ABSOLUTE neutrino mass measurements

1. ABSOLUTE neutrino mass measurements Markus Steidl HQL 2008, Melbourne, 9th June

2. Content • Why measuring ABSOLUTE neutrino mass(es) Status & Perspectives • Cosmology • 0n2b decay • 1n1b decay Complimentarity of Methods

3. Why measuring ABSOLUTE neutrino mass(es)…

4. Why measuring ABSOLUTE neutrino mass(es)… • Quasi-Degenerated Modells vs. Hierarchical Modells • Discrimination for many modell extension of S.M. • Next Generations of experiments have the sensitivity to exclude clearly the degenerated models • Potential to answer DIRAC or MAJORANA (see section Complimenatrity)

5. Why measuring ABSOLUTE neutrino mass(es)… • Past few years a new standard model of cosmology has been established • The precision of data (CMB, LSS, SNIa, …) allows probing particle physics, e.g. neutrino properties PDG2008 • Conversely, cosmology is at a level where unknowns from particle physics can significantly bias estimates of cosmological data

6. Why measuring ABSOLUTE neutrino mass(es)… • Matter Content of Universe • Growth of perturbations FINITE NEUTRINO MASSES SUPPRESS THE MATTER POWER SPECTRUM ON SCALES SMALLER THAN THE FREE-STREAMING LENGTH TRANSITION FROM RADIATION TO MATTER COMPONENT WHEN GETTING NON RELATIVISTIC Hannestad et al. 0.3 eV

7. Sensitivity benchmarks 2 eV • Today‘s reliable, model-independant mass limits • Insignificant contributions to dynamical evolution of universe • Negligible contribution to energy density • Quasi-degenerated models ruled out ~200 meV ~50 meV • Enter region of mass eigenstates in inverted hierarchy • Inverted Hierarchy excluded • Signal in Cosmology should be there • Lab experiments: Positive signal depends on mixing angles and/or Majorana Phases <50 meV

8. Content • Why measuring ABSOLUTE neutrino mass(es) Status & Perspectives • Cosmology • 0n2b decay • 1n1b decay Complimentarity of Methods

9. Cosmological observations Large Scale Structures • Suppression of small scale fluctuations • k>0.1 (h/Mpc) non-linear regime • Bias parameter must be incorporated • Wn degenerated with others parameters • -> Combine fits with other data sets (at best from different epochs) PDG 2007.

10. Cosmological observations CMB WMAP PDG 2007. • Sensitivity on neutrino mass from CMB alone is modest compared to LSS • Incorporation of CMB helps significantly to break degenaricies and improve precision of mulit-parameter fits in cosmological models (Npar>10)

11. Cosmological observations LSS CMB Baryonic Oscillations arXiv:0705.3323v2 [astro-ph]

12. Cosmological observations LSS CMB Baryonic Oscillations Lyman-a forest • Depleted flux -> regions of hydrogen excess • Reconstruction of 1D-mass distribution on scales of few Mpc • Systematic studies ongoing

13. Cosmological observations LSS CMB Baryonic Oscillations • Scatter of CMB photons on gravitational structures • Smears out peaks at high l • Allows reconstruction of mass distribution on small scales Weak Lensing 6° WL included

14. Limits from Cosmology Small Selection LSS Elgaroy et al, PRL 89 (2002) 6 LSS + CMB Sanchez et al., MNRAS, 366 (2006) 189 Hannestad, Raffelt, JCAP 11 (2006) 016 LSS + CMB + BAO LSS + CMB + SN1a Spergel et al. APJ 170 (2007) 377 Pushing Limits: LSS + CMB + BAO + SN1A + Lya Seljak et al., JCAP 10 ,(2006) 014 S.W. Allen et al., MNRAS 346 ,(2003) 593 LSS + CMB+X-ray data

15. The future 31Oct 2008 (?): Launch of Planck satellite: Improved precision on CMB data Weak Lensing in reach

16. The future 31Oct 2008 (?): Launch of Planck satellite: Improved precision on CMB data (2s) + LSS (today) arXiv:hep-ph/0403296v2 (1s ) + LSST survey [arXiv:astro-ph/0312175c [arXiv:astro-ph/0603019] + High Redshift Galaxy Surveys (95% CL) [arXiv:astro-ph/0703031 Distinction between Normal and Inverted Mass hierarchies Spread in derived limits will remain, boundaries will depend on number of free parameters (>10), data sets …

17. The ultimate future dreams Not earlier than 10 years: (Gravitational effects on Galaxy shapes) Other ideas: 21 cm surveys

