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Cluster Cooling Cores and Cosmology T. H. Reiprich & C. L. Sarazin (UVa)

Cluster Cooling Cores and Cosmology T. H. Reiprich & C. L. Sarazin (UVa). How are CCC & C related? Understanding of cluster physics important to use clusters as precision cosmological tools. Chandra & XMM-Newton can make crucial contribution.

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Cluster Cooling Cores and Cosmology T. H. Reiprich & C. L. Sarazin (UVa)

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  1. Cluster Cooling Cores and CosmologyT. H. Reiprich & C. L. Sarazin (UVa) • How are CCC & C related? • Understanding of cluster physics important to use clusters as precision cosmological tools. • Chandra & XMM-Newton can make crucial contribution.

  2. Galaxy clusters can yield competitive cosmological constraints, however, systematic uncertainties dominate.

  3. Cooling Cores and LX-M Relation x: M/M200≥2*10-13 *: 0<M/M200<2*10-13 +: no c.f. Inferred from surface brightness deprojection of clusters from extended HIFLUGCS. (Chen et al., in prep.) Presence of CCCs affects LX-M and therefore cosmo- logical parameter estimates.

  4. HIFLUGCS Chandra andXMM-Newton Follow-up T. Reiprich, C. Sarazin, H. Boehringer, E. Blanton, Y. Chen, T. Clarke, A. Evrard, Y. Fujita, Y. Ikebe, E. Pierpaoli, S. Randall, P. Schuecker, G. Sivakoff, M. Takizawa

  5. HIFLUGCS • Contains 63 X-ray brightest (fX ≥ 2*10-11 erg/s/cm2) clusters in sky (excluding Galactic band). • Complete sample, based on deeper cluster samples from ROSAT All-Sky Survey. • Clusters reanalyzed using pointed PSPC and ASCA observations. • LX-M relation and tight statistical cosmological constraints from mass and temperature function (Reiprich & Boehringer 2002, Ikebe et al. 2002).

  6. HIFLUGCS Chandra examples. XMM-Newton examples.

  7. Strategy Outline • Develop automated procedures for homogeneous reduction and analysis of complete sample. • Determine temperature structure: • Inner profile: Chandra. • Intermediate/outer profile: XMM. • Flag mergers using HR/TX maps, compare to simulations / weak lensing data. • With SB profile: => Mass, gas mass fraction. • Determine fluxes / luminosities: • CCC / AGN contribution, compare to ROSAT fX at same radius. • With 2.: => LX-M, mass function -> cosmo pars.

  8. Note on LX-M Relation Fill up gap with 50 groups from Chandra archive….

  9. Analysis of complete sample will also yield… • bubble statistics, • cold front statistics, • correlation CCC-AGN, • merger frequency, • tighter constraints on evol. of MF -> w, • ….

  10. A1644XMM + DSS(Reiprich, Sarazin, Kempner, to be submitted)

  11. Main clumpChandra + DSS +VLA 1.4 GHz(M. Ledlow)

  12. Sub clumpChandra + DSS +VLA 1.4 GHz(M. Ledlow)

  13. X-Ray TemperatureMOS1-MOS2-pn,black = main cluster,red = sub cluster.Similar to relaxed clusters. Metal abundance

  14. HR mapMOS1-MOS2-pn,0.3-2 / 2-10 keV,bkg/exp/vig corr.,adapt. smoothed,flipped.Dark = cool /metal rich.Bright = hot.

  15. X-Ray TemperatureMOS1-MOS2-pn,selected regions. Metal abundance

  16. T mapOff-axis merger, hydrodynamical simulation(E. Tittley,poster 35).Remarkably similar.

  17. HR mapMOS1-MOS2-pn,0.3-2 / 2-10 keV,bkg/exp/vig corr.,adapt. smoothed,flipped.Dark = cool /metal rich.Bright = hot. All that with only 12ks of good data.

  18. Conclusion • Chandra & XMM-Newton observations of a complete sample needed to stay competitive in cosmology. • Complete HIFLUGCS follow-up cheap because clusters bright and large fraction in archive.

  19. Observations of HIFLUGCS Clusters Chandra XMM

  20. Conclusion • Chandra & XMM-Newton observations of a complete sample needed to stay competitive in cosmology. • Complete HIFLUGCS follow-up cheap because clusters bright and large fraction in archive.

  21. This is the End.

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