Ludovic Van Waerbeke Department of Physics and Astronomy University of British Columbia
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Transcript of Ludovic Van Waerbeke Department of Physics and Astronomy University of British Columbia
Ludovic Van WaerbekeDepartment of Physics and Astronomy
University of British Columbia
A (very short) introduction to E/B modesMeasurement and high order statistics
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Convergence (or projected mass) power spectrum:
Aperture mass (Map) variance at scale c :
Top-hat shear variance at scale c:
Shear correlation function at separation :
Cosmic Shear two-points Statistics and mass Power Spectrum
ttγγ
rrγγ
Crittenden et al. 2000, Pen et al. 2002:
E and B mode decomposition of the two points statistics
Top-hat variance, which can be decomposed into E and B modes using
Aperture mass variance
How to get properly normalised E/B xi and top-hat variance?Use the aperture mass to fix your unknown B mode constant.
Useful formula in Schneider, LVW & Mellier, 2002:
Simulated 3x3 degrees reconstructed convergenceSimulated 3x3 degrees reconstructed convergence
mapmap
Convergence PDFConvergence PDF
ExpectedExpectedconstraintsconstraints
S3=<K3>/<K2>2
~40 zs-
1.3
VIRMOS-Descart: high order statistics(LVW, Bernardeau, Mellier, 1999)
Simulated 3x3 degrees shearSimulated 3x3 degrees shear
mapmap3-pts function pattern3-pts function pattern
d1212
33
21
High order statistics: shear 3-pts function (Bernardeau et al. 2003)
E+B and E-B for the two-points and three-points functions. Dotted lineIs TCDM and dashed line is OCDM.
Cosmic variance with the OCDM:
Uncorrected star (solid lines) and corrected galaxies (dotted) two and threePoints functions.
(Pen et al., 2003)
Aperture mass skewness from three point function integration
(Jarvis et al., 2004)
CTIOVIRMOS-Descart
+DEEP+COSMOS
More to come…soon!
Virmos-Descart
Wide CFHTLS