Upper Bound of 0.28 eV on Neutrino Masses from the Largest Photometric Redshift Survey

Phys. Rev. Lett. 105, 031301
The best fit angular power spectra Cl in the combined analysis (solid lines) are plotted over the MegaZ DR7 data. The panels relate to four redshift bins with width Δz=0.05 from z=0.45 (main panel) to z=0.65 (panel 4). These spectra are good fits to the galaxy statistics including scales not utilized in the analysis (l>300). The fit is also plotted for linear spectra (dashed lines) and highlights the scale at which the nonlinear regime starts to become significant. The dotted line demonstrates the effect of introducing mν=1eV neutrinos with all parameters, except Ωc, held fixed.The best fit angular power spectra Cl in the combined analysis (solid lines) are plotted over the MegaZ DR7 data. The panels relate to four redshift bins with width Δz=0.05 from z=0.45 (main panel) to z=0.65 (panel 4). These spectra are good fits to ... Show more
Left Panel: The marginalized 1D distribution for the neutrino from three incrementally combined analyses. The vertical dashed lines correspond to 95% confidence levels. Other Panels: 68% and 95% marginalized distributions for the matter density Ωm, Hubble parameter h, and spectral index ns against the total neutrino masses. The contours correspond to (from bottom layer) WMAP-only (red/dark), WMAP+MegaZ (yellow/light), WMAP+SNe+BAO (blue/dark), and WMAP+SNe+BAO+MegaZ+HST (green/light). Table  highlights that the vast majority of the gain in the last two contours originates from the new and complementary galaxy clustering data.Left Panel: The marginalized 1D distribution for the neutrino from three incrementally combined analyses. The vertical dashed lines correspond to 95% confidence levels. Other Panels: 68% and 95% marginalized distributions for the matter density Ωm, H... Show more
The 2D 68% and 95% contours and marginalized 1D distributions for 7 cosmological parameters (Ωbh2, Ωch2, ΩΛ, ns, τ, ln(1010As), and mν) in a WMAP5+SNe+BAO+MegaZ DR7+HST combined constraint (red contours). The amplitude of the Sunyaev-Zeldovich fluctuations (ASZ) and four bias parameters (b1, b2, b3, b4) are marginalized over but not plotted. The black contours are given for the WMAP-only analysis.The 2D 68% and 95% contours and marginalized 1D distributions for 7 cosmological parameters (Ωbh2, Ωch2, ΩΛ, ns, τ, ln(1010As), and mν) in a WMAP5+SNe+BAO+MegaZ DR7+HST combined constraint (red contours). The amplitude of the Sunyaev-Zeldovich fluc... Show more
Introduction.—

Studies of the neutrino have traditionally been the realm of particle physics experiments, with Super-Kamiokande [1] first indicating the presence of mass. Neutrinos were shown to oscillate between the known flavors ( νe, νμ, ντ) solving, in the process, the long-standing solar neutrino problem. This implies the neutrinos have at least two nonzero mass eigenstates ( m1, m2, m3) because the flavor mixing depends on the differences between their masses squared. Subsequently, bounds have been placed on the splitting between the neutrino mass eigenstates from a host of solar, accelerator, and atmospheric experiments; |Δm312|2.4×10-3eV2 and Δm2127.7×10-5eV2 (e.g., [2]). However, currently both the absolute scale and the hierarchy of the masses remain hidden. KATRIN, a kinematic beta decay experiment [3], aims to provide a constraint in the future.

Cosmology not only probes the absolute mass scale of the neutrino but is a completely independent method to test against, e.g., [4,5]. In any case, it is imperative to include an accurate prescription for the neutrino in cosmology, as any failure to do so can bias the other cosmological parameters. A cosmological constraint on the sum of the neutrino masses is primarily a constraint on the relic big bang neutrino density Ων. One can relate this density to the sum of the mass eigenstates mν (e.g., [6]) as given by

Ων=mν93.14h2eV.
(1)

The direct effects of the neutrinos depend on whether they are relativistic or nonrelativistic and the scale under consideration. Neutrinos have a large thermal velocity as a result of their low mass and subsequently erase their own perturbations on scales smaller than the free streaming length [5,7]. This subsequently contributes to a suppression of the statistical clustering of galaxies over small scales and can be observed in a galaxy survey. The abundance of neutrinos in the Universe can also have a direct effect on the primary CMB anisotropies if nonrelativistic before the time of decoupling (i.e., when sufficiently massive). However, one of the most clear effects at this epoch is a displacement in the time of matter-radiation equality. All these cosmological effects can be used to impose bounds on the neutrino mass.

Previous studies have capitalized on these signatures and have started to place sub eV constraints on the absolute mass scale [8–13]. We utilize the new Sloan Digital Sky Survey MegaZ luminous red galaxy (LRG) DR7 galaxy clustering data [14] to provide the first photometric galaxy clustering constraint on the neutrino and, combining with the CMB, examine the complementarity of these early- and late-time probes. With an almost comprehensive combination of probes this renders one of the tightest constraints on the neutrinos in cosmology and therefore physics.

