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Probing w(z) with future ISW measurements

Probing w(z) with future ISW measurements. http://physicsweb.org/. Levon Pogosian Syracuse University. With P.-S. Corasaniti, R. Crittenden, B. Nichol, C. Stephan-Otto. Extermal correlations of the CMB and Cosmology May 25-27, 2006, Fermilab. Growth factor. Growth Rate.

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Probing w(z) with future ISW measurements

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  1. Probing w(z) with future ISW measurements http://physicsweb.org/ Levon Pogosian Syracuse University With P.-S. Corasaniti, R. Crittenden, B. Nichol, C. Stephan-Otto Extermal correlations of the CMB and Cosmology May 25-27, 2006, Fermilab

  2. Growth factor Growth Rate Integrated Sachs-Wolfe effect

  3. Growth rate vs other probes “Growth Rate of Large Scale Structure as a Powerful Probe of Dark Energy” Cooray, Huterer & Baumann, astro-ph/0304268

  4. Cooray, Huterer & Baumann, astro-ph/0304268 Why?

  5. LSS and ISW are correlated http://physicsweb.org/ Crittenden & Turok, PRL96, astro-ph/9510072

  6. Current CMB/LSS correlation detection WMAP1 /HEAO-1:Boughn and Crittenden, astro-ph/0305001, 2.5-3 WMAP1 /NVSS:Boughn and Crittenden, astro-ph/0305001, 2-2.5 Nolta et al, astro-ph/0305097, 2-2.5 Vielva et al, astro-ph/0408252, 3.3 * McEwen et al, astro-ph/0602398, 3.9 * WMAP1 /APM:Fosalba and Gaztanaga, astro-ph/0305468, 2.5 WMAP1 /SDSS:Fosalba et al, astro-ph/0307249, 3 Scranton et al, astro-ph/0307335 N. Padmanabhan et al, astro-ph/0410360, 2.5 A. Cabre et al, astro-ph/0603690, 4.7 ** WMAP1 /2MASS:Afshordi et al, astro-ph/0308260, 2.5

  7. Precision cosmology? Compiled by Gaztanaga, Manera, Multamaki, astro-ph/0407022

  8. CMB/LSS correlation

  9. Planck CMB temperature and polarization http://sci.esa.int/ Future LSST 50 gal/arcmin2 20,000 deg2 10 photometric bins, zmax≈3 http://www.dmtelescope.org/

  10. ISW tomography LSST goal

  11. l(l+1)Xl/2π <z>~0.6 LCDM model

  12. S/N for LSST z-bins LCDM

  13. Other models (with same CMB TT)

  14. Precision cosmology with S/N<10? factor ~ 10 better sensitivity to DE properties probes large (linear) scales linear dependence on bias goes deep in z independent of  andr

  15. Model I flat geometry Planck +Planck/LSST +SNAP wa M w0 wa Pogosian, Corasaniti, Stephan-Otto, Crittenden, Nichol, astro-ph/0506396

  16. Model II: kink z w <w> today past

  17. Model II flat geometry Planck +Planck/LSST +SNAP w M <w> w Pogosian, Corasaniti, Stephan-Otto, Crittenden, Nichol, astro-ph/0506396

  18. Bias uncertainty

  19. Huterer & Starkman, PRL 2003 Principal Components

  20. Best determined modes R. Crittenden and L. Pogosian, astro-ph/0510293

  21. CMB/LSS correlation vs other probes General trend: high-z implies high frequency low frequency implies low-z CMB/LSS correlation: Provides a high-z low frequency mode “ Investigating dark energy experiments with principal components” R. Crittenden and L. Pogosian, astro-ph/0510293

  22. Summary competitive high-z constraints on wDE(z) a probe of alternatives to GR

  23. LSST bands

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