Constraints on a special running vacuum model. (arXiv:2001.05092v1 [astro-ph.CO])

<a href="http://arxiv.org/find/astro-ph/1/au:+Geng_C/0/1/0/all/0/1">Chao-Qiang Geng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_C/0/1/0/all/0/1">Chung-Chi Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yin_L/0/1/0/all/0/1">Lu Yin</a>

We study a special running vacuum model (RVM) with $Lambda = 3 alpha

H^2+3beta H_0^4 H^{-2}+Lambda_0$, where $alpha$, $beta$ and $Lambda_0$ are

the model parameters and $H$ is the Hubble one. This RVM has non-analytic

background solutions for the energy densities of matter and radiation, which

can only be evaluated numerically. From the analysis of the CMB power spectrum

and baryon acoustic oscillation along with the prior of $alpha>0$ to avoid

having a negative dark energy density, we find that $alpha<2.83times 10^{-4}$
and $beta=(-0.2^{+3.9}_{-4.5})times 10^{-4}$ (95$%$ C.L.). We show that the
RVM fits the cosmological data comparably to the $Lambda$CDM. In addition, we
relate the fluctuation amplitude $sigma_8$ to the neutrino mass sum $Sigma
m_nu$.

We study a special running vacuum model (RVM) with $Lambda = 3 alpha

H^2+3beta H_0^4 H^{-2}+Lambda_0$, where $alpha$, $beta$ and $Lambda_0$ are

the model parameters and $H$ is the Hubble one. This RVM has non-analytic

background solutions for the energy densities of matter and radiation, which

can only be evaluated numerically. From the analysis of the CMB power spectrum

and baryon acoustic oscillation along with the prior of $alpha>0$ to avoid

having a negative dark energy density, we find that $alpha<2.83times 10^{-4}$

and $beta=(-0.2^{+3.9}_{-4.5})times 10^{-4}$ (95$%$ C.L.). We show that the

RVM fits the cosmological data comparably to the $Lambda$CDM. In addition, we

relate the fluctuation amplitude $sigma_8$ to the neutrino mass sum $Sigma

m_nu$.

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