Detecting Baryon Acoustic Oscillations in Dark Matter from Kinematic Weak Lensing Surveys. (arXiv:1901.06326v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ding_Z/0/1/0/all/0/1">Zhejie Ding</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seo_H/0/1/0/all/0/1">Hee-Jong Seo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huff_E/0/1/0/all/0/1">Eric Huff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saito_S/0/1/0/all/0/1">Shun Saito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clowe_D/0/1/0/all/0/1">Douglas Clowe</a>
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 allow a detection of the BAO scale bias between galaxies
and dark matter.
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 allow a detection of the BAO scale bias between galaxies
and dark matter.
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