18. Content • Why measuring ABSOLUTE neutrino mass(es) Status & Perspectives • Cosmology • 0n2bb decay • 1n1b decay Complimentarity of Methods

19. Neutrinoless Double Beta Decay 2b2n well established 100Mo, 82Se, 48 Ca, 76Ge, 116Cd, 136Xe … PRL 95, 182302 (2005) • Neutrino must be massive • Neutrino must be MAJORANA particles

20. Neutrinoless Double Beta Decay arXiv:nucl-th/0305005v1 Shell model • Measurement of half-live: • Additional systematic uncertainity in n-mass due to • difficult accessible nuclear matrix elements. Cancellations due to non-zero CP phases, Possible difference to single Beta masses (see section complimentarity of methods)

21. Reject Backgrounds (Natural impurities, cosmogenics)state of the art: Ge-experiments (goal 10-3 (cts/kg y) • Excellent Energy Resolutions (Reject 2b2n) • High Isotope abundances, large Q-values • 50meV ~ 1 ton scale Measure several isotopes with different techniques

22. Current experiments Claim of evidence (2004) 76Ge -experiments NEMO • Well established technology Under controversial discussion, Next generation of Ge-experiments under way • Source = Detector • Enriched HP Ge-crystals • Bg‘s in region < 0.1 cts/kg/y GERDA (commissioning 2009 Needs 1y meas. time to check ) Vertex • Good energy resolution 8.9 kg y Physical Review D 65, 092007 (2002) • m < 0.33-1.35 eV Nuclear Physics B Proceedings Supplements 100, 309 (2001), hep-ph/0102276 • m < 0.32-1 eV 36 kg y 72 kg y Physics Letters B 586, 198 (2004). • m = 0.24-0.58 eV

23. Selection of experiments (non-Ge) CUORICONO NEMO Vertex @ Modane Laboratory • @ Gran Sasso Lab • 40,7 kg tower of TeO2 Passive isotope on thin foils surrounded by Geiger mode drift cells for electron tracking and plastic scintillatorfor energy measurement. • Bolometric readout at 10 mK • Energy Resolution • Bg: 0.2 c/keV/kg/y mee < 0.7-2.8 eV 100Mo mee < 0.2-0.7 eV Today‘s most sensitive Limits Future: SUPERNEMO • Future: CUORE

24. Future experiments (some of them …) CANDLES III MOON 191 kg CaF2 Start 2009, goal 50 meV Several tons of 100Mo ~ 30 meV SUPERNEMO 100-200 kg Se or Nd ~ 2016: 50-100 meV EXO Large variety on: Detector technologies Isotopes 136Xe (enriched) (1t-10t) 33-5 meV GERDAMAJORANA CUORE Joined effort for 1 t Ge Common attempt to achieve Bg < 0.1 c/t/y ~20meV in 5y live time 741 kg TeO2; start in 2011if Bg<1c/t/y in 5y 14-47 meV + : SNO+, COBRA, KIEV, XMass … Massiveattack on 50 meV scale (exploring inverted hierarchy scale), and/or excluding it

25. Content • Why measuring ABSOLUTE neutrino mass(es) Status & Perspectives • Cosmology • 0n2b decay • 1n1b decay Complimentarity of Methods

26. b-decay phase space determines energy spectrum transition energy E0 = Ee + En (+ recoil corrections) • KINEMATIC MEASUREMENT • DIRECT • MODEL-INDEPENDANT

27. b Bolometers

28. Karlsruhe Tritium Neutrino Experiment

29. KATRIN

30. KATRIN Sensitivity Sensitivity: m<0.2 eV (90% C.L.)

31. Status 1,5 years ago

32. STATUS KATRIN Installation Inner Electrode Status Experiments for systematic error of n-mass measurement (e.g.spectrometer characteristics) start early 2009 May08

33. Content • Why measuring ABSOLUTE neutrino mass(es) Status & Perspectives • Cosmology • 0n2bb decay • 1n1b decay Complimentarity of Methods

34. Complimentarity of Methods In any case • Lab-experiments as prior for multi-dimensional cosmological fits • improving limits and reliability • breaking degeneracies (e.g. w equation of state of dark energy with mn) Elagroy et al., arXiv:0709.4152v2 [astro-ph] Hannestad et al. PRL 95, 221301 (2005) In case of evidence M inconsistent to mee or mb • A Neutrinoless Universe Beacom et al. Phys.Rev.Lett. 93 (2004) 121302 • Mass varying neutrinos e.g. Päs et al. arXiv:astro-ph/0311131v2 mee inconsistent to mb • Majorana or Dirac ? • Access to CP phases in PMNS matrix

35. Summary In all 3 fields expect high significant data within next ~5 years!