Toshihiko Ota Saitama University based on Florian Bonnet, Martin Hirsch, TO, Walter Winter JHEP 1207 (2012) 153 arXiv.1212.3045
Preface If the SM is a low- E effective model of a fundamental theory...
Preface If the SM is a low- E effective model of a fundamental theory... : A typical scale of New physics Effective operators are a typical low- E remnant of New physics
Preface If the SM is a low- E effective model of a fundamental theory... : A typical scale of New physics Effective operators are a typical low- E remnant of New physics Weinberg op.
Preface If the SM is a low- E effective model of a fundamental theory... : A typical scale of New physics Effective operators are a typical low- E remnant of New physics Weinberg op. Four-Fermi
Preface If the SM is a low- E effective model of a fundamental theory... : A typical scale of New physics Effective operators are a typical low- E remnant of New physics Weinberg op. Four-Fermi
Preface If the SM is a low- E effective model of a fundamental theory... : A typical scale of New physics Effective operators are a typical low- E remnant of New physics Weinberg op. Four-Fermi
Preface If the SM is a low- E effective model of a fundamental theory... : A typical scale of New physics Effective operators are a typical low- E remnant of New physics Weinberg op. Four-Fermi Seesaw mech. (@tree)
Preface If the SM is a low- E effective model of a fundamental theory... : A typical scale of New physics Effective operators are a typical low- E remnant of New physics Weinberg op. Four-Fermi Seesaw mech. ? ? ? ? (@tree) What do these eff. ops. suggest to physics at high E scales? Exhaustive bottom-up approach
Preface If the SM is a low- E effective model of a fundamental theory... : A typical scale of New physics Effective operators are a typical low- E remnant of New physics Weinberg op. Four-Fermi Seesaw mech. ? ? ? ? (@tree) This talk! What do these eff. ops. suggest to physics at high E scales? Exhaustive bottom-up approach
Outline New Physics ( d=9 ) contributions in neutrinoless double beta decay (0n2b) Motivation: Why 0n2b? Why dim=9 ops? d=9 ops → half-life time of 0n2b processes “How sensitive 0n2b experiments to d=9 ops?” What do the d=9 ops suggest to TeV scale physics? d=9 ops → decompose them to the fundamental ints. → list the TeV signatures of each completion → The list helps us to discriminate the models Seeking a relation to the models at the TeV scale TeV scale models with LNV → Models for radiative neutrino masses
Outline New Physics ( d=9 ) contributions in neutrinoless double beta decay (0n2b) Motivation: Why 0n2b? Why dim=9 ops? d=9 ops → half-life time of 0n2b processes “How sensitive 0n2b experiments to d=9 ops?” What do the d=9 ops suggest to TeV scale physics? d=9 ops → decompose them to the fundamental ints. → list the TeV signatures of each completion → The list helps us to discriminate the models Seeking a relation to the models at the TeV scale TeV scale models with LNV → Models for radiative neutrino masses
Why 0n2b? Why d=9 op.? Effective neutrino mass In SM+3nu, 0n2b exp.s are sensitive to Effective nu mass Normal hierarchy Inverted hierarchy m0 represents the lightest neutrino mass and are Majorana phases
Why 0n2b? Why d=9 op.? Effective neutrino mass In SM+3nu, 0n2b exp.s are sensitive to Unknown Effective nu mass Normal hierarchy Inverted hierarchy m0 represents the lightest neutrino mass and are Majorana phases Oscillation exp.s told us... e.g., Gonzalez-Garcia Maltoni Salvado Schwetz, JHEP 1212 (2012) 123 w w o o n n k k e e w w , , r r a a f f o o S S
Why 0n2b? Why d=9 op.? Effective neutrino mass In SM+3nu, 0n2b exp.s are sensitive to Unknown Effective nu mass Normal hierarchy Inverted hierarchy m0 represents the lightest neutrino mass and are Majorana phases Oscillation exp.s told us... e.g., Gonzalez-Garcia Maltoni Salvado Schwetz, JHEP 1212 (2012) 123 w w o o n n k k e e w w , , r r a a f f o o S S On the other hand, Cosmological obs.s are sensitive to
Why 0n2b? Why d=9 op.? Effective neutrino mass 0n2b exp.s are sensitive to Cosmological obs.s constrain Effective nu mass Sum of nu masses
Why 0n2b? Why d=9 op.? Effective neutrino mass 0n2b exp.s are sensitive to Cosmological obs.s constrain Effective nu mass Sum of nu masses LSS Massless Nu Massive Nu suppresses the small scale parts CMB smaller scales Theoretical calcs are taken from Phys.Rep 429 (2006) 307 cf. Seto-san's talk Lesgourgues Pastor
