The current landscape of neutrino physics · Albright,Dueck,Rodejohann 1004.2798 Gflavor Deviation...
Transcript of The current landscape of neutrino physics · Albright,Dueck,Rodejohann 1004.2798 Gflavor Deviation...
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The current landscape The current landscape
of neutrino physicsof neutrino physicsJosé W F Valle
http://astroparticles.es/
Laboratori Nazionali di Frascati - Infn, Feb 2015
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Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
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Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
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Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
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Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
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Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
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Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
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Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
confirmed
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Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
confirmed
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Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
Needto reviseStandardmodel
confirmed
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The Standard Model up to energies ~ 100 GeV is the most
precise theory of particle interactions we have
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The Standard Model up to energies ~ 100 GeV is the most
precise theory of particle interactions we have
based on gauge principle and the Higgs mechanism
BEH
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With the historic Higgs discovery
SM complete
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With the historic Higgs discovery
complete were it not forneutrinos & cosmology
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With the historic Higgs discovery
complete were it not forneutrinos & cosmology
no neutrino massesno dark matterno baryon asymmetryno inflation
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Neutrinos &Invisible Higgs
http://arxiv.org/abs/1502.01649
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Neutrinos &Invisible Higgs
http://arxiv.org/abs/1502.01649
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Neutrinos &Invisible Higgs
http://arxiv.org/abs/1502.01649
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Neutrinos &Invisible Higgs
http://arxiv.org/abs/1502.01649
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Neutrinos &Invisible Higgs
http://arxiv.org/abs/1502.01649
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Schechter & JV PRD22 (1980) 2227 & PDG
LEPTONIC CKM MATRIXLEPTONIC CKM MATRIX
Rodejohann, JV Phys.Rev. D84 (2011) 073011
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Schechter & JV PRD22 (1980) 2227 & PDG
LEPTONIC CKM MATRIXLEPTONIC CKM MATRIX
Rodejohann, JV Phys.Rev. D84 (2011) 073011
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THE ERA OF LEPTONIC CPV STARTS
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ORIGIN OF NEUTRINO MASS AND SEESAW
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SCALE
MECHANISM
FLAVOR STRUCTURE
ORIGIN OF NEUTRINO MASS AND SEESAW
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SCALE
MECHANISM
FLAVOR STRUCTURE
ORIGIN OF NEUTRINO MASS AND SEESAW
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Minkowski 77 Gellman Ramond Slansky 80 Glashow, Yanagida 79 Mohapatra Senjanovic 80 Lazarides Shafi Weterrich 81 Schechter-Valle, 80 & 82
fermion exchangeTYPE I
ORIGIN OF NEUTRINO MASS AND SEESAW
SCALE
MECHANISM
FLAVOR STRUCTURE
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Schechter-Valle 80/82 Minkowski 77 Gellman Ramond Slansky 80 Glashow, Yanagida 79 Mohapatra Senjanovic 80 Lazarides Shafi Weterrich 81 Schechter-Valle, 80 & 82
fermion exchangeTYPE I
Scalar-exchange TYPE II
ORIGIN OF NEUTRINO MASS AND SEESAW
SCALE
MECHANISM
FLAVOR STRUCTURE
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Schechter-Valle 80/82 Minkowski 77 Gellman Ramond Slansky 80 Glashow, Yanagida 79 Mohapatra Senjanovic 80 Lazarides Shafi Weterrich 81 Schechter-Valle, 80 & 82
fermion exchangeTYPE I
Scalar-exchange TYPE II
ORIGIN OF NEUTRINO MASS AND SEESAW
Number & properties of messengers
SCALE
MECHANISM
FLAVOR STRUCTURELOW-SCALE SEESAW Mohapatra-Valle 86Akhmedov et al PRD53 (1996) 2752 Malinsky et al PRL95(2005)161801 Bazzocchi et al, PRD81 (2010) 051701
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Radiative neutrino mass in 331 scheme
Singer, Valle, Schechter, Phys.Rev. D22 (1980) 738
# generations = # coloursGauge vs Higgs
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Radiative neutrino mass in 331 scheme
Singer, Valle, Schechter, Phys.Rev. D22 (1980) 738
# generations = # coloursGauge vs Higgs
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Radiative neutrino mass in 331 scheme
Singer, Valle, Schechter, Phys.Rev. D22 (1980) 738
# generations = # coloursGauge vs Higgs
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Radiative neutrino mass in 331 scheme
Singer, Valle, Schechter, Phys.Rev. D22 (1980) 738
# generations = # coloursGauge vs Higgs
arXiv:1404.3751many other low-scale neutrino mass schemes ...
