Are observations of the galaxy cluster A1689 consistent with a neutrino dark matter scenario?

Nieuwenhuizen, Th. M.; Morandi, Andrea

doi:10.1093/mnras/stt1216

Cited by 13 publications

(43 citation statements)

References 30 publications

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“…Though the number of right handed neutrinos is not fixed in principle, the case N s = 3 has, if not a practical value [8][9][10][11], at least an esthetic one: for each left handed neutrino there is a right handed one, in the way it occurs for charged leptons and quarks. The three families of active left and sterile right handed neutrinos have the flavor 3 vectors 3…”

Section: The General Mass Matrix For 3 Sterile Neutrinosmentioning

confidence: 99%

“…is the Majorana matrix of the 3-neutrino problem; its η i are Dirac phases now 9 . We also introduced…”

Section: Charged and Neutral Currentmentioning

confidence: 99%

“…The only current knowledge of the involved matrix elements lies in (54). 9 A word on nomenclature: The Majorana phases in the matrix D M stem from the 3+0 SνM, without sterile neutrinos. While they become physical Dirac phases in the 3+3 DMνSM, there appear no true 3+3 Majorana phases, so we propose to keep this name for them.…”

Section: Charged and Neutral Currentmentioning

confidence: 99%

“…Normal ordering m 1 < m 2 < m 3 is connected to −∆ 1 = ∆m 2 atm = (2.44 ±0.06) 10 −3 eV 2 [16] and ∆ 2 = −∆ 1 −∆ 3 > 0, while inverse ordering m 3 < m 1 < m 2 leads to ∆ 1 = ∆m 2 atm and ∆ 2 < 0. Cluster lensing puts forward a valuem ∼ 1.5 − 1.9 eV for the absolute scale of the neutrino masses [8][9][10][11].…”

Section: Estimates For the Dirac And Majorana Massesmentioning

confidence: 99%

“…There is also input from cosmology. From the lensing of background galaxies by the large, reasonably relaxed galaxy clusters Abell 1689 [8][9][10] and Abell 1835 [11] there is indication for 3 active and 3 sterile neutrinos with common mass of 1.5-1.9 eV, which act as the cluster dark matter. We shall not dwell here into the many questions raised by and counter-evidence to that possibility, but refer to the discussion and cited articles in these references.…”

Section: Introductionmentioning

confidence: 99%

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The Standard Model of Particle Physics with Diracian Neutrino Sector

Nieuwenhuizen

2019

Symmetry

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The minimally extended standard model of particle physics contains three right handed or sterile neutrinos, coupled to the active ones by a Dirac mass matrix and mutually by a Majorana mass matrix. In the pseudo-Dirac case, the Majorana terms are small and maximal mixing of active and sterile states occurs, which is generally excluded for solar neutrinos. In a "Diracian" limit, the physical masses become pairwise degenerate and the neutrinos attain a Dirac signature. Members of a pair do not oscillate mutually so that their mixing can be undone, and the standard neutrino model follows as a limit. While two Majorana phases become physical Dirac phases and three extra mass parameters occur, a better description of data is offered. Oscillation problems are worked out in vacuum and in matter. With lepton number -1 assigned to the sterile neutrinos, the model still violates lepton number conservation and allows very feeble neutrinoless double beta decay. It supports a sterile neutrino interpretation of Earth-traversing ultra high energy events detected by ANITA.

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Section: The General Mass Matrix For 3 Sterile Neutrinosmentioning

confidence: 99%

“…is the Majorana matrix of the 3-neutrino problem; its η i are Dirac phases now 9 . We also introduced…”

Section: Charged and Neutral Currentmentioning

confidence: 99%

Section: Charged and Neutral Currentmentioning

confidence: 99%

Section: Estimates For the Dirac And Majorana Massesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Standard Model of Particle Physics with Diracian Neutrino Sector

Nieuwenhuizen

2019

Symmetry

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How Zwicky already ruled out modified gravity theories without dark matter

Nieuwenhuizen

2017

Fortschritte der Physik

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Various theories, such as MOND, MOG, Emergent Gravity and f(R) theories avoid dark matter by assuming a change in General Relativity and/or in Newton's law. Galactic rotation curves are typically described well. Here the application to galaxy clusters is considered, focussed on the good lensing and X‐ray data for A1689. As a start, the no‐dark‐matter case is confirmed to work badly: the need for dark matter starts near the cluster centre, where Newton's law is still supposed to be valid. This leads to the conundrum discovered by Zwicky, which is likely only solvable in his way, namely by assuming additional (dark) matter. Neutrinos with eV masses serve well without altering the successes in (dwarf) galaxies.

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The gravitational field of X-COP galaxy clusters

Eckert

Ettori

Pointecouteau

et al. 2022

A&A

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The mass profiles of massive dark matter halos are highly sensitive to the nature of dark matter and potential modifications of the theory of gravity on large scales. The Λ cold dark matter (CDM) paradigm makes strong predictions on the shape of dark matter halos and on the dependence of the shape parameters on halo mass, such that any deviation from the predicted universal shape would have important implications for the fundamental properties of dark matter. Here we use a set of 12 galaxy clusters with available deep X-ray and Sunyaev–Zel’dovich data to constrain the shape of the gravitational field with an unprecedented level of precision over two decades in radius. We introduce a nonparametric framework to reconstruct the shape of the gravitational field under the assumption of hydrostatic equilibrium and compare the resulting mass profiles to the expectations of Navarro–Frenk–White (NFW) and Einasto parametric mass profiles. On average, we find that the NFW profile provides an excellent description of the recovered mass profiles, with deviations of less than 10% over a wide radial range. However, there appears to be more diversity in the shape of individual profiles than can be captured by the NFW model. The average NFW concentration and its scatter agree very well with the prediction of the ΛCDM framework. For a subset of systems, we disentangle the gravitational field into the contribution of baryonic components (gas, brightest cluster galaxy, and satellite galaxies) and that of dark matter. The stellar content dominates the gravitational field inside ∼0.02R500 but is responsible for only 1–2% of the total gravitational field inside R200. The total baryon fraction reaches the cosmic value at R200 and slightly exceeds it beyond this point, possibly indicating a mild level of nonthermal pressure support (10 − 20%) in cluster outskirts. Finally, the relation between observed and baryonic acceleration exhibits a complex shape that strongly departs from the radial acceleration relation in spiral galaxies, which shows that the aforementioned relation does not hold at the galaxy-cluster scale.

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Are observations of the galaxy cluster A1689 consistent with a neutrino dark matter scenario?

Cited by 13 publications

References 30 publications

The Standard Model of Particle Physics with Diracian Neutrino Sector

The Standard Model of Particle Physics with Diracian Neutrino Sector

How Zwicky already ruled out modified gravity theories without dark matter

The gravitational field of X-COP galaxy clusters

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