Testable Scenarios for the origin of neutrino masses & Baryon asymmetry Jacobo López-Pavón IFT UAM-CSIC January 21, 2019 Outline ● What we know/don’t know. ● Leptogenesis and Seesaw Model. ● Testable Leptogenesis. Hernandez, Kekic, JLP, Racker, Rius 1508.03676; Hernandez, Kekic, JLP, Racker, Salvado 1606.06719 ● Flavor structure & CP violation in minimal model. Caputo, Hernandez, Kekic, JLP, Salvado 1611.05000 Caputo, Hernandez, JLP, Salvado 1704.08721 ● Conclusions What we know in the neutrino sector What we know. Atmospheric sector Interference/Reactor Solar sector What we know. Atmospheric sector Interference/Reactor Solar sector (1s) Esteban, Gonzalez-Garcia, Hernandez-Cabezudo, Maltoni, Schwetz 1811.05487 http://www.nu-fit.org/ What we know. Atmospheric sector Interference/Reactor Solar sector (1s) Esteban, Gonzalez-Garcia, Hernandez-Cabezudo, Maltoni, Schwetz 1811.05487 http://www.nu-fit.org/ What we know. Atmospheric sector Interference/Reactor Solar sector (1s) Esteban, Gonzalez-Garcia, Hernandez-Cabezudo, Maltoni, Schwetz 1811.05487 http://www.nu-fit.org/ What we know. ● Recent results from T2K and NOvA excluded at 2s What we still do not know in the neutrino sector What we don’t know. CP violation in the lepton sector ? Fukugita, Yanagida 1986 Essential in order to explain the Baryon asymmetry of the universe via Leptogenesis. See for instance: King et al 1402.4271 Altarelli et al 1205.5133, 1002.0211 ? The Octant: . Very relevant for the flavour puzzle. Neutrino ordering ( sign of ) ? Normal Inverted Ordering Ordering (NO) (IO) What we don’t know. CP violation in the lepton sector ? Fukugita, Yanagida 1986 Essential in order to explain the Baryon asymmetry of the universe via Leptogenesis. See for instance: King et al 1402.4271 Altarelli et al 1205.5133, 1002.0211 ? The Octant: . Very relevant for the flavour puzzle. Neutrino ordering ( sign of ) ? Extremely relevant input for other observables as decay Normal Inverted Ordering Ordering Absolute neutrino mass scale (NO) (IO) ? Cosmological probes, Tritium beta decay (KATRIN) ? Dirac vs Majorana: decay mixing mass of propagating neutrino Baryon asymmetry ? Baryon asymmetry ● Observed universe mainly made out of matter. ● Reasonable assumption: after Big-Bang same amount of matter and antimatter generated. ● The observed baryon asymmetry is quoted in terms of the abundance (number-density asymmetry of baryons normalized to the entropy density): How can this matter asymmetry of our Universe be generated? Sakharov conditions ● In order to generate the baryon asymmetry the following conditions should be satisfied: Baryon number violation 1 If baryon asymmetry is conserved, no baryon number can be generated Sakharov conditions ● In order to generate the baryon asymmetry the following conditions should be satisfied: Baryon number violation 1 If baryon asymmetry is conserved, no baryon number can be generated OK in Sphalerons the SM @T 140Gev Sakharov conditions ● In order to generate the baryon asymmetry the following conditions should be satisfied: C and CP violation 2 If C or CP are conserved: Sakharov conditions ● In order to generate the baryon asymmetry the following conditions should be satisfied: C and CP violation 2 If C or CP are conserved: Exist in the SM There is CP violation in the quark sector Sakharov conditions ● In order to generate the baryon asymmetry the following conditions should be satisfied: C and CP violation 2 If C or CP are conserved: Exist Jarlskog in the invariant SM too small There is CP violation Not enough CP violation in the quark sector in SM !! Gavela, Hernandez Orloff, Pene, Quimbay 1994 Sakharov conditions ● In order to generate the baryon asymmetry the following conditions should be satisfied: Departure from thermal equilibrium 3 Production/destruction rates of Baryons are equal in thermal equilibrium: Sakharov conditions ● In order to generate the baryon asymmetry the following conditions should be satisfied: Departure from thermal equilibrium 3 Production/destruction rates of Baryons are equal in thermal equilibrium: Exist in the SM Due to Hubble expansion of the universe Sakharov conditions ● In order to generate the baryon asymmetry the following conditions should be satisfied: Departure from thermal equilibrium 3 Production/destruction rates of Baryons are equal in thermal equilibrium: Exist Deviation in the too small SM Due to Hubble expansion Not enough deviation from of the universe thermal equilibrium in the SM!! Kajantie, Laine, Rummukainen, Shaposhnikov, 1996 Observed Baryon asymmetry can not be generated in the SM Gavela, Hernandez Orloff, Pene, Quimbay 1994 Leptogenesis Neutrino Baryon Masses Asymmetry Why are neutrinos so light? Seesaw Model Simplest extension of SM able to account for neutrino masses. Consists