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gauge coupling unification : a near miss in SM ?
Boucenna, Fonseca, Gonzalez-Canales, JV arXiv:1411.0566
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gauge coupling unification : a near miss in SM ?
What makes the gauge couplings unify? - A GUT (p decay)
Boucenna, Fonseca, Gonzalez-Canales, JV arXiv:1411.0566
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gauge coupling unification : a near miss in SM ?
What makes the gauge couplings unify? - A GUT (p decay) - SUSY (LHC-II)
Boucenna, Fonseca, Gonzalez-Canales, JV arXiv:1411.0566
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gauge coupling unification : a near miss in SM ?
What makes the gauge couplings unify? - A GUT (p decay) - SUSY (LHC-II) - NEUTRINO PHYSICS
The physics responsible for gauge coupling unification may also induce small neutrino masses
Boucenna, Fonseca, Gonzalez-Canales, JV arXiv:1411.0566
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Order in the chaos?
FLAVOR GUT
Flavor symmetries have the potential of relating Q & L masses ...
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Order in the chaos?
FLAVOR GUT
Flavor symmetries have the potential of relating Q & L masses ...
Morisi et al Phys.Rev. D84 (2011) 036003
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Order in the chaos?
FLAVOR GUT
Morisi et al Phys.Rev. D88 (2013) 036001
King et al Phys. Lett. B 724 (2013) 68
Bonilla et al
Flavor symmetries have the potential of relating Q & L masses ...
Phys.Lett. B742 (2015) 99
Morisi et al Phys.Rev. D84 (2011) 036003
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CHARGED LEPTONS
Sectors are separatedSectors are separatedby an extra Abelian Znby an extra Abelian Zn
FLAVORSYMMETRY
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CHARGED LEPTONS
Sectors are separatedSectors are separatedby an extra Abelian Znby an extra Abelian Zn
Babu-Ma-Valle PLB552 (2003) 207Hirsch et al PRD69 (2004) 093006
A4
FLAVORSYMMETRY
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CHARGED LEPTONS
Sectors are separatedSectors are separatedby an extra Abelian Znby an extra Abelian Zn
Babu-Ma-Valle PLB552 (2003) 207Hirsch et al PRD69 (2004) 093006
A4
FLAVORSYMMETRY
Tri-BiMaximal ansatz Harrison, Perkins, Scott 2000
(CP assummed)
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CHARGED LEPTONS
Sectors are separatedSectors are separatedby an extra Abelian Znby an extra Abelian Zn
A4
Tri-BiMaximal ansatz Harrison, Perkins, Scott 2000
(CP assummed)
Altarelli, Feruglio 2005
FLAVORSYMMETRY
Babu-Ma-Valle PLB552 (2003) 207Hirsch et al PRD69 (2004) 093006
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Gflavor
FLASY2011, 2012,2013, 2014, 2015 Jun29-Jul2
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Gflavor
Deviationof TBM
Ishimori.etal ProgTheor Phys Suppl 183 (2010) 1
Holthausen et al 1212.2411
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change ansatz:
Albright,Dueck,Rodejohann 1004.2798
Gflavor
Deviationof TBM
Ishimori.etal ProgTheor Phys Suppl 183 (2010) 1
Holthausen et al 1212.2411
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change ansatz:
Albright,Dueck,Rodejohann 1004.2798
Gflavor
Deviationof TBM
Abelian Ding, Morisi, JV PRD87 (2013) 1211.6506
Ishimori.etal ProgTheor Phys Suppl 183 (2010) 1
Holthausen et al 1212.2411
Boucenna,M,Tortola, JVPRD86 (2012) 051301
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change ansatz:
Albright,Dueck,Rodejohann 1004.2798
Gflavor
Deviationof TBM
