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002242538 005__ 20240508051230.0
002242538 0248_ $$aoai:cds.cern.ch:2242538$$pcerncds:CERN$$pcerncds:CERN:FULLTEXT$$pcerncds:FULLTEXT
002242538 0247_ $$2DOI$$a10.1016/j.physletb.2017.03.014
002242538 035__ $$9arXiv$$aoai:arXiv.org:1701.03097
002242538 035__ $$9Inspire$$aoai:inspirehep.net:1508602$$d2024-05-07T09:00:36Z$$h2024-05-08T02:00:27Z$$mmarcxml$$ttrue$$uhttps://inspirehep.net/api/oai2d
002242538 035__ $$9Inspire$$a1508602
002242538 037__ $$9arXiv$$aarXiv:1701.03097$$castro-ph.HE
002242538 037__ $$aKCL-PH-TH-2017-01
002242538 037__ $$aCERN-TH-2017-007
002242538 041__ $$aeng
002242538 084__ $$2CERN Library$$aTH-2017-007
002242538 100__ $$aBonetti, Luca$$uLPC2E, Orleans$$uOrleans U.$$vObservatoire des Sciences de l'Univers en région Centre, UMS 3116, Université d'Orléans, 1A rue de la Férollerie, Orléans, 45071, France$$vPôle de Physique, Collegium Sciences et Techniques, Université d'Orléans, Rue de Chartres, Orléans, 45100, France$$vLaboratoire de Physique et Chimie de l'Environnement et de l'Espace, UMR 7328, Centre Nationale de la Recherche Scientifique, LPC2E, Campus CNRS, 3A Avenue de la Recherche Scientifique, Orléans, 45071, France
002242538 245__ $$9arXiv$$aFRB 121102 Casts New Light on the Photon Mass
002242538 246__ $$9arXiv$$aFRB 121102 Casts New Light on the Photon Mass
002242538 269__ $$c2017-01-11
002242538 260__ $$c2017-05-10
002242538 300__ $$a4 p
002242538 500__ $$9arXiv$$a9 pages, 1 figure, version to appear in PLB
002242538 520__ $$9Elsevier$$aThe photon mass, mγ , can in principle be constrained using measurements of the dispersion measures (DMs) of fast radio bursts (FRBs), once the FRB redshifts are known. The DM of the repeating FRB 121102 is known to <1% , a host galaxy has now been identified with high confidence, and its redshift, z , has now been determined with high accuracy: z=0.19273(8) . Taking into account the plasma contributions to the DM from the Intergalactic medium (IGM) and the Milky Way, we use the data on FRB 121102 to derive the constraint mγ≲2.2×10−14 eVc−2 ( 3.9×10−50 kg ). Since the plasma and photon mass contributions to DMs have different redshift dependences, they could in principle be distinguished by measurements of more FRB redshifts, enabling the sensitivity to mγ to be improved.
002242538 520__ $$9arXiv$$aThe photon mass, $m_\gamma$, can in principle be constrained using measurements of the dispersion measures (DMs) of fast radio bursts (FRBs), once the FRB redshifts are known. The DM of the repeating FRB 121102 is known to $< 1$\%, a host galaxy has now been identified with high confidence,and its redshift, $z$, has now been determined with high accuracy: $z = 0.19273(8)$. Taking into account the plasma contributions to the DM from the Intergalactic medium (IGM) and the Milky Way, we use the data on FRB 121102 to derive the constraint $m_\gamma \lesssim 2.2 \times 10^{-14}$ eV c$^{-2}$ ($3.9 \times 10^{-50}$ kg). Since the plasma and photon mass contributions to DMs have different redshift dependences, they could in principle be distinguished by measurements of more FRB redshifts, enabling the sensitivity to $m_\gamma$ to be improved.
002242538 540__ $$aarXiv nonexclusive-distrib. 1.0$$barXiv$$uhttp://arxiv.org/licenses/nonexclusive-distrib/1.0/
002242538 540__ $$3preprint$$aCC-BY-4.0
002242538 540__ $$3publication$$aCC-BY-4.0$$fSCOAP3
002242538 542__ $$3preprint$$dCERN$$g2017
002242538 542__ $$3publication$$dThe Author(s)$$g2017
002242538 595__ $$aCERN-TH
002242538 65017 $$2arXiv$$ahep-ph
002242538 65017 $$2SzGeCERN$$aParticle Physics - Phenomenology
002242538 65017 $$2arXiv$$ahep-ex
002242538 65017 $$2SzGeCERN$$aParticle Physics - Experiment
002242538 65017 $$2arXiv$$aastro-ph.CO
002242538 65017 $$2SzGeCERN$$aAstrophysics and Astronomy
002242538 65017 $$2arXiv$$aastro-ph.HE
002242538 65017 $$2SzGeCERN$$aAstrophysics and Astronomy
002242538 690C_ $$aCERN
002242538 690C_ $$aARTICLE
002242538 695__ $$2INSPIRE$$9bibclassify$$aphoton: mass
002242538 695__ $$2INSPIRE$$9bibclassify$$aredshift: dependence
002242538 695__ $$2INSPIRE$$9bibclassify$$adark matter
002242538 695__ $$2INSPIRE$$9bibclassify$$aplasma
002242538 695__ $$2INSPIRE$$9bibclassify$$asensitivity
002242538 695__ $$2INSPIRE$$9bibclassify$$adispersion
002242538 695__ $$2INSPIRE$$9bibclassify$$agalaxy
002242538 695__ $$2INSPIRE$$9bibclassify$$aburst
002242538 700__ $$aEllis, John$$uKing's Coll. London$$uCERN$$vTheoretical Particle Physics and Cosmology Group, Physics Department, King's College London, Strand, London, WC2R 2LS, United Kingdom$$vTheoretical Physics Department, CERN, Genève 23, CH-1211, Switzerland
