Towards a cosmological neutrino mass detection

Allison, Rupert; Caucal, Paul; Calabrese, E.; Dunkley, Joanna; Louis, Thibaut

doi:10.1103/physrevd.92.123535

Cited by 225 publications

(263 citation statements)

References 79 publications

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“…This change leaves a characteristic imprint on several cosmological observables (see, e.g. [16,[63][64][65][66][67]), letting cosmology to strongly bound the neutrino mass scale, indeed providing the current strongest (albeit model dependent) bounds on Σ. Bounds on Σ from recent cosmological data have been presented in several papers (see, for example, [68][69][70][71][72][73] and references therein) while forecasts for near (and far) future cosmological datasets have been obtained in [74][75][76][77][78][79].…”

Section: Cosmologymentioning

confidence: 99%

Global constraints on absolute neutrino masses and their ordering

et al. 2017

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Within the standard three-neutrino framework, the absolute neutrino masses and their ordering (either normal, NO, or inverted, IO) are currently unknown. However, the combination of current data coming from oscillation experiments, neutrinoless double beta (0νββ) decay searches, and cosmological surveys, can provide interesting constraints for such unknowns in the sub-eV mass range, down to O(10 −1 ) eV in some cases. We discuss current limits on absolute neutrino mass observables by performing a global data analysis, that includes the latest results from oscillation experiments, 0νββ decay bounds from the KamLAND-Zen experiment, and constraints from representative combinations of Planck measurements and other cosmological data sets. In general, NO appears to be somewhat favored with respect to IO at the level of ∼ 2σ, mainly by neutrino oscillation data (especially atmospheric), corroborated by cosmological data in some cases. Detailed constraints are obtained via the χ 2 method, by expanding the parameter space either around separate minima in NO and IO, or around the absolute minimum in any ordering. Implications for upcoming oscillation and non-oscillation neutrino experiments, including β-decay searches, are also discussed.

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Section: Cosmologymentioning

confidence: 99%

Global constraints on absolute neutrino masses and their ordering

et al. 2017

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“…In particular, gravitational lensing converts some of the E-mode polarization into B-mode polarization (Zaldarriaga & Seljak 1998). Measurements of temperature and polarization with sufficient resolution and sensitivity can be used to reconstruct the intervening matter distribution, and,in the future, such bias-free measurements of large-scale structures will become some of the most powerful probes in cosmology (e.g., Hu 2002;Namikawa et al 2010;Wu et al 2014;Abazajian et al 2015;Allison et al 2015;Pan & Knox 2015). Lensing can also act as a noise source for primordial B modes, which peak at degreescales (e.g., Kesden et al 2002;Knox & Song 2002).…”

Section: Introductionmentioning

confidence: 99%

Bicep2/KECK ARRAY VIII: MEASUREMENT OF GRAVITATIONAL LENSING FROM LARGE-SCALE B-MODE POLARIZATION

Ade¹,

Ahmed²,

Aikin³

et al. 2016

ApJ

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We present measurements of polarization lensing using the 150 GHz maps, which include all data taken by the BICEP2andKeck Array Cosmic Microwave Background polarization experiments up to and including the 2014 observing season (BK14). Despite their modest angular resolution (~ 0 . 5), the excellent sensitivity (∼3μK-arcmin) of these maps makes it possible to directly reconstruct the lensing potential using only information at larger angular scales (  ℓ 700). From the auto-spectrum of the reconstructed potential, we measure an amplitude of the spectrum to be) and reject the no-lensing hypothesis at s 5.8 , which is the highest significance achieved to date using an EB lensing estimator. Taking ). We perform a series of null tests and consistency checks to show that these results are robust against systematics and are insensitive to analysis choices. These results unambiguously demonstrate that the B modes previously reported by BICEP/Keck at intermediate angular scales350) are dominated by gravitational lensing. The good agreement between the lensing amplitudes obtained from the lensing reconstruction and B-mode spectrum starts to place constraints on any alternative cosmological sources of B modes at these angular scales.

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“…Equation 3 is integral along the line-of-sight, dl. For a given spherical pressure profile, P e (r) = n e (r)kT e (r) the y signal for a cluster projected on the sky is, We emphasize that this is a straw-person experimental design for CMB Stage-4, for example the frequency bands for CMB Stage- 4 have not yet been determined. These particular bands were chosen to cover the main atmospheric windows around the peak CMB and tSZ sensitivity with extra high and low frequency bands for potential foreground cleaning.…”

Section: Methodsmentioning

confidence: 99%

“…While not critical for the science targets, we show how much the addition of DESI can improve our constraints. The Fisher formalism for CMB and BAO and the experimental configurations for Planck and DESI follow those used in [4].…”

Section: Parameter Fiducial Step Prior ωChmentioning

confidence: 99%

Fundamental physics from future weak-lensing calibrated Sunyaev-Zel’dovich galaxy cluster counts

2017

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Future high-resolution measurements of the cosmic microwave background (CMB) will produce catalogs of tens of thousands of galaxy clusters through the thermal Sunyaev-Zel'dovich (tSZ) effect. We forecast how well different configurations of a CMB Stage-4 experiment can constrain cosmological parameters, in particular the amplitude of structure as a function of redshift σ8(z), the sum of neutrino masses Σmν , and the dark energy equation of state w(z). A key element of this effort is calibrating the tSZ scaling relation by measuring the lensing signal around clusters. We examine how the mass calibration from future optical surveys like the Large Synoptic Survey (LSST) compares with a purely internal calibration using lensing of the CMB itself. We find that, due to its high-redshift leverage, internal calibration gives constraints on cosmological parameters comparable to the optical calibration, and can be used as a cross-check of systematics in the optical measurement. We also show that in contrast to the constraints using the CMB lensing power spectrum, lensing-calibrated tSZ cluster counts can detect a minimal Σmν at the 3-5σ level even when the dark energy equation of state is freed up.

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Towards a cosmological neutrino mass detection

Cited by 225 publications

References 79 publications

Global constraints on absolute neutrino masses and their ordering

Global constraints on absolute neutrino masses and their ordering

Bicep2/KECK ARRAY VIII: MEASUREMENT OF GRAVITATIONAL LENSING FROM LARGE-SCALE B-MODE POLARIZATION

Fundamental physics from future weak-lensing calibrated Sunyaev-Zel’dovich galaxy cluster counts

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