Statistical lensing in COSMOS
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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. Weak lensing two-points statistics: What is measured?.

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Ludovic Van Waerbeke Department of Physics and Astronomy University of British Columbia

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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


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


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.


redshift distributions based on the Hubble deep fields

25.<i<27.

Zphot~1.4


Cycle 12 area Polygon masks (ds9 format) are available


PSF anisotropy pattern averaged over cycle 12 chips


Preliminary E and B modes aperture mass


LCDM model with s8=0.8 and zS~1.4


~30 stars per chip


Needs image reprocessing with smaller pixel size?


Star-gal shear aperture correlation


Star-gal shear correlation function


Strong lensing with R. Gavazzi (OMP, Toulouse)


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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