# Detecting Baryon Acoustic Oscillations in Dark Matter from Kinematic Weak Lensing Surveys

## TL;DR

This paper explores the potential of future kinematic weak lensing surveys to detect and measure Baryon Acoustic Oscillations in dark matter with high precision, outperforming traditional photometric surveys.

## Contribution

It demonstrates that spectroscopic kinematic weak lensing surveys can effectively detect BAO features in dark matter and measure the BAO scale with 2-4 ext{%} precision, surpassing photometric methods.

## Key findings

- Stage IV KWL surveys can detect BAO at 3-σ significance.
- BAO scale can be measured with 4 ext{%} precision in such surveys.
- Cross-correlation with galaxy surveys can improve BAO detection and constrain bias.

## Abstract

We investigate the feasibility of extracting Baryon Acoustic Oscillations (BAO) from cosmic shear tomography. We particularly focus on the BAO scale precision that can be achieved by future spectroscopy-based, kinematic weak lensing (KWL) surveys \citep[e.g.,][]{Huff13} in comparison to the traditional photometry-based weak lensing surveys. We simulate cosmic shear tomography data of such surveys with a few simple assumptions to focus on the BAO information, extract the spacial power spectrum, and constrain the recovered BAO feature. Due to the small shape noise and the shape of the lensing kernel, we find that a Dark Energy Task Force Stage IV version of such KWL survey can detect the BAO feature in dark matter by $3$-$\sigma$ and measure the BAO scale at the precision level of 4\% while it will be difficult to detect the feature in photometry-based weak lensing surveys. With a more optimistic assumption, a KWL-Stage IV could achieve a $\sim 2\%$ BAO scale measurement with $4.9$-$\sigma$ confidence. A built-in spectroscopic galaxy survey within such KWL survey will allow cross-correlation between galaxies and cosmic shear, which will tighten the constraint beyond the lower limit we present in this paper and therefore possibly allow a detection of the BAO scale bias between galaxies and dark matter.