Why 0n2b? Why d=9 op.? Effective neutrino mass 0n2b exp.s are sensitive to Cosmological obs.s constrain Effective nu mass Sum of nu masses Obs: Planck, WMAP-9year, and balloons Obs: SDSS, 2dFGRS LSS Massless Nu Massive Nu suppresses the small scale parts CMB smaller scales Theoretical calcs are taken from Phys.Rep 429 (2006) 307 cf. Seto-san's talk Lesgourgues Pastor
Why 0n2b? Why d=9 op.? Effective neutrino mass 0n2b exp.s are sensitive to Cosmological obs.s constrain Effective nu mass Sum of nu masses Standard 3nu parameter space
Why 0n2b? Why d=9 op.? Effective neutrino mass 0n2b exp.s are sensitive to Cosmological obs.s constrain Effective nu mass Sum of nu masses Planck (combined) 1303.5076 WMAP9 (combined) Planck first result 1212.5226 Excluded by 1303.5076 SPT reports non-zero mNu! 1212.6267 Standard 3nu parameter space
Why 0n2b? Why d=9 op.? Effective neutrino mass 0n2b exp.s are sensitive to Cosmological obs.s constrain Effective nu mass Sum of nu masses KamLAND-Zen Planck (combined) PRL110 (2013) 062502 1303.5076 0n2b bounds EXO-200 WMAP9 (combined) Planck first result PRL109 (2012) 032505 1212.5226 Excluded by 1303.5076 GERDA (forthcoming) SPT reports non-zero mNu! 1212.6267 Standard 3nu parameter space
Why 0n2b? Why d=9 op.? Effective neutrino mass 0n2b exp.s are sensitive to Cosmological obs.s constrain Effective nu mass Sum of nu masses KamLAND-Zen Planck (combined) PRL110 (2013) 062502 1303.5076 If 0n2b is discovered!? EXO-200 WMAP9 (combined) Planck first result PRL109 (2012) 032505 1212.5226 Excluded by 1303.5076 GERDA (forthcoming) SPT reports non-zero mNu! 1212.6267 Q: If, in future, they will conflict with each other, what can we learn from them?
d=9 op. in 0n2b 0n2b experiments measure... In SM+3nu, the 0n2b rate is estimated as... 0n2b in Standard Nu Model
d=9 op. in 0n2b 0n2b experiments measure... In SM+3nu, the 0n2b rate is estimated as... 0n2b in Standard Nu Model ~100 MeV A typical momentum of neutrino in nuclei Current exp. limit
d=9 op. in 0n2b 0n2b experiments measure... In SM+3nu, the 0n2b rate is estimated as... 0n2b in Standard Nu Model ~100 MeV A typical momentum of neutrino in nuclei Current exp. limit Sensitive to
d=9 op. in 0n2b 0n2b experiments measure... If we have an additional New Physics contribution to 0n2b... Mediated by something with mass of NP + d=9 0n2b in Standard Nu Model ~100 MeV A typical momentum of neutrino in nuclei Current exp. limit Sensitive to
d=9 op. in 0n2b 0n2b experiments measure... If we have an additional New Physics contribution to 0n2b... Mediated by something with mass of NP + d=9 0n2b in Standard Nu Model ~100 MeV A typical momentum of neutrino in nuclei ! e Current exp. limit g Sensitive to n a r C H L 0n2b exps are sensitive to not only Majorana neutrino mass but also NP at TeV.
d=9 op. in 0n2b Effective ops → half-life time …falls into the following 5 types of effective ops. NP d=9
d=9 op. in 0n2b Effective ops → half-life time …falls into the following 5 types of effective ops. NP d=9 Nice (&compact) Formula to calculate the half-life time: Paes et al. PLB498 (2001) 35 Nuclear matrix elements Phase space factors
d=9 op. in 0n2b Effective ops → half-life time …falls into the following 5 types of effective ops. NP d=9 Nice (&compact) Formula to calculate the half-life time: Paes et al. PLB498 (2001) 35 Nuclear matrix elements Phase space factors Q: What is the high E (TeV) origin of these d=9 effective ops? d=9 ops. High E completions 0nu2b-LHC complementarity bottom-up
Outline New Physics ( d=9 ) contributions in neutrinoless double beta decay (0n2b) Motivation: Why 0n2b? Why dim=9 ops? d=9 ops → half-life time of 0n2b processes “How sensitive 0n2b experiments to d=9 ops?” What do the d=9 ops suggest to TeV scale physics? d=9 ops → decompose them to the fundamental ints. → list the TeV signatures of each completion → The list helps us to discriminate the models Seeking a relation to the models at the TeV scale TeV scale models with LNV → Models for radiative neutrino masses
Decomposition Effective ops → High E completions High E completion: We focus on tree-level decompositions NP d=9
Decomposition Effective ops → High E completions High E completion: We focus on tree-level decompositions Signature @ low E 0n2b P N s i h C t H f o L NP n @ i g i e r l O b d=9 a t s e t @Tree
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