Abstract
We study galaxy distributions with Sloan Digital Sky Survey SDSS DR14 data and with simulations searching for variables that can constrain neutrino masses. To be specific, we consider the scenario of three active neutrino eigenstates with approximately the same mass, so Σmv=3mv. Fitting the predictions of the ΛCDM model to the Sachs-Wolfe effect, σ8, the galaxy power spectrum Pga1(k) , fluctuations of galaxy counts in spheres of radii ranging from 16/h to 128/h Mpc, Baryon Acoustic Oscillation (BAO) measurements, and h=0.678±0.009, in various combinations, with free spectral index n, and free galaxy bias and galaxy bias slope, we obtain consistent measurements of Σmv. The results depend on h, so we have presented confidence contours in the (Σmv, h) plane. A global fit with h=0.678±0.009 obtains eV, and the amplitude and spectral index of the power spectrum of linear density fluctuations P(k): , and n=1.021±0.075. The fit also returns the galaxy bias b including its scale dependence.
Highlights
We measure neutrino masses by comparing the predictions of the ΛCDM model with measurements of the power spectrum of linear density perturbationsP (k )
We study galaxy distributions with Sloan Digital Sky Survey SDSS DR14 data and with simulations searching for variables that can constrain neutrino masses
( ) log10 Pgal (k ) h−3 Mpc3 ≈ 3.47 for our data sample, and ≈3.49 for our reference simulation. To test these ideas we can select a narrow range of MAGr, MAGg, or MAG to shift the noise upwards, compare Figures 9-11 (which plot the first term on the right hand side of Equation (45) and include the noise at large k)
Summary
We consider three active neutrino eigenstates with nearly the same mass, so ∑mν = 3mν. Shown are various fits to this data (with floating normalization), and to measurements of the Sachs-Wolfe effect, and σ8. The fit obtains A = 8738 Mpc , keq = 0.068h Mpc−1 , η = 4.5 , and b2 = 1.8 , with χ 2 = 24.7 for 19 degrees of freedom. Note that ∑mν is largely degenerate with the remaining parameters in Equation (5), unless we are able to constrain keq. The parameters A, η , and keq , as well as the normalization factor b2, are free in the fit. Ωm is the total (dark plus baryonic plus neutrino) matter density today relative to the critical density, and includes the contribu-
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
