• • • We do not use the following data for averages, fits, limits, etc. • • • 
$<0.26$ 
95 
^{ 1} 

COSM 
$<0.18$ 
95 
^{ 2} 

COSM 
$<0.152$ 
95 
^{ 3} 

COSM 
$0.064$ ${}^{+0.061}_{0.005}$ 
95 
^{ 4} 

COSM 
$<0.151$ 
95 
^{ 5} 

COSM 
$<0.14$ 
95 
^{ 6} 

COSM 
$<0.0926$ 
90 
^{ 7} 

COSM 
$<0.18$ 
95 
^{ 8} 

COSM 
$<0.14$ 
95 
^{ 9} 

COSM 
$<0.23$ 
95 
^{ 10} 

COSM 
$0.320$ $\pm0.081$ 

^{ 11} 

COSM 
$0.35$ $\pm0.10$ 

^{ 12} 

COSM 
$0.22$ ${}^{+0.09}_{0.10}$ 

^{ 13} 

COSM 
$<0.22$ 
95 
^{ 14} 

COSM 
$0.32$ $\pm0.11$ 

^{ 15} 

COSM 
$<0.26$ 
95 
^{ 16} 

COSM 
$<0.18$ 
95 
^{ 17} 

COSM 
$<0.24$ 
68 
^{ 18} 

COSM 
$<0.29$ 
95 
^{ 19} 

COSM 
$<0.81$ 
95 
^{ 20} 

COSM 
$<0.44$ 
95 
^{ 21} 

COSM 
$<0.6$ 
95 
^{ 22} 

COSM 
$<0.28$ 
95 
^{ 23} 

COSM 
$<1.1$ 

^{ 24} 

COSM 
$<1.3$ 
95 
^{ 25} 

COSM 
$<1.2$ 

^{ 26} 

COSM 
$<0.33$ 

^{ 27} 

COSM 
$<0.28$ 

^{ 28} 

COSM 
$\text{< 0.17  2.3}$ 

^{ 29} 

COSM 
$<0.42$ 
95 
^{ 30} 

COSM 
$\text{< 0.63  2.2}$ 

^{ 31} 

COSM 
$<0.24$ 
95 
^{ 32} 

COSM 
$<0.62$ 
95 
^{ 33} 

COSM 
$<1.2$ 

^{ 34} 

COSM 
$<0.17$ 
95 
^{ 32} 

COSM 
$<2.0$ 
95 
^{ 35} 

COSM 
$<0.75$ 

^{ 36} 

COSM 
$<1.0$ 

^{ 37} 

COSM 
$<0.7$ 

^{ 38} 

COSM 
$<0.9$ 

^{ 39} 

COSM 
$<4.2$ 

^{ 40} 

COSM 
$<2.7$ 

^{ 41} 

COSM 
$<5.5$ 

^{ 42} 

ASTR 
$<180$ 



COSM 
$<132$ 



COSM 
$<280$ 



COSM 
$<400$ 



COSM 
^{1}
LOUREIRO 2019 combines data from large scale structure, cosmic microwave background, type Ia supernovae and big bang nucleosynthesis using physically motivated neutrino mass models.

^{2}
UPADHYE 2019 uses the shape of the BOSS redshiftspace galaxy power spectrum in combination with the CMB, and supernovae data. Limit weakens to $<$ 0.54 eV if the dark energy equation of state is allowed to vary.

^{3}
CHOUDHURY 2018 combines 2015 Planck CMB temperature data, information from the optical depth to reionization from Planck 2016 intermediate results together with baryon acoustic oscillation data from BOSS, MGS, and 6dFGS as well as supernovae Type Ia data from the Pantheon Sample. The limit is strengthened to 0.118 eV when high$\mathit l$ CMB polarization data is also included.

^{4}
SIMPSON 2017 uses a combination of laboratory and cosmological measurements to determine the light neutrino masses and argue that there is strong evidence for the normal mass ordering.

