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Constraints on Neutrino Masses from Baryon Acoustic Oscillation Measurements

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^{}

_{v}, h, and Ω

_{b}h

^{2}. For and , we obtain at 95% confidence.

KEYWORDS

1. Introduction

We extend the analysis presented in “Study of baryon acoustic oscillations with SDSS DR13 data and measurements of ${\Omega}_{k}$ and ${\Omega}_{\text{DE}}\left(a\right)$ ” [1] to include neutrino masses. The present analysis has three steps: 1) we calculate the distance of propagation ${r}_{s}$ , in units of $c/{H}_{0}$ , referred to the present time, of sound waves in the photon-electron-baryon plasma until decoupling by numerical integration of Equation (16) and Equation (17) of Ref. [1] ; 2) we fit the Friedmann equation of evolution of the universe to 21 independent Baryon Acoustic Oscillation (BAO) distance measurements listed in [1] used as uncalibrated standard rulers and obtain the length d of these rulers, in units of $c/{H}_{0}$ , referred to the present time; and 3) we set

${r}_{s}=d$ (1)

to constrain the sum of neutrino masses $\sum}\text{\hspace{0.05em}}\text{\hspace{0.05em}}{m}_{\nu$ . c is the speed of light, and ${H}_{0}\equiv 100h\text{\hspace{0.17em}}\text{km}\cdot {\text{s}}^{-1}\cdot {\text{Mpc}}^{-1}$ is the present day Hubble expansion parameter.

2. Constraints on Neutrino Masses

The main body of this article assumes: 1) flat space, i.e. ${\Omega}_{k}=0$ , and 2) constant dark energy density relative to the critical density, i.e. ${\Omega}_{\text{DE}}$ independent of the expansion parameter a. These constraints are in agreement with all observations to date [1] [2] . Results without these constraints are presented in Appendix 1. Results with partial data sets are presented in Appendix 2.

To be specific we consider three active neutrino flavors with three eigenstates with nearly the same mass ${m}_{\nu}$ , so $\sum}\text{\hspace{0.05em}}{m}_{\nu}=3{m}_{\nu$ . This is a useful scenario to consider since our current limits on ${m}_{\nu}^{2}$ are much larger than the mass-squared-differences $\Delta {m}^{2}$ and $\Delta {m}_{21}^{2}$ obtained from neutrino oscillations [2] . These neutrinos become non-relativistic at a neutrino temperature ${T}_{\nu}={m}_{\nu}/3.15$ or a photon temperature $T={m}_{\nu}{\left(11/4\right)}^{1/3}/3.15$ . The corresponding expansion parameter is ${a}_{\nu}={T}_{0}/T=5.28\times {10}^{-4}\left(1\text{\hspace{0.17em}}\text{eV}/{m}_{\nu}\right)$ .

The matter density relative to the present critical density is ${\Omega}_{m}/{a}^{3}$ for $a>{a}_{\nu}$ . ${\Omega}_{m}$ includes the density ${\Omega}_{\nu}={h}^{-2}{\displaystyle \sum}\text{\hspace{0.05em}}{m}_{\nu}/94\text{\hspace{0.17em}}\text{eV}$ of Dirac or Majorana neutrinos that are non-relativistic today. Note that for Dirac neutrinos we are considering the scenario in which right-handed neutrinos and left-handed anti-neutrinos are sterile and never achieved thermal equilibrium. Our results can be amended for other specific scenarios. For $a<{a}_{\nu}$ we take the matter density to be $\left({\Omega}_{m}-{\Omega}_{\nu}\right)/{a}^{3}$ . The radiation density is ${\Omega}_{\gamma}{N}_{\text{eq}}/\left(2{a}^{4}\right)$ for $a<{a}_{\nu}$ , where ${N}_{\text{eq}}=3.36$ for three flavors of Dirac (mostly) left-handed neutrinos and right-handed anti-neutrinos. We also take ${N}_{\text{eq}}=3.36$ for three active flavors of Majorana left-handed and right-handed neutrinos. For $a>{a}_{\nu}$ , we take the radiation density to be $\left({\Omega}_{\gamma}{N}_{eq}/2-{a}_{\nu}{\Omega}_{\nu}\right)/{a}^{4}={\Omega}_{\gamma}/{a}^{4}$ . The present density of photons relative to the critical density is ${\Omega}_{\gamma}=2.473\times {10}^{-5}{h}^{-2}$ [2] .

