 - 50 ksec
XMM proposal: Why low-temperature clusters have high Iron abundance?
The case at 0.2 < z < 0.5
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Can we measure the elements at high redshifts through the stacking technique?
Residual of the spectrawith respect to thebremmstrahlung onlymodel
Ettori et al in progress
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The residuals match with expected lines from Si, Ca, and S!
Ettori et al in progress
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Abundance ratios at z~1 as diagnostic tool
Ettori et al. 2005