Computer Science
Scientific paper
Jun 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004phdt.........8j&link_type=abstract
Thesis (PhD). THE UNIVERSITY OF CHICAGO, Source DAI-B 64/12, p. 6120, Jun 2004, 71 pages.
Computer Science
Scientific paper
We discuss the galaxy-galaxy-mass three-point correlation function and show how to measure it with weak gravitational lensing. The method entails choosing pairs of foreground lens galaxies, rotating them to the common coordinate system defined by the axis connecting them and then constructing a mean shear map by averaging the ellipticities of background source galaxies for a large number of foreground pairs. An average mass map can be reconstructed from this shear map and this will represent the average mass distribution around pairs of galaxies. We show how this mass map is related to the projected galaxy-galaxy-mass three-point correlation function. Using a large N-body dark matter simulation populated with galaxies using the Halo Occupation Distribution (HOD) bias prescription, we compute these correlation functions, mass maps, and shear maps. The resultant mass maps are distinctly bimodal, tracing the galaxy centers and remaining anisotropic up to scales much larger than the galaxy separation. At larger scales, the shear is approximately tangential about the center of the pair but with azimuthal variation in amplitude. We estimate the signal-to-noise ratio of the reconstructed mass maps for a survey of similar depth to the Sloan Digital Sky Survey (SDSS) and conclude that the galaxy-galaxy-mass three- point function should be measurable with the current SDSS weak lensing data. Measurements of this three-point function, along with galaxy-galaxy lensing and galaxy auto-correlation functions, will provide new constraints on galaxy bias models. The anisotropic shear profile around close pairs of galaxies is a prediction of cold dark matter models and may be difficult to reconcile with alternative theories of gravity without dark matter.
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