The data used to obtain d are 18 independent BAO distance measurements with Sloan Digital Sky Survey (SDSS) data release DR13 galaxies in the redshift range $z=0.1$ to 0.7 [3] [4] [5] summarized in Table 3 of [1] , two BAO distance measurements in the Lyman-alpha forest (Lyα) at $z=2.36$ (cross-correlation [6] ) and $z=2.34$ (auto-correlation [7] ) summarized in Section 6 of [1] , and the Cosmic Microwave Background (CMB) correlation angle ${\theta}_{\text{MC}}=0.010410\pm 0.000005$ [2] [8] , used as an uncalibrated standard ruler. Note that the correlation angle ${\theta}_{\text{MC}}$ is also determined by BAO. These 21 independent BAO measurements and full details of the fitting method are presented in [1] .

As a reference we take

$h=0.678\pm 0.009,\text{\hspace{1em}}{\Omega}_{b}{h}^{2}=0.02226\pm 0.00023$ (2)

(at 68% confidence) from “Planck TT + low P + lensing” data (that does not contain BAO information) [2] . ${\Omega}_{b}$ is the present density of baryons relative to the critical density.

Due to correlations and non-linearities we obtain our final result (Equation (9) below) with a global fit. The following equations are included to illustrate the dependence of ${r}_{s}$ and d on the cosmological parameters h, ${\Omega}_{b}{h}^{2}$ and $\sum}\text{\hspace{0.05em}}{m}_{\nu$ in limited ranges of interest. Integrating the comoving sound speed of the photon-baryon-electron plasma until ${a}_{\text{dec}}=1/\left(1+{z}_{\text{dec}}\right)$ with ${z}_{\text{dec}}=1089.9\pm 0.4$ [2] we obtain

${r}_{s}\approx 0.0339\times A\times {\left(\frac{0.28}{{\Omega}_{m}}\right)}^{0.24}$ (3)

with

$A\approx 0.990+0.007\cdot \delta h-0.001\cdot \delta b+0.020\cdot \frac{{\displaystyle \sum}\text{\hspace{0.05em}}{m}_{\nu}}{1\text{\hspace{0.17em}}\text{eV}},$ (4)

where

$\delta h\equiv \left(h-0.678\right)/0.009\mathrm{,}$ (5)

$\delta b\equiv \left({\Omega}_{b}{h}^{2}-0.02226\right)/0.00023\mathrm{.}$ (6)

To obtain d we minimize the ${\chi}^{2}$ with 21 terms, corresponding to the 21 BAO observables, with respect to ${\Omega}_{\text{DE}}$ and d, and obtain ${\Omega}_{\text{DE}}=0.718\pm 0.003$ and

$d\approx 0.0340\pm \mathrm{0.0002,}$ (7)

with ${\chi}^{2}$ per degree of freedom 19.8/19, and correlation coefficient 0.989 between ${\Omega}_{\text{DE}}$ and d (this high correlation coefficient is due to the high precision of ${\theta}_{\text{MC}}$ ). Setting ${r}_{s}=d$ we obtain

$\sum}\text{\hspace{0.05em}}{m}_{\nu}\approx 0.73-0.35\cdot \delta h+0.05\cdot \delta b\pm 0.15\text{\hspace{0.17em}}\text{eV}\mathrm{.$ (8)

A more precise result is obtained with a global fit by minimizing the ${\chi}^{2}$ with 21 terms varying ${\Omega}_{\text{DE}}$ and $\sum}\text{\hspace{0.05em}}{m}_{\nu$ directly. We obtain ${\Omega}_{\text{DE}}=0.7175\pm 0.0023$ and

$\sum}\text{\hspace{0.05em}}{m}_{\nu}=0.711-0.335\cdot \delta h+0.050\cdot \delta b\pm 0.063\text{\hspace{0.17em}}\text{eV},$ (9)

with ${\chi}^{2}/\text{d}\text{.f}\text{.}=19.9/19$ , and correlation coefficient 0.924 between ${\Omega}_{\text{DE}}$ and $\sum}\text{\hspace{0.05em}}{m}_{\nu$ . This is our main result. Equation (9) is obtained from BAO measurements alone, and is written in a way that can be combined with independent constraints on the cosmological parameters $\sum}\text{\hspace{0.05em}}{m}_{\nu$ , $h$ and ${\Omega}_{b}{h}^{2}$ , such as measurements of the power spectrum of density fluctuations $P\left(k\right)$ , the CMB, and direct measurements of the Hubble parameter.