AnarchyDonoghue et al PRD73Hall,Murayama,Weiner,PRLAltarelli, Feruglio,Masina,JHEP
Abelian Ding, Morisi, JV PRD87 (2013) 1211.6506
Ishimori.etal ProgTheor Phys Suppl 183 (2010) 1
Holthausen et al 1212.2411
Boucenna,M,Tortola, JVPRD86 (2012) 051301
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change ansatz:
Albright,Dueck,Rodejohann 1004.2798
Gflavor
Deviationof TBM
AnarchyDonoghue et al PRD73Hall,Murayama,Weiner,PRLAltarelli, Feruglio,Masina,JHEP
Abelian Ding, Morisi, JV PRD87 (2013) 1211.6506
Ishimori.etal ProgTheor Phys Suppl 183 (2010) 1
Holthausen et al 1212.2411
Flavor roadmap Fortsch.Phys. 61 (2013) 466-492
Boucenna,M,Tortola, JVPRD86 (2012) 051301
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arXiv:1305.6774
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arXiv:1305.6774
STRIKING CORRELATION
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OSCILLATION PARAMETER CORRELATIONS
Boucenna et alPhysRevD.86.073008
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OSCILLATION PARAMETER CORRELATIONS
Boucenna et alPhysRevD.86.073008
Dorame et al Nucl Phys B861, 259–270
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OSCILLATION PARAMETER CORRELATIONS
Boucenna et alPhysRevD.86.073008
Dorame et al Nucl Phys B861, 259–270Bonilla et al Phys.Lett. B742 (2015) 99
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Bilarge mixing & Cabibbo angle Boucenna et al, Phys. Rev. D 86, 051301(R)
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Bilarge mixing & Cabibbo angle
reactor seeds solar & atmBoucenna et al, Phys. Rev. D 86, 051301(R)
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Bilarge mixing & Cabibbo angle
reactor seeds solar & atmBoucenna et al, Phys. Rev. D 86, 051301(R)
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Bilarge mixing & Cabibbo angle
reactor seeds solar & atmBoucenna et al, Phys. Rev. D 86, 051301(R)
arXiv:1410.3658
Abelian Flavor Models Ding, et al Phys.Rev. D87 (2013) 053013 Roy, Singh, ..arXiv:1211.7207
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A.S. Barabash arXiv:1104.2714
Neutrinoless Double Beta Decay
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Family symmetry dependent lower bound
A.S. Barabash arXiv:1104.2714
Bonilla et al arXiv:1411.4883
Neutrinoless Double Beta Decay and flavor
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Family symmetry dependent lower bound
A.S. Barabash arXiv:1104.2714
Bonilla et al arXiv:1411.4883
Dorame et alNPB861 (2012) 259-270
PhysRevD.86.056001 King et al Phys. Lett. B 724 (2013) 68
Neutrinoless Double Beta Decay and flavor
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Schechter, JWFV 82Lindner et al JHEP 1106 (2011) 091
A.S. Barabash arXiv:1104.2714
Neutrinoless Double Beta Decay significance
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Neutrinoless Double Beta Decay
Schechter, JWFV 82Lindner et al JHEP 1106 (2011) 091
Short versus longrange and the LHC
A.S. Barabash arXiv:1104.2714
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Neutrinoless Double Beta Decay
Schechter, JWFV 82Lindner et al JHEP 1106 (2011) 091
Short versus longrange and the LHC
A.S. Barabash arXiv:1104.2714
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Neutrinos affect the CMB and large scale structure in the Universe …
BIGBANG
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Neutrinos affect the CMB and large scale structure in the Universe …
are key in the synthesis of light elements
BIGBANG
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Neutrinos affect the CMB and large scale structure in the Universe …