002242538 700__ $$aMavromatos, Nikolaos E.$$uKing's Coll. London$$uCERN$$vTheoretical Particle Physics and Cosmology Group, Physics Department, King's College London, Strand, London, WC2R 2LS, United Kingdom$$vTheoretical Physics Department, CERN, Genève 23, CH-1211, Switzerland
002242538 700__ $$aSakharov, Alexander S.$$uNew York U.$$uManhattan Coll., Riverdale$$uCERN$$vDepartment of Physics, New York University, 4 Washington Place, New York, NY, 10003, United States$$vPhysics Department, Manhattan College, 4513 Manhattan College Parkway, Riverdale, NY, 10471, United States$$vExperimental Physics Department, CERN, Genève 23, CH-1211, Switzerland
002242538 700__ $$aSarkisyan-Grinbaum, Edward K.$$iINSPIRE-00123290$$uCERN$$uTexas U., Arlington$$vExperimental Physics Department, CERN, Genève 23, CH-1211, Switzerland$$vDepartment of Physics, The University of Texas at Arlington, 502 Yates Street, Box 19059, Arlington, TX, 76019, United States
002242538 700__ $$aSpallicci, Alessandro D. A. M.$$uOrleans U.$$uLPC2E, Orleans$$vLaboratoire de Physique et Chimie de l'Environnement et de l'Espace, UMR 7328, Centre Nationale de la Recherche Scientifique, LPC2E, Campus CNRS, 3A Avenue de la Recherche Scientifique, Orléans, 45071, France$$vObservatoire des Sciences de l'Univers en région Centre, UMS 3116, Université d'Orléans, 1A rue de la Férollerie, Orléans, 45071, France$$vPôle de Physique, Collegium Sciences et Techniques, Université d'Orléans, Rue de Chartres, Orléans, 45100, France
002242538 773__ $$c326-329$$pPhys. Lett. B$$v768$$y2017
002242538 8564_ $$81271829$$s504274$$uhttps://cds.cern.ch/record/2242538/files/arXiv:1701.03097.pdf
002242538 8564_ $$81271828$$s7940$$uhttps://cds.cern.ch/record/2242538/files/dispMeasureMgamma121102.png$$y00000 \it Contributions to the dispersion measure (DM) budget for FRB 121102. The top (green) band represents the experimental measurement of the total DM $= 558.1 \pm 3.3$~pc cm$^{-3}$. The middle (blue) band shows the extragalactic contribution, as obtained by subtracting from the central value of the total DM the galactic contribution DM$_{\rm MW} \equiv$ DM$_{\rm NE2001} + $DM$_{\rm halo} = 218$~pc cm$^{-3}$~\protect\cite{FRB121102redshift}, to which is assigned an estimated uncertainty of 20\%. The bottom (pink) band is obtained by subtracting also the estimated contribution from the intergalactic medium (IGM): DM$_{\rm IGM} \simeq 200$~pc cm$^{-3}$~\protect\cite{FRB121102redshift}, which has an uncertainty of $85$~pc cm$^{-3}$ associated with inhomogeneities in the IGM, and a 1.2\% uncertainty associated with the cosmological parameters (indicated by the narrow magenta band). The outer pink band shows the total uncertainty in the residual DM after subtraction of DM$_{\rm MW}$ and DM$_{\rm IGM}$, with errors added in quadrature. The curved (black) band shows the possible contribution of a non-zero photon mass, $m_\gamma$, also including the uncertainties in cosmological parameters.
002242538 8564_ $$81290249$$s8153$$uhttps://cds.cern.ch/record/2242538/files/dispMeasureMgamma121102_Zerror.png$$y00000 \it Contributions to the dispersion measure (DM) budget for FRB 121102. The top (green) band represents the experimental measurement of the total DM $= 558.1 \pm 3.3$~pc cm$^{-3}$. The middle (blue) band shows the extragalactic contribution, as obtained by subtracting from the central value of the total DM the galactic contribution DM$_{\rm MW} \equiv$ DM$_{\rm NE2001} + $DM$_{\rm halo} = 218$~pc cm$^{-3}$~\protect\cite{FRB121102redshift}, to which is assigned an estimated uncertainty of 20\%. The bottom (pink) band is obtained by subtracting also the estimated contribution from the intergalactic medium (IGM): DM$_{\rm IGM} \simeq 200$~pc cm$^{-3}$~\protect\cite{FRB121102redshift}, which has an uncertainty of $85$~pc cm$^{-3}$ associated with inhomogeneities in the IGM, and a smaller uncertainty associated with the cosmological parameters (indicated by the narrow magenta band). The outer pink band shows the total uncertainty in the residual DM after subtraction of DM$_{\rm MW}$ and DM$_{\rm IGM}$, with errors added in quadrature. The curved (black) band shows the possible contribution of a non-zero photon mass, $m_\gamma$, also including the uncertainties in cosmological parameters and the redshift of FRB 121102.
002242538 8564_ $$81292866$$s813767$$uhttps://cds.cern.ch/record/2242538/files/scoap3-fulltext.pdf$$yArticle from SCOAP3
002242538 960__ $$a13
002242538 980__ $$aARTICLE