Prediction for the neutrino mass in the KATRIN experiment from lensing by the galaxy cluster A1689

Nieuwenhuizen, Th. M.; Morandi, Andrea

doi:10.48550/arxiv.1103.6270

Cited by 4 publications

(6 citation statements)

References 17 publications

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“…This approach has been followed up whenever new data became available. In [50] we apply the model to SL data by [51] and X-ray data by [52], confirming the result. In [45] we adopt the galactic matter profile of [53], to find that neutrinos perform better (χ 2 /ν ∼ 0.7) than the NFW profile (χ 2 /ν ∼ 2.2).…”

Section: The Galaxy Cluster Abell 1689supporting

confidence: 75%

“…1 expose that Σ does not decay fast for r > 300 kpc. Hence our previous fits [49,50,45] with a large chemical potential µ and fast decay of ρ ν (r) do not apply. But this turns out to be a blessing: isothermal fermions can produce a good fit to the data including the tails.…”

Section: Neutrino Modelmentioning

confidence: 95%

“…This exceeds the 1.45±0.03 of [49], the 1.55±0.04 of [50] and the 1.51±0.04 eV of [45]. However, in those works an additional type of dark matter is assumed, and modeled explicitly in Ref.…”

Section: Neutrino Modelmentioning

confidence: 99%

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Dirac neutrino mass from a neutrino dark matter model for the galaxy cluster Abell 1689

Nieuwenhuizen

2015

Preprint

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The dark matter in the galaxy cluster Abell 1689 is modelled as an isothermal sphere of neutrinos. New data on the 2d mass density allow an accurate description of its core and halo. The model has no "missing baryon problem" and beyond 2.1 Mpc the baryons have the cosmic mass abundance. Combination of cluster data with the cosmic dark matter fraction -here supposed to stem from the neutrinos -leads to a solution of the dark matter riddle by left and right handed neutrinos with mass 1.847 ± 0.016 eV/c 2 . The thus far observed absence of neutrinoless double beta decay points to (quasi-) Dirac neutrinos: uncharged electrons with different flavour and mass eigenbasis, as for quarks. Though the cosmic microwave background spectrum is matched up to some 10% accuracy only, the case is not ruled out because the plasma phase of the early Universe may be turbulent. Nothing matters more than dark matter 11 And nothing energises more than dark energy years across, exceeding the theoretical limit of 1.2 billion light years for the largest possible structures expected from the cosmological principle [19]; for the "cosmic train wreck" galaxy cluster Abell 520, which has a central 3− 4 10 13 M ⊙ mass clump with the enormous mass-to-light ratio 800M ⊙ /L R⊙ , it is difficult to explain why weakly interacting DM would have separated itself from the galaxies [20,21,22]; in the cluster Abell 3827 an offset between baryonic and dark mass occurs [23], which is an order of magnitude larger than ΛCDM can explain [24]. Global issues exist as well: the predicted transition for the most massive galaxies to transform from their initial halo assembly at redshifts z = 8 − 4 to the later baryonic evolution seen in star-forming galaxies and quasars is not observed [25]; the galaxy power spectrum deduced from SDSS-III observations fits well to the stretched exponential exp[−(k/k b ) 1/2 ] predicted by turbulence [26].These and further issues [27,28,29] make us reflect on the whole DM riddle. Of course, the most natural source for DM is neutrinos. In ΛCDM they cannot make up the DM due to free streaming: structure formation is hindered when the total mass in the neutrino families exceeds a bound that is maximally 0.72 eV/c 2 [2]. This corresponds to a cosmic mass fraction Ω ν < 1.6%, far below the cosmic dark matter fraction Ω c = 24.2 ± 0.2% 2 . However, there is an argument against this linear structure formation: the Jeans instability is absolute beyond linear perturbations, since any domain of "Jeans-stable" plane waves contains pairs of plane waves which produce at the bilinear level a beat with wavelength inside the Jeans-unstable regime [30]. Hence the plasma may be (weakly) turbulent, produce nonlinear structures like galaxy clusters [31], explain many perplexing observations [27,28] and leave signatures of turbulence in the galaxy distribution [26]. Indeed, the quark-gluon plasma has a low viscosity, which leads to a very large Reynolds number Re ∼ 10 19 for a patch of acoustic horizon size [32,33]. Since this horizon is larger than the...

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Section: The Galaxy Cluster Abell 1689supporting

confidence: 75%

Section: Neutrino Modelmentioning

confidence: 95%

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Dirac neutrino mass from a neutrino dark matter model for the galaxy cluster Abell 1689

Nieuwenhuizen

2015

Preprint

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“…The vanishing of the MZH acceleration at small radii in their figure 1 is perfectly physical while consistent with the finite value of their upper bound. Third, MZH employ A1689 parameters from our paper Nieuwenhuizen (2017), in particular from 2 runs of X-ray data by the Chandra satellite that were introduced by us in Nieuwenhuizen & Morandi (2011). Below we present here the final A1689 Chandra data for the X-ray gas, and notice a calibration error in analysing the previous data sets.…”

Section: Introductionmentioning

confidence: 99%

Modified Gravity and its test on galaxy clusters

Nieuwenhuizen

Morandi

Limousin

2018

Monthly Notices of the Royal Astronomical Society

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The MOdified Gravity (MOG) theory of J. Moffat assumes a massive vector particle which causes a repulsive contribution to the tensor gravitation. For the galaxy cluster A1689 new data for the X-ray gas and the strong lensing properties are presented. Fits to MOG are possible by adjusting the galaxy density profile. However, this appears to work as an effective dark matter component, posing a serious problem for MOG. New gas and strong lensing data for the cluster A1835 support these conclusions and point at a tendency of the gas-alone to overestimate the lensing effects in MOG theory.

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“…In recent years we have made a series of studies for the case of neutrinos as Zwicky DM, specialising to the cluster Abell 1689, for which good lensing and gas data are available [34][35][36] . This leads to a perfect fit without missing baryons The electron density ne in units of 0.001cm −3 from CHANDRA 42 and ROSAT /PSPC 43 .…”

Section: Introductionmentioning

confidence: 99%

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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Prediction for the neutrino mass in the KATRIN experiment from lensing by the galaxy cluster A1689

Cited by 4 publications

References 17 publications

Dirac neutrino mass from a neutrino dark matter model for the galaxy cluster Abell 1689

Dirac neutrino mass from a neutrino dark matter model for the galaxy cluster Abell 1689

Modified Gravity and its test on galaxy clusters

How Zwicky already ruled out modified gravity theories without dark matter

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