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Center for Cosmology and Astro-Particle Physics

Probing Dark Energy with Cluster-Galaxy Weak Lensing. J AIYUL Y OO AND D AVID W EINBERG D EPARTMENT OF A STRONOMY , T HE O HIO S TATE U NIVERSITY. Center for Cosmology and Astro-Particle Physics Great Lakes Cosmology Workshop VIII, June, 1-3, 2007.

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Center for Cosmology and Astro-Particle Physics

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  1. Probing Dark Energy with Cluster-Galaxy Weak Lensing JAIYUL YOO AND DAVID WEINBERG DEPARTMENTOF ASTRONOMY, THE OHIO STATE UNIVERSITY Center for Cosmology and Astro-Particle Physics Great Lakes Cosmology Workshop VIII, June, 1-3, 2007

  2. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Cluster-GalaxyWeak Lensing • cluster-matter cross correlation (profile & bias) • stacking rank-ordered clusters: monotonic relation of the mean mass-observable no mass estimate of individual clusters no accurate relation to true cluster mass • weak lensing of the stacked sample of clusters

  3. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Why Robust? • stacked sample

  4. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Why Robust? • stacked sample

  5. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Why Robust? • stacked sample ≅ mass-ordered clusters

  6. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Why Robust? • stacked sample ≅ mass-ordered clusters • works for arbitrary relation and bias

  7. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Cosmological Probe? • stacked sample is set by cosmology! • growth factor, volume, halo mass function (given number of clusters) • constituent clusters are also different!

  8. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Prediction and Observable critical surface density angular diameter distance

  9. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Why Better? • clusters provide high S/N (vs cosmic shear) • spherical symmetric dark matter halo • apparent lens center (central cD galaxies) • stacking increases S/N → high redshift clusters • tangential shear profile • clusters provide high S/N (vs cosmic shear) • spherical symmetric dark matter halo • apparent lens center (central cD galaxies) • stacking increases S/N → high redshift clusters • tangential shear profile

  10. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Parameter Sensitivity

  11. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Parameter Sensitivity

  12. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Dark Energy Constraint • DES type survey • 1,2,3 σ contours • no CMB priors • flat universe

  13. PROBING DARK ENERGY WITHCLUSTER-GALAXY WEAK LENSING Conclusion and Prospects • novel method of cluster-galaxy weak lensing works for arbitrary mass-observables robust to scatter and bias • readily applicable, strong constraints • application to OSU Dark Energy Survey with Large Binocular Telescope (LBT) Stay “fine” tuned!!!

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