
Impacts of dark energy on constraining neutrino mass after Planck 2018
Ming Zhang,Jing-Fei Zhang,Xin Zhang
Communications in Theoretical Physics ›› 2020, Vol. 72 ›› Issue (12) : 125402.
Impacts of dark energy on constraining neutrino mass after Planck 2018
Considering the mass splittings of three active neutrinos, we investigate how the properties of dark energy affect the cosmological constraints on the total neutrino mass
neutrino mass / mass hierarchies of neutrinos / dark energy / cosmological constraints / Planck 2018 {{custom_keyword}} /
• | The ΛCDM+ |
• | The wCDM+ |
• | The CPL+ |
• | The HDE+ |
• | The CMB data: We employ the CMB likelihood including the TT, TE, and EE spectra at ℓ ≥ 30, the low-ℓ temperature Commander likelihood, and the low-ℓ SimAll EE likelihood, from the Planck 2018 release [12]. |
• | The BAO data: We employ the measurements of the BAO signals from different galaxy surveys, including the DR7 Main Galaxy Sample at the effective redshift of zeff = 0.15 [72], the six-degree-field Galaxy Survey (6dFGS) at zeff = 0.106 [73], and the latest BOSS data release 12 (DR12) in three redshift slices of zeff = 0.38, 0.51, and 0.61 [74]. |
• | The SNe data: We use the latest SNe data given the Pantheon Sample [75], which contains 1048 SNe data in the redshift range of 0.01 < z < 2.3. |
• | The Hubble constant: We use the result of the direct measurement of the Hubble constant, with the result of H0 = 74.03 ± 1.42 km s−1 Mpc−1, given by Riess et al [68]. |
Figure 1. Left: the one-dimensional marginalized posterior distributions for |
Figure 2. The two-dimensional marginalized contours (1σ and 2σ) in the |
Table 1. Fitting results of the cosmological parameters in the ΛCDM+ |
Data | Planck+BAO+SNe | Planck+BAO+SNe+H0 | ||||
---|---|---|---|---|---|---|
Mass ordering | DH | NH | IH | DH | NH | IH |
H0 (km s−1 Mpc−1) | 67.75 ± 0.49 | 67.48 ± 0.47 | 67.26 ± 0.45 | 68.40 ± 0.44 | 68.11 ± 0.43 | 67.88 ± 0.43 |
Ωm | 0.3097 ± 0.0063 | 0.3126 ± 0.0063 | 0.3150 ± 0.0060 | 0.3015 ± 0.0056 | 0.3044 ± 0.0056 | 0.3069 ± 0.0056 |
σ8 | ||||||
<0.156 | <0.185 | <0.082 | <0.125 | <0.160 | ||
| ||||||
χ2 | 3805.133 | 3807.205 | 3809.012 | 3821.466 | 3825.557 | 3828.810 |
Figure 3. The two-dimensional marginalized contours (1σ and 2σ) in the w0-wa plane for three neutrino mass hierarchy cases, i.e. the DH case, the NH case, and the IH case, by using Planck+BAO+SNe and Planck+BAO+SNe+H0 data combinations in the CPL+ |
Table 2. Fitting results of the cosmological parameters in the wCDM+ |
Data | Planck+BAO+SNe | Planck+BAO+SNe+H0 | ||||
---|---|---|---|---|---|---|
Mass ordering | DH | NH | IH | DH | NH | IH |
w | −1.029 ± 0.035 | −1.042 ± 0.035 | −1.051 ± 0.035 | −1.078 ± 0.033 | −1.090 ± 0.033 | |
H0 (km s−1 Mpc−1) | 68.27 ± 0.83 | 68.23 ± 0.83 | 68.21 ± 0.81 | 69.79 ± 0.73 | 69.74 ± 0.73 | 69.70 ± 0.74 |
Ωm | 0.3064 ± 0.0078 | 0.3076 ± 0.0078 | 0.3084 ± 0.0076 | 0.2932 ± 0.0066 | 0.2945 ± 0.0066 | 0.2954 ± 0.0067 |
σ8 | 0.819 ± 0.015 | 0.805 ± 0.014 | 0.820 ± 0.014 | |||
<0.155 | <0.195 | <0.220 | <0.145 | <0.183 | <0.210 | |
| ||||||
χ2 | 3805.053 | 3806.381 | 3807.724 | 3817.072 | 3818.757 | 3819.912 |
Table 3. Fitting results of the cosmological parameters in the CPL+ |
Data | Planck+BAO+SNe | Planck+BAO+SNe+H0 | ||||
---|---|---|---|---|---|---|
Mass ordering | DH | NH | IH | DH | NH | IH |
w0 | −0.945 ± 0.087 | −0.933 ± 0.089 | −0.923 ± 0.089 | −1.003 ± 0.082 | −0.988 ± 0.086 | −0.978 ± 0.088 |
wa | ||||||
H0 (km s−1 Mpc−1) | 68.22 ± 0.83 | 68.19 ± 0.83 | 68.14 ± 0.84 | 69.78 ± 0.73 | 69.71 ± 0.74 | 69.69 ± 0.73 |
Ωm | 0.3087 ± 0.0082 | 0.3102 ± 0.0083 | 0.3113 ± 0.0083 | 0.2948 ± 0.0068 | 0.2965 ± 0.0070 | 0.2976 ± 0.0069 |
σ8 | ||||||
<0.247 | <0.290 | <0.305 | <0.216 | <0.255 | <0.281 | |
| ||||||
χ2 | 3804.644 | 3805.938 | 3806.531 | 3816.716 | 3817.806 | 3818.809 |
Table 4. Fitting results of the cosmological parameters in the HDE+ |
Data | Planck+BAO+SNe | Planck+BAO+SNe+H0 | ||||
---|---|---|---|---|---|---|
Mass ordering | DH | NH | IH | DH | NH | IH |
c | 0.595 ± 0.024 | |||||
H0 (km s−1 Mpc−1) | 67.85 ± 0.81 | 67.79 ± 0.79 | 67.74 ± 0.80 | 69.38 ± 0.72 | 69.33 ± 0.71 | 69.27 ± 0.71 |
Ωm | 0.3061 ± 0.0077 | 0.3077 ± 0.0076 | 0.3087 ± 0.0076 | 0.2927 ± 0.0065 | 0.2939 ± 0.0065 | 0.2951 ± 0.0065 |
σ8 | 0.797 ± 0.013 | 0.789 ± 0.013 | 0.783 ± 0.013 | 0.811 ± 0.013 | 0.803 ± 0.012 | 0.796 ± 0.12 |
<0.080 | <0.129 | <0.163 | <0.075 | <0.123 | <0.159 | |
| ||||||
χ2 | 3822.977 | 3828.219 | 3830.980 | 3838.467 | 3845.127 | 3845.289 |
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We thank Hai-Li Li, Jing-Zhao Qi, and Yun-He Li for helpful discussions. This work was supported by the National Natural Science Foundation of China (Grant Nos. 11975072, 11875102, 11835009, and 11690021), the Liaoning Revitalization Talents Program (Grant No. XLYC1905011), the Fundamental Research Funds for the Central Universities (Grant No. N2005030), and the Top- Notch Young Talents Program of China (Grant No. W02070050).
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