^{5}
Combines temperature anisotropies of the CMB from Planck with data on baryon acoustic oscillations and the optical depth to reionization. Limit is strengthened to 0.118 when high multipole polarization data is included. Updates GIUSARMA 2016 .

^{6}
Constrains the total mass of neutrinos using the Lymanalpha forest power spectrum with BOSS (midresolution), XQ100 (highresolution) and CMB. Without the CMB data, the limit relaxes to 0.8 eV. Supersedes PALANQUEDELABROUILLE 2015A.

^{7}
Constrains the total mass of neutrinos from Planck CMB data combined with baryon acoustic oscillation and Planck cluster data.

^{8}
Constrains the total mass of neutrinos from BAO data from SDSSIII/BOSS combined with CMB data from Planck. Limit quoted for normal mass hierarchy. The limit for the inverted mass hierarchy is 0.20 eV and for the degenerate mass hierarchy it is 0.15 eV.

^{9}
ROSSI 2015 sets limits on the sum of neutrino masses using BOSS Lyman alpha forest data combined with Planck CMB data and baryon acoustic oscillations.

^{10}
Constrains the total mass of neutrinos from Planck CMB data along with WMAP polarization, high L, and BAO data.

^{11}
Finite neutrino mass fit to resolve discrepancy between CMB and lensing measurements.

^{12}
Fit to the total mass of neutrinos from BOSS data along with WMAP CMB data and data from other BAO constraints and weak lensing.

^{13}
Fit to the total mass of neutrinos from Planck CMB data along with BAO.

^{14}
Constrains the total mass of neutrinos from Planck CMB data combined with baryon acoustic oscillation data from BOSS and HST data on the Hubble parameter.

^{15}
Fit based on the SPTSZ survey combined with CMB, BAO, and ${{\mathit H}_{{0}}}$ data.

^{16}
Constraints the total mass of neutrinos (marginalizing over the effective number of neutrino species) from CMB, CMB lensing, BAO, and galaxy clustering data.

^{17}
Constrains the total mass of neutrinos from Planck CMB data combined with baryon acoustic oscillation data from BOSS, 6dFGS, SDSS, WiggleZ data on the galaxy power spectrum, and HST data on the Hubble parameter. The limit is increased to 0.25 eV if a lower bound to the sum of neutrino masses of 0.04 eV is assumed.

^{18}
Constrains the total mass of neutrinos from observational Hubble parameter data with sevenyear WMAP data and the most recent estimate of ${{\mathit H}_{{0}}}$.

^{19}
Constrains the total mass of neutrinos from the CFHTLS combined with sevenyear WMAP data and a prior on the Hubble parameter. Limit is relaxed to 0.41 eV when small scales affected by nonlinearities are removed.

^{20}
Constrains the total mass of neutrinos from the Sloan Digital Sky Survey and the fiveyear WMAP data.

^{21}
Constrains the total mass of neutrinos from the 7year WMAP data including SDSS and HST data. Limit relaxes to 1.19 eV when CMB data is used alone. Supersedes HANNESTAD 2006 .

^{22}
Constrains the total mass of neutrinos from a combination of CMB data, a recent measurement of ${{\mathit H}_{{0}}}$ (SHOES), and baryon acoustic oscillation data from SDSS.

^{23}
Constrains the total mass of neutrinos from SDSS MegaZ LRG DR7 galaxy clustering data combined with CMB, HST, supernovae and baryon acoustic oscillation data. Limit relaxes to 0.47 eV when the equation of state parameter, $\mathit w$ ${}\not=$ 1.

^{24}
Constrains the total mass of neutrinos from weak lensing measurements when combined with CMB. Limit improves to 0.54 eV when supernovae and baryon acoustic oscillation observations are included. Assumes $\Lambda CDM$ model.

^{25}
Constrains the total mass of neutrinos from fiveyear WMAP data. Limit improves to 0.67 eV when supernovae and baryon acoustic oscillation observations are included. Limits quoted assume the $\Lambda CDM$ model. Supersedes SPERGEL 2007 .

