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• W3049020199 abstract "As briefly discussed at the start of Chap. 9, the main weakness of cosmological limits on neutrino masses is their (in)stability against a larger parameter space, particularly when the extended parameters are strongly correlated/degenerate with (M_{nu }). So far, we focused on the effect other parameters have on the limits on (M_{nu }) (e.g. [1]). Of course, this problem can be in some sense reversed: if a particular parameter X is strongly correlated with (M_{nu }), the values inferred for X might be sensitive to the assumptions I make when introducing (M_{nu }) into the picture, or to the very fact that I introduced (M_{nu }) in first place. Recall, in fact, that in the baseline (Lambda )CDM model, (M_{nu }) is not a free parameter, but is fixed to (M_{nu }=0.06,mathrm{eV}), the minimum value allowed by oscillations data." @default.
• W3049020199 created "2020-08-21" @default.
• W3049020199 creator A5048780307 @default.
• W3049020199 date "2020-01-01" @default.
• W3049020199 modified "2023-09-25" @default.
• W3049020199 title "Massive Neutrinos Meet Inflation" @default.
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• W3049020199 doi "https://doi.org/10.1007/978-3-030-53502-5_10" @default.
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