Exploring neutrino mass and mass hierarchy in interacting dark energy models. (arXiv:1903.08848v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Feng_L/0/1/0/all/0/1">Lu Feng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_H/0/1/0/all/0/1">Hai-Li Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_J/0/1/0/all/0/1">Jing-Fei Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_X/0/1/0/all/0/1">Xin Zhang</a>
We investigate how the dark energy properties impact the constraints on the
total neutrino mass in interacting dark energy (IDE) models. In this study, we
focus on two typical interacting dynamical dark energy models, i.e., the
I$w$CDM model and the IHDE model. To avoid the large-scale instability problem
in IDE models, we apply the parameterized post-Friedmann (PPF) approach to
calculate the perturbation of dark energy. We employ the Planck 2015 CMB
temperature and polarization data, combined with low-redshift measurements on
baryon acoustic oscillation distance scales, type Ia supernovae, and the Hubble
constant, to constrain the cosmological parameters. We find that the dark
energy properties could influence the constraint limits on the total neutrinos
mass. Once dynamical dark energy is considered in the IDE models, the upper
bounds of $sum m_nu$ will be changed. By considering the values of
$chi^2_{rm min}$, we find that in these IDE models the NH case is slightly
preferred over the IH case; for example, the difference of $Deltachi^2=2.720$
is given in the IHDE+$sum m_nu$ model. In addition, we also find that in the
I$w$CDM+$sum m_nu$ model $beta=0$ is consistent with current observational
data inside the 1$sigma$ range, and in the IHDE+$sum m_nu$ model $beta>0$
is favored at more than the 2$sigma$ level.
We investigate how the dark energy properties impact the constraints on the
total neutrino mass in interacting dark energy (IDE) models. In this study, we
focus on two typical interacting dynamical dark energy models, i.e., the
I$w$CDM model and the IHDE model. To avoid the large-scale instability problem
in IDE models, we apply the parameterized post-Friedmann (PPF) approach to
calculate the perturbation of dark energy. We employ the Planck 2015 CMB
temperature and polarization data, combined with low-redshift measurements on
baryon acoustic oscillation distance scales, type Ia supernovae, and the Hubble
constant, to constrain the cosmological parameters. We find that the dark
energy properties could influence the constraint limits on the total neutrinos
mass. Once dynamical dark energy is considered in the IDE models, the upper
bounds of $sum m_nu$ will be changed. By considering the values of
$chi^2_{rm min}$, we find that in these IDE models the NH case is slightly
preferred over the IH case; for example, the difference of $Deltachi^2=2.720$
is given in the IHDE+$sum m_nu$ model. In addition, we also find that in the
I$w$CDM+$sum m_nu$ model $beta=0$ is consistent with current observational
data inside the 1$sigma$ range, and in the IHDE+$sum m_nu$ model $beta>0$
is favored at more than the 2$sigma$ level.
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