^{26}
Constrains the total mass of neutrinos from weak lensing measurements when combined with CMB. Limit improves to 0.03 $<\Sigma {\mathit m}_{{{\mathit \nu}}}<$ 0.54 eV when supernovae and baryon acoustic oscillation observations are included. The slight preference for massive neutrinos at the twosigma level disappears when systematic errors are taken into account. Assumes $\Lambda CDM$ model.

^{27}
Constrains the total mass of neutrinos from recent Chandra Xray observations of galaxy clusters when combined with CMB, supernovae, and baryon acoustic oscillation measurements. Assumes flat universe and constant darkenergy equation of state, $\mathit w$.

^{28}
Constraints the total mass of neutrinos from recent CMB and SOSS LRG power spectrum data along with bias mass relations from SDSS, DEEP2, and LymanBreak Galaxies. It assumes $\Lambda CDM$ model. Limit degrades to 0.59 eV in a more general wCDM model.

^{29}
Constrains the total mass of neutrinos from neutrino oscillation experiments and cosmological data. The most conservative limit uses only WMAP threeyear data, while the most stringent limit includes CMB, largescale structure, supernova, and Lymanalpha data.

^{30}
Constrains the total mass of neutrinos from recent CMB, large scale structure, SN1a, and baryon acoustic oscillation data. The limit relaxes to 1.75 when WMAP data alone is used with no prior. Paper shows results with several combinations of data sets. Supersedes KRISTIANSEN 2006 .

^{31}
Constrains the total mass of neutrinos from the CMB and the large scale structure data. The most conservative limit is obtained when generic initial conditions are allowed.

^{32}
Constrains the total mass of neutrinos from recent CMB, large scale structure, Lymanalpha forest, and SN1a data.

^{33}
Constrains the total mass of neutrinos from recent CMB and large scale structure data. See also GOOBAR 2006 . Superseded by HANNESTAD 2010 .

^{34}
Constrains the total mass of neutrinos from the CMB and the final 2dF Galaxy Redshift Survey.

^{35}
Constrains the total mass of neutrinos from the CMB experiments alone, assuming $\Lambda $CDM Universe. FUKUGITA 2006 show that this result is unchanged by the 3year WMAP data.

^{36}
Constrains the total mass of neutrinos from the power spectrum of fluctuations derived from the Sloan Digital Sky Survey and the 2dF galaxy redshift survey, WMAP and 27 other CMB experiments and measurements by the HST Key project.

^{37}
Constrains the total mass of neutrinos from the power spectrum of fluctuations derived from the Sloan Digital Sky Survey, the 2dF galaxy redshift survey, WMAP and ACBAR. The limit is strengthened to 0.6 eV when measurements by the HST Key project and supernovae data are included.

^{38}
Constrains the fractional contribution of neutrinos to the total matter density in the Universe from WMAP data combined with other CMB measurements, the 2dfGRS data, and Lyman $\alpha $ data. The limit does not noticeably change if the Lyman $\alpha $ data are not used.

^{39}
LEWIS 2002 constrains the total mass of neutrinos from the power spectrum of fluctuations derived from the CMB, HST Key project, 2dF galaxy redshift survey, supernovae type$~$Ia, and BBN.

^{40}
WANG 2002 constrains the total mass of neutrinos from the power spectrum of fluctuations derived from the CMB and other cosmological data sets such as galaxy clustering and the Lyman $\alpha $ forest.

^{41}
FUKUGITA 2000 is a limit on neutrino masses from structure formation. The constraint is based on the clustering scale $\sigma _{8}$ and the COBE normalization and leads to a conservative limit of $0.9~$eV assuming 3$~$nearly degenerate neutrinos. The quoted limit is on the sum of the light neutrino masses.

^{42}
CROFT 1999 result based on the power spectrum of the ${}^{}\mathrm {Ly}$ $\alpha $ forest. If $\Omega _{{\mathrm {matter}}}<0.5$, the limit is improved to ${\mathit m}_{{{\mathit \nu}}}<2.4$ ($\Omega _{{\mathrm {matter}}}/0.17  1$) eV.
