How to measure galaxy-galaxy-galaxy-lensing with higher precision and accuracy. (arXiv:1909.06190v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Linke_L/0/1/0/all/0/1">Laila Linke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simon_P/0/1/0/all/0/1">Patrick Simon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_P/0/1/0/all/0/1">Peter Schneider</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hilbert_S/0/1/0/all/0/1">Stefan Hilbert</a>

Galaxy-galaxy-galaxy lensing (G3L) is a powerful tool for constraining the
three-point correlation between the galaxy and the matter field and thereby
models of galaxy evolution. We propose three improvements to current
measurements of G3L, designed to improve the precision and the accuracy by
using the galaxies’ redshifts and removing biases of the estimator. We further
show how to account for lens galaxy magnification by the cosmic large-scale
structure and how to convert the G3L signal from angular to physical scales.
The improvements are tested on simple mock data and simulated data based on the
Millennium Run with an implemented semi-analytic model of galaxies. Our
improvements increase the signal-to-noise ratio by on average $35~%$ at
angular scales between $0.1’$ and $10’$ and physical scales between $0.02$ and
$2 , h^{-1},textrm{Mpc}$. They also remove the bias of the G3L estimator at
angular scales below $1’$, which was originally up to $40,%$. The signal due
to lens magnification is approximately $10,%$ of the total signal.

Galaxy-galaxy-galaxy lensing (G3L) is a powerful tool for constraining the
three-point correlation between the galaxy and the matter field and thereby
models of galaxy evolution. We propose three improvements to current
measurements of G3L, designed to improve the precision and the accuracy by
using the galaxies’ redshifts and removing biases of the estimator. We further
show how to account for lens galaxy magnification by the cosmic large-scale
structure and how to convert the G3L signal from angular to physical scales.
The improvements are tested on simple mock data and simulated data based on the
Millennium Run with an implemented semi-analytic model of galaxies. Our
improvements increase the signal-to-noise ratio by on average $35~%$ at
angular scales between $0.1’$ and $10’$ and physical scales between $0.02$ and
$2 , h^{-1},textrm{Mpc}$. They also remove the bias of the G3L estimator at
angular scales below $1’$, which was originally up to $40,%$. The signal due
to lens magnification is approximately $10,%$ of the total signal.

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