Image simulations the UVBrick:

Filipe Batoni Abdalla

and

Weak Lensing: Cosmic Shear Background sources Dark matter halos

Observer

     

Statistical measure of shear pattern, ~1% distortion Radial distances depend on geometry of Universe Foreground mass distribution depends on growth of structure

Neutral at z=1000

Ionized at z<6 COBE

space weak lensing shear

ground

Space: small and stable PSF ! larger number of resolved galaxies ! reduced systematics

Typical cosmic shear is ~ 1%, and must be measured with high accuracy

Ciardi et al.

nmax Refregier 2003, Refregier & Bacon 2003, Massey & Refregier 2005

Complete orthogonal basis functions Capture all shape information of an object

!n,m

8 6 4 m 2 0

Simple and analytic form for convolution and shear

-2

Adapted to cosmic shear

-4 -6 -8

0

1 2 3

4

n

5

6 7 8

Refregier 2003, Refregier & Bacon 2003, Massey & Refregier 2005

Complete orthogonal basis functions Capture all shape information of an object Simple and analytic form for convolution and shear Adapted to cosmic shear

Apologies to the Black belt radio astronomers in the room if this is too simple

•  Simulate a grid of points • 

•  • 

with DFT’s -> fill MS Simulate the same points with the UVBrick -> subtract the UV values from MS. Image difference. sigma:3.02036e-05

•  1200x1200 at 120'

•  Simulate a grid of points • 

•  • 

with DFT’s -> fill MS Simulate the same points 0.5 pix offset with the UVBrick -> subtract the UV values from MS. Image difference. sigma:0.000555845

•  1200x1200 at 120'

Size of support convolution is important, if smaller than 4 we get ghosts

s-cubed.physics.ox.ac.uk

Design requirements of the SemiEmpirical eXtragalactic (SEX) simulation:

Radion version of this plot!!!

Image simulations and the UVBrick - GitHub

Oct 7, 2009 - Empirical. eXtragalactic (SEX) simulation: s-c ube d.physic. s.o. x.a c.uk. Size of support convolution is important, if smaller than 4 we get ghosts ...

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