Baryon acoustic oscillation, Hubble parameter, and angular size measurement constraints on the Hubble constant, dark energy dynamics, and spatial curvature. (arXiv:1902.03196v1 [astro-ph.CO])

Baryon acoustic oscillation, Hubble parameter, and angular size measurement constraints on the Hubble constant, dark energy dynamics, and spatial curvature. (arXiv:1902.03196v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ryan_J/0/1/0/all/0/1">Joseph Ryan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Yun Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ratra_B/0/1/0/all/0/1">Bharat Ratra</a>

In this paper we use all available baryon acoustic oscillation and Hubble
parameter data to constrain six dark energy cosmological models, both spatially
flat and non-flat. These data mildly favor (at 1.3-1.4$sigma$) closed spatial
hypersurfaces in the dynamical dark energy models, and favor dark energy
dynamics (at $>1$-2$sigma$, depending on the model) over a cosmological
constant $Lambda$. They also favor, at 2.2$sigma$ to $3.5sigma$, depending
on the model, a lower Hubble constant than what is measured from the local
expansion rate by Riess et al. (2018).

In this paper we use all available baryon acoustic oscillation and Hubble
parameter data to constrain six dark energy cosmological models, both spatially
flat and non-flat. These data mildly favor (at 1.3-1.4$sigma$) closed spatial
hypersurfaces in the dynamical dark energy models, and favor dark energy
dynamics (at $>1$-2$sigma$, depending on the model) over a cosmological
constant $Lambda$. They also favor, at 2.2$sigma$ to $3.5sigma$, depending
on the model, a lower Hubble constant than what is measured from the local
expansion rate by Riess et al. (2018).

http://arxiv.org/icons/sfx.gif