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?.
Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.
Statistical lensing in COSMOS
Ludovic Van Waerbeke
Department of Physics and Astronomy
University of British Columbia
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
Contaldi et al. 2004
LVW et al.
COSMOS should reach ~ same accuracy with two major differences:
-followups. In particular photoz enables lenses selection, 3D lensing, etc…
-depth enables high order statistics despite small FOV.
redshift distributions based on the Hubble deep fields
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
M~4.4x1011 Mo h70-1