Setting $\delta h=\pm 1$ and $\delta b=\pm 1$ we obtain the following upper bound on the mass of active neutrinos ${m}_{\nu}=\frac{1}{3}{\displaystyle \sum}\text{\hspace{0.05em}}{m}_{\nu}$ :

${m}_{\nu}<0.43\text{\hspace{0.17em}}\text{eV}\text{\hspace{0.17em}}\text{at}\text{\hspace{0.17em}}\mathrm{95\%}\text{\hspace{0.17em}}\text{confidence}\text{.}$ (10)

Appendix

Appendix 1. Removing constraints

Freeing ${\Omega}_{k}$ and keeping ${\Omega}_{\text{DE}}$ constant we obtain ${\Omega}_{k}=-0.003\pm 0.006$ , ${\Omega}_{\text{DE}}+2.2{\Omega}_{k}=0.719\pm 0.003$ , and

$\sum}\text{\hspace{0.05em}}{m}_{\nu}=0.623-0.334\cdot \delta h+0.050\cdot \delta b\pm 0.191\text{\hspace{0.17em}}\text{eV}\mathrm{,$ (11)

with ${\chi}^{2}/\text{d}\text{.f}\text{.}=19.6/18$ .

Fixing ${\Omega}_{k}=0$ and letting ${\Omega}_{\text{DE}}\left(a\right)={\Omega}_{\text{DE}}\cdot \left\{1+{w}_{a}\cdot \left(1-a\right)\right\}$ we obtain ${\Omega}_{\text{DE}}=0.716\pm 0.004$ , ${w}_{a}=0.064\pm 0.148$ , and

$\sum}\text{\hspace{0.05em}}{m}_{\nu}=0.603-0.349\cdot \delta h+0.052\cdot \delta b\pm 0.257\text{\hspace{0.17em}}\text{eV},$ (12)

with ${\chi}^{2}/\text{d}\text{.f}\text{.}=19.7/18$ .

Freeing ${\Omega}_{k}$ and letting ${\Omega}_{\text{DE}}\left(a\right)={\Omega}_{\text{DE}}\cdot \left\{1+{w}_{a}\cdot \left(1-a\right)\right\}$ we obtain ${\Omega}_{k}=-0.008\pm 0.004$ , ${\Omega}_{\text{DE}}+2.2{\Omega}_{k}=0.718\pm 0.004$ , ${w}_{a}=0.227\pm 0.069$ , and

$0<{\displaystyle \sum}\text{\hspace{0.05em}}{m}_{\nu}=-0.388-0.350\cdot \delta h+0.050\cdot \delta b\pm 0.830\text{\hspace{0.17em}}\text{eV},$ (13)

with ${\chi}^{2}/\text{d}\text{.f}\text{.}=17.8/17$ .

Appendix 2. Removing data.

In this Appendix we apply the constraints ${\Omega}_{k}=0$ and ${\Omega}_{\text{DE}}$ constant. Removing the measurement of ${\theta}_{\text{MC}}$ we obtain ${\Omega}_{\text{DE}}=0.722\pm 0.011$ and

$\sum}\text{\hspace{0.05em}}{m}_{\nu}=0.579-0.333\cdot \delta h+0.049\cdot \delta b\pm 0.285\text{\hspace{0.17em}}\text{eV},$ (14)

with ${\chi}^{2}/\text{d}\text{.f}\text{.}=19.7/18$ .

Removing the measurement of ${\theta}_{\text{MC}}$ and the two Lya measurements we obtain ${\Omega}_{\text{DE}}=0.716\pm 0.014$ and

$\sum}\text{\hspace{0.05em}}{m}_{\nu}=0.743-0.330\cdot \delta h+0.049\cdot \delta b\pm 0.366\text{\hspace{0.17em}}\text{eV},$ (15)

with ${\chi}^{2}/\text{d}\text{.f}\text{.}=11.2/16$ .

Keeping only the measurement of ${\theta}_{\text{MC}}$ we need to fix ${\Omega}_{\text{DE}}$ in order to get zero degrees of freedom and have a unique solution. The best way to fix ${\Omega}_{\text{DE}}$ is with BAO measurements, and that is the purpose of the present study.

Conflicts of Interest

The authors declare no conflicts of interest.

Cite this paper

*International Journal of Astronomy and Astrophysics*,

**8**, 1-5. doi: 10.4236/ijaa.2018.81001.

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