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Accelerating the 2-point and 3-point galaxy correlation functions using Fourier transforms

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arxiv 1506.04746 v2 pith:BZSSUZXE submitted 2015-06-15 astro-ph.CO

classification astro-ph.CO
keywords correlationusedfourierfunctionspairpointtransformsaccelerate
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Though Fourier Transforms (FTs) are a common technique for finding correlation functions, they are not typically used in computations of the anisotropy of the two-point correlation function (2PCF) about the line of sight in wide-angle surveys because the line-of-sight direction is not constant on the Cartesian grid. Here we show how FTs can be used to compute the multipole moments of the anisotropic 2PCF. We also show how FTs can be used to accelerate the 3PCF algorithm of Slepian & Eisenstein (2015). In both cases, these FT methods allow one to avoid the computational cost of pair counting, which scales as the square of the number density of objects in the survey. With the upcoming large datasets of DESI, Euclid, and LSST, FT techniques will therefore offer an important complement to simple pair or triplet counts.

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Cited by 3 Pith papers

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    astro-ph.CO 2026-07 conditional novelty 6.0 of 10

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    astro-ph.CO 2025-08 conditional novelty 6.0 of 10

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  3. Modeling and measuring the anisotropic halo 3-point correlation function: a coordinated study

    astro-ph.CO 2024-08 conditional novelty 6.0 of 10

    Novel implementation of anisotropic 3PCF model and estimator tested on 298 halo catalogs shows degeneracy breaking between f and b1 in 3PCF-only analysis but limited added value in joint 2PCF+3PCF due to tree-level mo...

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