The Future of Neutrino Mass Measurements: Terrestrial, Astrophysical, and Cosmological Measurements in the Next Decade. Highlights of the NuMass 2013 Workshop. Milano, Italy, February 4 - 7, 2013

Barker, G.J.; Gastaldo, L.; Formaggio, J.; Engle, J.W.; Lahiri, S.; Gatti, F.; Sorel, M.; Ota, T.; Vissani, F.; Yoshimura, M.; Koster, U.; De Rujula, A.; Biassoni, M.; Lusignoli, M.; Gorla, P.; de Vega, H.J.; Sisti, M.; Wandkowsky, N.

If you experience any problem watching the video, click the download button below

Preprint
Report number	arXiv:1309.7810
Title	The Future of Neutrino Mass Measurements: Terrestrial, Astrophysical, and Cosmological Measurements in the Next Decade. Highlights of the NuMass 2013 Workshop. Milano, Italy, February 4 - 7, 2013
Author(s)	Barker, G.J. (Warwick U.) ; Biassoni, M. (Milan U. ; INFN, Milan Bicocca) ; De Rujula, A. (CERN ; CSIC, Madrid) ; de Vega, H.J. (Paris, LPTHE ; LERMA, Ivry) ; Engle, J.W. (Los Alamos) ; Faverzani, M. (ed.) (Milan U. ; INFN, Milan Bicocca) ; Ferri, E. (ed.) (Milan U. ; INFN, Milan Bicocca) ; Formaggio, J. (MIT) ; Gastaldo, L. (Kirchhoff Inst. Phys.) ; Gatti, F. (Genoa U. ; INFN, Genoa) ; Gorla, P. (Gran Sasso) ; Koster, U. (Laue-Langevin Inst.) ; Lahiri, S. (Saha Inst.) ; Lusignoli, M. (Rome U. ; INFN, Rome) ; Nucciotti, A. (ed.) (Milan U. ; INFN, Milan Bicocca) ; Ota, T. (Saitama U.) ; Sisti, M. (Milan U. ; INFN, Milan Bicocca) ; Sorel, M. (Valencia U., IFIC) ; Terranova, F. (ed.) (Milan U. ; INFN, Milan Bicocca) ; Vissani, F. (Gran Sasso) ; Wandkowsky, N. (KIT, Karlsruhe) ; Yoshimura, M. (Okayama U.)
Publication	2013
Imprint	30 Sep 2013
Number of pages	63
Subject category	Particle Physics - Experiment
Abstract	The third Workshop of the NuMass series ("The Future of Neutrino Mass Measurements: Terrestrial, Astrophysical, and Cosmological Measurements in the Next Decade: NuMass 2013") was held at Dipartimento di Fisica "G. Occhialini, University of Milano-Bicocca in Milano, Italy, on 4-7 February 2013. The goal of this international workshop was to review the status and future of direct and indirect neutrino mass measurements in the laboratory as well as from astrophysical and cosmological observations. This paper collects most of the contributions presented during the Workshop.
Other source	Inspire
Copyright/License	arXiv nonexclusive-distrib. 1.0

$noimgObserved values $ r_h $, velocity dispersion $ v, \; \sqrt{Q_h}, \; \rho(0)$ and $ M_h $ covering from ultracompact galaxies to large spiral galaxies from refs.[4,5]. The phase space density is larger for smaller galaxies, both in mass and size. Notice that the phase space density is obtained from the stars velocity dispersion which is expected to be smaller than the DM velocity dispersion. Therefore, the reported $ Q_h $ are in fact upper bounds to the true values [4].$ $In the left panel we display the galaxy phase-space density $ \hbar^3 \; Q(0)/({\rm keV})^4 $ obtained from the numerical resolution of the Thomas-Fermi eqs. (\ref{pois})-(\ref{den}) for WDM fermions of mass $ m = 1 $ and $ 2 $ keV versus the ordinary logarithm of the product $ \log_{10}\{r_h \; [{\rm pc}^3 \; \rho_0/ M_\odot]^{\frac16} \} $ in parsecs. The red stars $ * $ are the observed values of $ \hbar^3 \; Q(0)/({\rm keV})^4 $ from Table \ref{pgal}. Notice that the observed values $ Q_h $ from the stars' velocity dispersion are in fact upper bounds for the DM $ Q_h $ and therefore the theoretical curve is slightly below them. In the right panel we display the galaxy mass $ (M / M_\odot) \sqrt{M_\odot / [\rho_0 \; {\rm pc}^3]} $ obtained from the numerical resolution of the Thomas-Fermi eqs.(\ref{pois})-(\ref{den}) for WDM fermions of mass $ m = 1 $ and $ 2 $ keV versus the product $ r_h \; [{\rm pc}^3 \; \rho_0/ M_\odot]^{\frac16} $ in parsecs. The red stars $ * $ are the observed values of $ (M / M_\odot) \sqrt{M_\odot / [\rho_0 \; {\rm pc}^3]} $ from Table \ref{pgal}. Notice that the error bars of the observational data are not reported here but they are at least about $ 10-20 \%$.$ $The MH discovery sensitivity of NO$\nu$A alone and combined with T2K (Left) for normal hierarchy and (Right) for inverted hierarchy. `New' NO$\nu$A refers to a new analysis event selection optimised for the measured (large) value of $\theta_{13}$. From [3].$ Show more plots

Back to search

Record created 2013-10-01, last modified 2023-12-13

Registos similares

Fulltext:

PDF

External link:

Preprint

Add to personal basket
Export as BibTeX, MARC, MARCXML, DC, EndNote, NLM, RefWorks

CERN Document Server

Access articles, reports and multimedia content in HEP

Main menu

CERN Accelerating science