Relativistic bias in neutrino cosmologies

Fidler, Christian; Sujata, Nils; Archidiacono, Maria

doi:10.1088/1475-7516/2019/06/035

Cited by 11 publications

(11 citation statements)

References 31 publications

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“…Anyhow, Refs. [56,57] have recently demonstrated that even neutrino bias is not sensitive to the specific mass hierarchy (see however Ref. [58]).…”

Section: Changes To the Lss Observables -Galaxy Clustering And Weak L...mentioning

confidence: 99%

What will it take to measure individual neutrino mass states using cosmology?

Archidiacono¹,

Hannestad²,

Lesgourgues³

2020

Preprint

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We study the impact of assumptions made about the neutrino mass ordering on cosmological parameter estimation with the purpose of understanding whether in the future it will be possible to infer the specific neutrino mass distribution from cosmological data. We find that although the commonly used assumption of a degenerate neutrino hierarchy is manifestly wrong and leads to changes in cosmological observables such as the cosmic microwave background and large scale structure compared to the correct (normal or inverted) neutrino hierarchy, the induced changes are so small that even with extremely optimistic assumptions about future data they will remain undetectable. We are thus able to conclude that while cosmology can probe the neutrino contribution to the cosmic energy density extremely precisely (and hence provide a detection of a non-zero total neutrino mass at high significance), it will not be possible to directly measure the individual neutrino masses.

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“…Anyhow, Refs. [56,57] have recently demonstrated that even neutrino bias is not sensitive to the specific mass hierarchy (see however Ref. [58]).…”

Section: Changes To the Lss Observables -Galaxy Clustering And Weak L...mentioning

confidence: 99%

What will it take to measure individual neutrino mass states using cosmology?

Archidiacono¹,

Hannestad²,

Lesgourgues³

2020

Preprint

Self Cite

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show abstract

“…from Euclid [230] or DESI [231]. We also stress that the scale-dependent bias we are considering here is relevant on small scales (large k), and is totally distinct from the spurious scale-dependence studied by some of us in [232], appearing on large scales (small k) in the presence of massive neutrinos if the bias itself is not correctly defined (see also [201,203,233,234]). The rest of this work is then structured as follows.…”

Section: Introductionmentioning

confidence: 70%

“…Nonetheless, this distinction is not important given the sensitivity of current galaxy clustering data, and will only become relevant with upcoming data (e.g. from Euclid or DESI), as discussed for instance in [201,203,[232][233][234].…”

Section: Galaxy Biasmentioning

confidence: 99%

Updated neutrino mass constraints from galaxy clustering and CMB lensing-galaxy cross-correlation measurements

Tanseri,

Hagstotz,

Vagnozzi

et al. 2022

Preprint

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We revisit cosmological constraints on the sum of the neutrino masses Σm ν from a combination of full-shape BOSS galaxy clustering [P (k)] data and measurements of the crosscorrelation between Planck Cosmic Microwave Background (CMB) lensing convergence and BOSS galaxy overdensity maps [C κg ], using a simple but theoretically motivated model for the scale-dependent galaxy bias in auto-and cross-correlation measurements. We improve upon earlier related work in several respects, particularly through a more accurate treatment of the correlation and covariance between P (k) and C κg measurements. When combining these measurements with Planck CMB data, we find a 95% confidence level upper limit of Σm ν < 0.14 eV, while slightly weaker limits are obtained when including small-scale ACTPol CMB data, in agreement with our expectations. We confirm earlier findings that (once combined with CMB data) the full-shape information content is comparable to the geometrical information content in the reconstructed BAO peaks given the precision of current galaxy clustering data, discuss the physical significance of our inferred bias and shot noise parameters, and perform a number of robustness tests on our underlying model. While the inclusion of C κg measurements does not currently appear to lead to substantial improvements in the resulting Σm ν constraints, we expect the converse to be true for near-future galaxy clustering measurements, whose shape information content will eventually supersede the geometrical one.

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“…(2.8) [26,29,30] that will therefore be scale-dependent. The analytical calculation of [26,31,50], as well as the results from N-body simulations [30] indicate that b ν O(1)f ν and is only important on linear scales k ≤ 0.01 h/Mpc. Being so small, this form of scale-dependent bias is not expected to add much in terms of constraining power on massive neutrinos.…”

Section: Scale-dependent Effects From Massive Neutrinosmentioning

confidence: 83%

Weighing neutrinos with the halo environment

Banerjee,

Castorina,

Villaescusa-Navarro

et al. 2019

Preprint

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Nonlinear objects like halos and voids exhibit a scale-dependent bias on linear scales in massive neutrino cosmologies. The shape of this scale-dependent bias is a unique signature of the neutrino masses, but the amplitude of the signal is generally small, of the order of f ν , the contribution of neutrinos to the total matter content ( 1%). In this paper, we demonstrate for the first time how the strength of this signal can be substantially enhanced by using information about the halo environment at a range of scales. This enhancement is achieved by using certain combinations of the large scale Cold Dark Matter and total matter environments of halos, both of which are measurable from galaxy clustering and weak lensing surveys.

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Relativistic bias in neutrino cosmologies

Cited by 11 publications

References 31 publications

What will it take to measure individual neutrino mass states using cosmology?

What will it take to measure individual neutrino mass states using cosmology?

Updated neutrino mass constraints from galaxy clustering and CMB lensing-galaxy cross-correlation measurements

Weighing neutrinos with the halo environment

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