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Statistical Lensing in COSMOS: Weak Lensing Two-Points Statistics

Learn about weak lensing two-points statistics: mass power spectrum, power spectrum slope, density parameter, source redshift, and more in the COSMOS project. Explore follow-ups, photoz for lenses selection, 3D lensing, high order statistics with small FOV, and more.

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Statistical Lensing in COSMOS: Weak Lensing Two-Points Statistics

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  1. Statistical lensing in COSMOS Ludovic Van Waerbeke Department of Physics and Astronomy University of British Columbia With: F. Bernardeau (CEA) Y. Mellier (IAP) E. Semboloni (IAP) & the COSMOS team

  2. Weak lensing two-points statistics: What is measured? <g2>~0.01 s82 W1.6 zs1.4 q-(n+2)/2 • Mass power spectrum normalisation • Slope of the power spectrum • Mean density parameter • Redshift of the sources Contaldi et al. 2004

  3. VIRMOS I~24 Z~0.9 LVW et al. COSMOS should reach ~ same accuracy with two major differences: -followups. In particular photoz enables lenses selection, 3D lensing, etc… -morphology -depth enables high order statistics despite small FOV.

  4. redshift distributions based on the Hubble deep fields 25.<i<27. Zphot~1.4

  5. Cycle 12 area Polygon masks (ds9 format) are available

  6. PSF anisotropy pattern averaged over cycle 12 chips

  7. Preliminary E and B modes aperture mass

  8. LCDM model with s8=0.8 and zS~1.4

  9. ~30 stars per chip

  10. Needs image reprocessing with smaller pixel size?

  11. Star-gal shear aperture correlation

  12. Star-gal shear correlation function

  13. Strong lensing with R. Gavazzi (OMP, Toulouse)

  14. Inverse pixel mapping into the source plane Singular IS Zlens~0.4 Zsource~3 Re=1.58” M~4.4x1011 Mo h70-1

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