in the addition of heavy fermion singlets ( ) to the SM field content: New Physics Scale Minkowski 77; Gell-Mann, Ramond, Slansky 79 Yanagida 79; Mohapatra, Senjanovic 80. Seesaw Model Simplest extension of SM able to account for neutrino masses. Consists in the addition of heavy fermion singlets ( ) to the SM field content: Seesaw Model Simplest extension of SM able to account for neutrino masses. Consists in the addition of heavy fermion singlets ( ) to the SM field content: Interaction with SM particles via Yukawa coupling Seesaw Model Simplest extension of SM able to account for neutrino masses. Consists in the addition of heavy fermion singlets ( ) to the SM field content: Majorana mass Interaction with SM particles term via Yukawa coupling Lepton Number Violation Standard Leptogenesis Right-handed neutrino decays which violate CP and lepton number generate lepton asymmetry before Lepton Baryon Sphalerons Asymmetry Asymmetry L 0 B-L=0 B 0 Temperature Time Sakharov conditions Baryon number violation 1 If baryon asymmetry is conserved, no baryon number can be generated OK in Sphalerons the SM @T 140Gev Sakharov conditions C and CP violation 2 There is CP violation Not enough CP violation in the SM quark sector in SM !! if it enough also exists CP violation in lepton sector Sakharov conditions C and CP violation 2 At one loop: CP asymmetry generated via interference effects Dependence on leptonic CP phases ● It is encoded in the Yukawa couplings: ● Generation of light neutrino masses imposes constraints on Yukawa couplings from neutrino oscillation data Dependence on leptonic CP phases ● It is encoded in the Yukawa couplings: Casas-Ibarra Light Sector Heavy Sector ● Majorana phases ● Complex orthogonal matrix (experimentally challenging) # of extra CP phases ● Dirac CP phase 3 (accessible via neutrino oscillations) 1 Sakharov conditions Departure from thermal equilibrium 3 out of abundance decoupling equilibrium decay before TEW x equilibrium distribution Testable Leptogenesis Neutrino Baryon Masses Asymmetry Testability The New Physics Scale Vanilla Leptogenesis meV eV keV MeV GeV TeV not testable GUTs The New Physics Scale Vanilla Cosmology Leptogenesis meV eV keV MeV GeV TeV not testable GUTs P. Hernandez, M. Kekic, JLP 1311.2614;1406.2961 The New Physics Scale Vanilla Cosmology Leptogenesis meV eV keV MeV GeV TeV not testable GUTs ● decay ● Leptogenesis ● Resonant LFV, SHiP, LHC via Oscillations Leptogenesis FCC. M=0.1-100GeV M>100GeV Akhmedov, Rubakov, Smirnov (ARS) Pilaftsis Asaka, Shaposnikov (AS) The New Physics Scale Vanilla Cosmology Leptogenesis meV eV keV MeV GeV TeV not testable GUTs ● decay ● Leptogenesis ● Resonant LFV, SHiP, LHC via Oscillations Leptogenesis FCC. M=0.1-100GeV M>100GeV Akhmedov, Rubakov, Smirnov (ARS) Pilaftsis Asaka, Shaposnikov (AS) Low Scale Leptogenesis (ARS) abundance CP asymmetry generated through NR oscillations deviation from equilibrium before TEW equilibrium distribution sphalerons Kinematic Equations We have computed the equations for the density matrix in the Raffelt- Sigl formalism ● Fermi-Dirac or Bose-Einstein statistics is kept throughout ● Collision terms include 2 ↔ 2 scatterings at tree level with top quarks and gauge bosons, as well as 1 ↔ 2 scatterings, including the resummation of scatterings mediated by soft gauge bosons ● Leptonic chemical potentials are kept in all collision terms to linear order ● Include spectator processes Solved using SQuIDS Arguelles Delgado, Salvado, Weaver 2015 https://github.com/jsalvado/SQuIDS Full parameter space exploration NR=2 Bayesian posterior probabilities (using nested sampling Montecarlo MultiNest) Casas-Ibarra Parameters of the model Fixed by neutrino Free oscillation experiments parameters Leptogenesis in Minimal Model NR=2 Non very degenerate solutions PRESENT BOUND FUTURE SENSITIVITY Inverted light neutrino ordering (IH) Hernandez, Kekic, JLP, Racker, Salvado 2016 arXiv:1606.06719 Leptogenesis in Minimal Model NR=2 Non very degenerate solutions PRESENT BOUND FUTURE SENSITIVITY Inverted light neutrino ordering (IH) Hernandez, Kekic, JLP, Racker, Salvado 2016 arXiv:1606.06719 Leptogenesis in Minimal Model NR=2 Non very degenerate solutions PRESENT BOUND FUTURE SENSITIVITY Inverted light neutrino ordering (IH) Hernandez, Kekic, JLP, Racker, Salvado 2016 arXiv:1606.06719 Leptogenesis in Minimal Model NR=2 SHiP DUNE Inverted light neutrino ordering Hernandez, Kekic, JLP, Racker, Salvado 2016 arXiv:1606.06719 Can we experimentally determine Baryon asymmetry generated in minimal model ? Predicting YB in minimal model NR=2 ● Baryon asymmetry depends on all the unknown parameters ● SHiP sensitivity Hernandez, Kekic, JLP, Racker, Salvado 2016 Predicting YB in minimal model NR=2 ● Baryon asymmetry depends on all the unknown