000159241 001__ 159241
000159241 005__ 20181203022144.0
000159241 0247_ $$2doi$$a10.1103/PhysRevD.80.083506
000159241 02470 $$2ISI$$a000271353700021
000159241 037__ $$aARTICLE
000159241 245__ $$aModel independent constraints on mass-varying neutrino scenarios
000159241 269__ $$a2009
000159241 260__ $$c2009
000159241 336__ $$aJournal Articles
000159241 520__ $$aModels of dark energy in which neutrinos interact with the scalar field supposed to be responsible for the acceleration of the Universe usually imply a variation of the neutrino masses on cosmological time scales. In this work we propose a parametrization for the neutrino mass variation that captures the essentials of those scenarios and allows one to constrain them in a model independent way, that is, without resorting to any particular scalar field model. Using WMAP 5 yr data combined with the matter power spectrum of SDSS and 2dFGRS, the limit on the present value of the neutrino mass is m(0) equivalent to m(nu)(z = 0) < 0.43 (0.28) eV at 95% C.L. for the case in which the neutrino mass was lighter ( heavier) in the past, a result competitive with the ones imposed for standard (i.e., constant mass) neutrinos. Moreover, for the ratio of the mass variation of the neutrino mass Delta m(nu) over the current mass m(0) we found that log[vertical bar Delta m(nu)vertical bar/m(0)] < -1.3 (-2.7) at 95% C.L. for Delta m(nu) < 0 (Delta m(nu) > 0), totally consistent with no mass variation. These stringent bounds on the mass variation are not related to the neutrino freestreaming history which may affect the matter power spectrum on small scales. On the contrary, they are imposed by the fact that any significant transfer of energy between the neutrino and dark energy components would lead to an instability contradicting CMB and large-scale structure data on the largest observable scales.
000159241 6531_ $$aMicrowave Background Anisotropies
000159241 6531_ $$aHubble-Space-Telescope
000159241 6531_ $$aDark Energy
000159241 6531_ $$aPower-Spectrum
000159241 6531_ $$aCosmological Constant
000159241 6531_ $$aAccelerating Universe
000159241 6531_ $$aMatter
000159241 6531_ $$aSupernovae
000159241 700__ $$aFranca, Urbano
000159241 700__ $$aLattanzi, Massimiliano
000159241 700__ $$aLesgourgues, Julien
000159241 700__ $$aPastor, Sergio
000159241 773__ $$j80$$tPhysical Review D$$q-
000159241 909C0 $$xU10077$$0252369$$pSB
000159241 909CO $$pSB$$particle$$ooai:infoscience.tind.io:159241
000159241 917Z8 $$xWOS-2010-11-30
000159241 937__ $$aEPFL-ARTICLE-159241
000159241 973__ $$rREVIEWED$$sPUBLISHED$$aEPFL
000159241 980__ $$aARTICLE