EPJ Web Conf.
Volume 168, 2018Joint International Conference of ICGAC-XIII and IK-15 on Gravitation, Astrophysics and Cosmology
|Number of page(s)||8|
|Published online||09 January 2018|
Accelerated cosmological expansion without tension in the Hubble parameter*
Fast evolution of the Hubble parameter H(z)
614 Yeongsil-Gwan, Department of Physics and Astronomy, Sejong University, 143-747 Seoul, South Korea
** e-mail: email@example.com
Published online: 9 January 2018
The H0-tension problem poses a confrontation of dark energy driving latetime cosmological expansion measured by the Hubble parameter H(z) over an extended range of redshifts z. Distinct values H0 ≃ 73 km s–1 Mpcs–1 and H0 ≃ 68 km s–1 Mpcs–1 obtain from surveys of the Local Universe and, respectively, ΛCBM analysis of the CMB. These are representative of accelerated expansion with H′(0) ≃ 0 by and, respectively, H′(0) > 0 in ΛCDM, where is a fundamental frequency of the cosmological horizon in a Friedmann-Robertson-Walker universe with deceleration parameter q(z) = -1 + (1+z)H–1 H′(z). Explicit solution H(z) = H0 and, respectively, H(z) = H0 are here compared with recent data on H(z) over 0 ≲ z ≲ 2.The first is found to be free of tension with H0 from local surveys, while the latter is disfavored at 2:7σ A further confrontation obtains in galaxy dynamics by a finite sensitivity of inertia to background cosmology in weak gravity, putting an upper bound of m ≲ 10–30 eV on the mass of dark matter. A C0 onset to weak gravity at the de Sitter scale of acceleration adS = cH(z), where c denotes the velocity of light, can be seen in galaxy rotation curves covering 0 ≲ z ≲ 2 Weak gravity in galaxy dynamics hereby provides a proxy for cosmological evolution.
© The Authors, published by EDP Sciences, 2018
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