Assumptions.—

We assume a flat universe with Gaussian and adiabatic primordial fluctuations and a constant spectral index. The effective number of neutrinos is fixed to Neff=3.04, thereby assuming no sterile neutrinos or other relativistic degrees of freedom. The constant dark energy equation of state is at first set to w=-1 and later relaxed. Finally, we consider the neutrinos to be completely mass degenerate given that current inferred bounds are much greater than the splitting hierarchies. The potential of future surveys to discriminate the mass hierarchy has been discussed in [15–20].

Analysis.—

Although parameter degeneracies and a mild insensitivity to relativistic (lighter) neutrinos limit the upper bound one can place on mν with the CMB [21], it represents a clean and relatively systematicless cosmological tool whose high statistical discrimination of the remaining cosmological model facilitates a competitive combination of probes. We therefore start by using the latest 5-year WMAP data and likelihood as described in [22] to vary seven ΛCDM parameters— Ωbh2, Ωch2, ΩΛ, ns, τ, ln(1010As), and ASZ—in addition to mν. τ, ns, and As represent the optical depth to reionization, the scalar spectral index, and the amplitude of curvature perturbations defined at k=0.002/Mpc, respectively. The contributions from the Sunyaev-Zeldovich fluctuations are included by adding a template spectrum ClSZ with prefactor ASZ following [23]. This is allowed to vary as 0<ASZ<2 [22]. We use the pre–March 2008 version of CAMB [24] to produce the CMB power spectra. The reionization is therefore treated as a semi-instantaneous process. The gravitational lensing effect on the CMB is also included, e.g., [25], and the CosmoMC package [26] is used for parameter exploration.

Our CMB run yields mν<1.271eV at the 95% confidence level consistent with [12]. This bound implies the neutrinos were relativistic at decoupling and as such induces a degeneracy between the neutrino masses and Ωm as well as the Hubble parameter h. This can be seen in Fig. 2 as well as [11,12,21]. This degeneracy can be improved by adding supernovae (SNe) data from the first year Supernova Legacy Survey (SNLS [27]) and the baryon acoustic oscillation (BAO) data from [28]. Our analysis for WMAP+SNe+BAO gives mν<0.695eV (95% CL) similar to [12] ( mν<0.67eV) and [11] ( mν<0.76eV).

In order to go beyond such studies we include the MegaZ LRG (DR7) photometric redshift survey that will be presented in [14], which we have checked to be compatible with earlier Sloan Digital Sky Survey clustering [29] and photo- z analyses [30,31]. This adds galaxy clustering information that is sensitive to the growth of structure suppressed by the free streaming neutrinos. The Sloan Digital Sky Survey colors provide reliable photometric redshift estimates and, due to their high luminosity, probe a large region of cosmic volume. Encapsulating 7746deg2, we utilize 723 556 photometrically determined LRGs in four redshift bins of width Δz=0.05 within 0.45<z<0.65 in a spherical harmonic analysis of the galaxy distribution until a maximum multipole lmax=300. These galaxies are calibrated by the 2SLAQ redshift survey [32] using ANNz [30] as in [31] and the previous DR4 photometric release [29,33]. Specifically we use the angular power spectrum defined as

Clδ2Dδ*2D=4πΔ2(k)Wl2(k)dkk,
(2)

where Δ2(k) is the dimensionless power spectrum calculated with CAMB. The matter distribution is projected onto a plane in the sky with weight Wl2(k) in this statistic described by both Wl(k)=f(z)jl(kz)dz and f(z)=n(z)D(z)(dzdx), with the spherical Bessel function jl(kz), the linear growth factor D(z), and the normalized redshift distribution n(z). The effects of redshift space distortions are included as described in [34,35]. The likelihood combines the four measured redshift bins and includes the full covariance as a result of photometric errors scattering galaxies between bins and therefore correlating slices. There are four additional parameters included in the study as a result of the galaxy bias in each bin ( b1, b2, b3, and b4), i.e., modestly accounting for the redshift dependence, which is seen to increase at high z [14,29]. Despite the nonlinear contribution becoming significant only at scales l>300 we use halofit [36] to model the nonlinear power spectrum. It is interesting to note that the point corresponding to the largest angular scale band in the highest redshift bin indicates an excess of power. Hints of this were seen in the earlier photometric releases by [29,35] with the excess labeled by the arrow in panel 4 in Fig. 1.

This survey is not only one of the most recent and largest to date but is one of the most competitive available. However, these power spectra provide an additional incentive for this combined measurement. This is because the BAOs, which were shown to be so advantageous before, can be used in conjunction to MegaZ with no cross covariance. The BAO data are extracted at z=0.2 and z=0.35, whereas MegaZ is defined at a higher redshift. They therefore constitute two independent data sets and can be used both simply and simultaneously.

