Determining the Hubble Constant without the Sound Horizon: Measurements from Galaxy Surveys. (arXiv:2008.08084v3 [astro-ph.CO] UPDATED)

Determining the Hubble Constant without the Sound Horizon: Measurements from Galaxy Surveys. (arXiv:2008.08084v3 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Philcox_O/0/1/0/all/0/1">Oliver H. E. Philcox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sherwin_B/0/1/0/all/0/1">Blake D. Sherwin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Farren_G/0/1/0/all/0/1">Gerrit S. Farren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baxter_E/0/1/0/all/0/1">Eric J. Baxter</a>

Two sources of geometric information are encoded in the galaxy power
spectrum: the sound horizon at recombination and the horizon at
matter-radiation equality. Analyzing the BOSS DR12 galaxy power spectra using
perturbation theory with $Omega_m$ priors from Pantheon supernovae but no
priors on $Omega_b$, we obtain constraints on $H_0$ from the second scale,
finding $H_0 =
65.1^{+3.0}_{-5.4},mathrm{km},mathrm{s}^{-1}mathrm{Mpc}^{-1}$; this
differs from the best-fit of SH0ES at 95% confidence. Similar results are
obtained if $Omega_m$ is constrained from uncalibrated BAO: $H_0 =
65.6^{+3.4}_{-5.5},mathrm{km},mathrm{s}^{-1}mathrm{Mpc}^{-1}$. Adding the
analogous lensing results from Baxter & Sherwin 2020, the posterior shifts to
$70.6^{+3.7}_{-5.0},mathrm{km},mathrm{s}^{-1}mathrm{Mpc}^{-1}$. Using mock
data, Fisher analyses, and scale-cuts, we demonstrate that our constraints do
not receive significant information from the sound horizon scale. Since many
models resolve the $H_0$ controversy by adding new physics to alter the sound
horizon, our measurements are a consistency test for standard cosmology before
recombination. A simple forecast indicates that such constraints could reach
$sigma_{H_0} simeq 1.6,mathrm{km},mathrm{s}^{-1}mathrm{Mpc}^{-1}$ in the
era of Euclid.

Two sources of geometric information are encoded in the galaxy power
spectrum: the sound horizon at recombination and the horizon at
matter-radiation equality. Analyzing the BOSS DR12 galaxy power spectra using
perturbation theory with $Omega_m$ priors from Pantheon supernovae but no
priors on $Omega_b$, we obtain constraints on $H_0$ from the second scale,
finding $H_0 =
65.1^{+3.0}_{-5.4},mathrm{km},mathrm{s}^{-1}mathrm{Mpc}^{-1}$; this
differs from the best-fit of SH0ES at 95% confidence. Similar results are
obtained if $Omega_m$ is constrained from uncalibrated BAO: $H_0 =
65.6^{+3.4}_{-5.5},mathrm{km},mathrm{s}^{-1}mathrm{Mpc}^{-1}$. Adding the
analogous lensing results from Baxter & Sherwin 2020, the posterior shifts to
$70.6^{+3.7}_{-5.0},mathrm{km},mathrm{s}^{-1}mathrm{Mpc}^{-1}$. Using mock
data, Fisher analyses, and scale-cuts, we demonstrate that our constraints do
not receive significant information from the sound horizon scale. Since many
models resolve the $H_0$ controversy by adding new physics to alter the sound
horizon, our measurements are a consistency test for standard cosmology before
recombination. A simple forecast indicates that such constraints could reach
$sigma_{H_0} simeq 1.6,mathrm{km},mathrm{s}^{-1}mathrm{Mpc}^{-1}$ in the
era of Euclid.

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