are key in the synthesis of light elements
can “probe” the Universe earlier than photons …
BIGBANG
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Boucenna et al arXiv:1405.2332
type-I seesaw
PRD90 (2014) 055023
SEESAW INFLATION & MAJORON DARK MATTER
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Boucenna et al arXiv:1405.2332
type-I seesaw
PRD90 (2014) 055023
SEESAW INFLATION & MAJORON DARK MATTER
but http://arxiv.org/pdf/1502.00612v1
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DARK MATTER MAJORONS Berezinsky, Valle PLB318 (1993) 360
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DARK MATTER MAJORONS Berezinsky, Valle PLB318 (1993) 360
Lattanzi & Valle, PRL99 (2007) 121301Lattanzi & Valle, PRL99 (2007) 121301
Esteves et al, PRD 82, 073008 (2010)
Bazzocchi & al JCAP 0808 (2008) 013Bazzocchi & al JCAP 0808 (2008) 013
Consistency with CMB
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DARK MATTER MAJORONS Berezinsky, Valle PLB318 (1993) 360
Lattanzi & Valle, PRL99 (2007) 121301Lattanzi & Valle, PRL99 (2007) 121301
Esteves et al, PRD 82, 073008 (2010)
Bazzocchi & al JCAP 0808 (2008) 013Bazzocchi & al JCAP 0808 (2008) 013
Lattanzi et al PRD88 (2013) 063528
Consistency with CMB
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DARK MATTER MAJORONS Berezinsky, Valle PLB318 (1993) 360
Lattanzi & Valle, PRL99 (2007) 121301Lattanzi & Valle, PRL99 (2007) 121301
Esteves et al, PRD 82, 073008 (2010)
Bazzocchi & al JCAP 0808 (2008) 013Bazzocchi & al JCAP 0808 (2008) 013 128
Lattanzi et al PRD88 (2013) 063528
Consistency with CMB
Aristizabal et al arXiv:1405.4706
– Leptogenesis in dynamical seesaw JCAP
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DARK MATTER STABILITY FROM FLAVOUR SYMMETRY
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DARK MATTER STABILITY FROM FLAVOUR SYMMETRY
accidental? Lavoura, Morisi, JV JHEP 1302(2013) 118 unbroken subgroup
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DARK MATTER FROM FLAVOUR SYMMETRY
Z2 PARITY
HIGGS PORTAL DIRECT DETECTION
accidental? Lavoura, Morisi, JV JHEP 1302(2013) 118 unbroken subgroup
Boucenna et al
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ISBN: 978-3-527-41197-9456 pagesFebruary 2015
Thank you !! more at
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Now the back up slides
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Lightest neutralino decay length
De Campos et al Phys.Rev. D86 (2012) 075001
LIGHTEST NEUTRALINO DECAYS: PROBING NEUTRINOS @ LHC
Lightest neutralino decay correlates with atm angle
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decaying Gravitino dark matterdecaying Gravitino dark matter decays suppressed by Planck mass & smallness of m-nu
chosen to fit neutrino osc. data
excluded by gamma line searches @
Egret & Fermi-LAT
relic abundance
+ LHC searches
Restrepo et al PRD85 (2012) 023523 LHCLHC
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Forero, Tortola, JWFV arXiv:1405.7540Oscillations after nu2014
Double Chooz: 467.9 days [arXiv:1406.7763]RENO: 800 days [talk by Seon-Hee Seo@ICHEP2014]Daya Bay: 621 days of data (6AD + 8AD) [Talk by Chao Zhang@ICHEP2014]
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LSP is SNEUTRINO-like
instead of neutralino ..
Arina et al PRL101 (2008) 161802Bazzocchi, Cerdeno, Munoz, J.V., PRD81 (2010) 051701De Romeri, Hirsch, JHEP 1212 (2012) 106
If neutrinos get mass a la Inverse seesaw susy Spectrum can change so …
WIMP DARK MATTER