By combining the MegaZ LRGs as described above with the previous CMB, SNe, and BAO data in a complete joint analysis we find a significantly lower bound of mν<0.325eV at the 95% confidence level. Again, this is roughly a factor 2 improvement in the neutrino masses with the addition of the LRGs and is shown clearly against Ωm, h, and the one-dimensional (1D) marginalized distribution in Fig. 2.

The information on the growth of structure is paramount to the improvement seen in this study. However, part of this information originates from the quasinonlinear regime and could systematically bias the inferred constraint. While approaches are developed and work continues into the effects of the neutrino on these scales (e.g., [37]), we repeat the combined analysis with the smaller scales removed. By truncating the multipoles at lmax=200 this more conservative approach is seen to give a similar but slightly relaxed limit of mν<0.393eV. While this highlights the importance of understanding nonlinearities for obtaining the most stringent constraints, it is reassuring that there is still a marked improvement on the previous study ( CMB+SNe+BAO) with linear LRGs.

It is also intriguing to compare the input of the LRGs to those of the two distance measures ( SNe+BAO). These have previously been highly beneficial to the uncertainty. We therefore perform a joint analysis using just the WMAP5 and LRG data, subsequently obtaining the limit mν<0.651eV at the 95% confidence level. This is comparable to the spectroscopic DR7 galaxy clustering addition to the CMB in [13] with mν<0.62eV and illustrates the development of photometric surveys as a competitive tool for the future.

We conclude this work by further restricting the cosmological parameter space with the addition of the new Hubble Space Telescope (HST) prior on the Hubble parameter to the WMAP5+SNe+BAO+MegaZ DR7 run. The improved prior was recently found to be H0=74.2±3.6kms-1Mpc-1 [38]. With this, the final limit in this study is reduced to mν<0.28eV at the 95% confidence level. This is one of the tightest constraints in the literature. The angular power spectra Cl corresponding to the best fit values are plotted in Fig. 1 with the galaxy clustering data. An overview of all the neutrino bounds are displayed in Table I and a plot of all parameter combinations compared to the CMB-only study is displayed in Fig. 3. Our estimates on the bias are b1=1.74±0.07, b2=2.02±0.08, b3=2.12±0.09, and b4=2.39±0.10.

TABLE I.

A summary of the bounds placed on mν in this Letter. l200 corresponds to the truncation in the maximum multipole scale to remove the quasinonlinear regime. The top constraints are for w=-1; the bottom for w-1, marginalized over.

mν (95% CL) Analysis
< 1.271 eV WMAP5
< 0.695 eV WMAP 5 + SNe + BAO
< 0.651 eV WMAP 5 + Mega Z
< 0.393 eV WMAP 5 + SNe + BAO + Mega Z ( l 200 )
< 0.344 eV WMAP 5 + SNe + BAO + Mega Z ( l 200 ) + HST
< 0.325 eV WMAP 5 + SNe + BAO + Mega Z
< 0.281 eV WMAP 5 + SNe + BAO + MegaZ + HST
< 0.491 eV WMAP 5 + SNe + BAO + Mega Z ( l 200 ) + HST
< 0.471 eV WMAP 5 + SNe + BAO + Mega Z + HST

For w-1 the tighter bound relaxes slightly to mν<0.47eV, which should be compared to mν0.62eV from [39]. We note that biasing could act to mimic the neutrino signature over smaller scale analyses. As a gauge of this effect we implement, as an example, the “ Q model” of [40], resulting in a combined constraint (all data) of mν<0.44eV. However, undertaking the challenge of modeling the possibility of scale dependent bias accurately and self-consistently is left to future work.

Conclusions.—

Using the biggest ever large-scale structure survey, we have set bounds on the neutrino masses at mν<0.28eV ( lmax=300) and mν<0.34eV ( lmax=200) at 95% CL, when combined with WMAP5+SNe+BAO+HST data. This is the first ever determination of neutrino masses from a photometric galaxy redshift survey. Not only have we shown that photometric redshifts can be used for this problem, but also that such a galaxy survey is competitive with all currently available geometric probes ( SNe+BAO) or spectroscopic clustering when added to the CMB. Our constraint is one of the tightest current bounds available without the use of data from Lyman- α (e.g., [9]), which is prone to systematics, or a complicated modeling of the bias [41]. Further, all our results show that KATRIN’s [3] projected 90% sensitivity ( mν0.6eV) leaves an unlikely neutrino mass detection. Finally, our overall method shows great promise for the next generation of surveys, which will yield upper limits of, e.g., 0.12 eV [42] and 0.025 eV [15] at 95% C.L.

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About the Authors

Image of Shaun A. Thomas
Image of Filipe B. Abdalla
Image of Ofer Lahav

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