On The Upper Bound of Neutrino Masses from Combined Cosmological Observations and Particle Physics Experiments. (arXiv:1811.02578v1 [astro-ph.CO])

<a href="http://arxiv.org/find/astro-ph/1/au:+Loureiro_A/0/1/0/all/0/1">Arthur Loureiro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cuceu_A/0/1/0/all/0/1">Andrei Cuceu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abdalla_F/0/1/0/all/0/1">Filipe B. Abdalla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moraes_B/0/1/0/all/0/1">Bruno Moraes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Whiteway_L/0/1/0/all/0/1">Lorne Whiteway</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McLeod_M/0/1/0/all/0/1">Michael McLeod</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balan_S/0/1/0/all/0/1">Sreekumar T. Balan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lahav_O/0/1/0/all/0/1">Ofer Lahav</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benoit_Levy_A/0/1/0/all/0/1">Aurélien Benoit-Lévy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manera_M/0/1/0/all/0/1">Marc Manera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rollins_R/0/1/0/all/0/1">Richard P. Rollins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xavier_H/0/1/0/all/0/1">Henrique S. Xavier</a>

We investigate the impact of prior models on the upper bound of the sum of

neutrino masses, $sum m_{nu}$. We use data from Large Scale Structure of

galaxies, Cosmic Microwave Background, Type Ia SuperNovae, and Big Bang

Nucleosynthesis. We probe physically motivated neutrino mass models (respecting

oscillation experiment constraints) and compare them to constraints using

standard cosmological approximations. The former give a consistent upper bound

of $sum m_{nu} lesssim 0.26$ eV ($95%$ CI) and yields a strong competitive

upper bound for the lightest neutrino mass species, $m_0^{nu} < 0.086$ eV
($95%$ CI). By contrast one of the approximations, which is somewhat
inconsistent with oscillation experiments, yields an upper bound of $sum
m_{nu} lesssim 0.15$ eV ($95%$ CI), which differs substantially from the
former upper bound. We, therefore, argue that cosmological neutrino mass and
hierarchy determination should be pursued using physically motivated models
since approximations might lead to incorrect and nonphysical upper bounds.

We investigate the impact of prior models on the upper bound of the sum of

neutrino masses, $sum m_{nu}$. We use data from Large Scale Structure of

galaxies, Cosmic Microwave Background, Type Ia SuperNovae, and Big Bang

Nucleosynthesis. We probe physically motivated neutrino mass models (respecting

oscillation experiment constraints) and compare them to constraints using

standard cosmological approximations. The former give a consistent upper bound

of $sum m_{nu} lesssim 0.26$ eV ($95%$ CI) and yields a strong competitive

upper bound for the lightest neutrino mass species, $m_0^{nu} < 0.086$ eV

($95%$ CI). By contrast one of the approximations, which is somewhat

inconsistent with oscillation experiments, yields an upper bound of $sum

m_{nu} lesssim 0.15$ eV ($95%$ CI), which differs substantially from the

former upper bound. We, therefore, argue that cosmological neutrino mass and

hierarchy determination should be pursued using physically motivated models

since approximations might lead to incorrect and nonphysical upper bounds.

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