absolute neutrino mass measurements

HQL 2008, Melbourne, 9th June www.kit.edu

ABSOLUTE neutrino mass measurementsMarkus Steidl

Content

Why measuring ABSOLUTE neutrino mass(es)

02 decay 11 decayCosmology

Status & Perspectives

Complimentarity of Methods

Why measuring ABSOLUTE neutrino mass(es)…

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)

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

Why measuring ABSOLUTE neutrino mass(es)…

Growth of perturbationsMatter Content of Universe

FINITE NEUTRINO MASSES SUPPRESS THE MATTER POWER SPECTRUM ON SCALES SMALLER THAN THE FREE-STREAMINGLENGTH

TRANSITION FROM RADIATION TO MATTER COMPONENT WHEN GETTING NON RELATIVISTIC

0.3 eV

Hannestad et al.

Sensitivity benchmarks

2 eV2 eV

Insignificant contributions to dynamical evolution of universe

Negligible contribution to energy density

Quasi-degenerated models ruled out

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

Today‘s reliable, model-independant mass limits

~200 meV~200 meV

~50 meV~50 meV

<50 meV<50 meV

Content

Why measuring ABSOLUTE neutrino mass(es)

02 decay 11 decayCosmology

Status & Perspectives

Complimentarity of Methods

Cosmological observations Large Scale Structures

Suppression of small scale fluctuations

k>0.1 (h/Mpc) non-linear regime

Bias parameter must be incorporated

degenerated with others parameters

-> Combine fits with other data sets (at best from different epochs)

PDG 2007.

Cosmological observations CMBWMAP

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)

PD

G 2

007.

Cosmological observations CMBLSS

Baryonic Oscillations

arXiv:0705.3323v2 [astro-ph]

Cosmological observations CMBLSS

Lyman- forest

Baryonic Oscillations

Depleted flux -> regions of hydrogen excess

Reconstruction of 1D-mass distribution on scales of few Mpc

Systematic studies ongoing

Cosmological observations

Weak LensingScatter of CMB photons on gravitational structures

Smears out peaks at high l

Allows reconstruction of mass distribution on small scales

WL included

6°

CMB

Baryonic Oscillations

LSS

Limits from Cosmology Small Selection

LSS eVmi

i 8.1 Elgaroy et al, PRL 89 (2002) 6

eVmi

i 62.0 Hannestad, Raffelt, JCAP 11 (2006) 016LSS + CMB + BAO

LSS + CMB

LSS + CMB + BAO + SN1A + Ly

eVmi

i30.026.056.0

Seljak et al., JCAP 10 ,(2006) 014

Sanchez et al., MNRAS, 366 (2006) 189eVmi

i 2.1

Spergel et al. APJ 170 (2007) 377eVmi

i 66.0LSS + CMB + SN1a

S.W. Allen et al., MNRAS 346 ,(2003) 593 LSS + CMB+X-ray data

eVmi

i 17.0

Pushing Limits:

The future

31Oct 2008 (?): Launch of Planck satellite:

Improved precision on CMB data

Weak Lensing

in reach

The future

31Oct 2008 (?): Launch of Planck satellite:

Improved precision on CMB data

Spread in derived limits will remain, boundaries will depend on number of free parameters (>10), data sets …

+ LSST survey

Distinction between Normal and Inverted Mass hierarchies

[arXiv:astro-ph/0312175c

+ High Redshift Galaxy Surveys

[arXiv:astro-ph/0603019]

[arXiv:astro-ph/0703031

+ LSS (today)arXiv:hep-ph/0403296v2 eVm 2.0

eVm 05.0

eVm 08.0 (95% CL)

(2)

(1 )

The ultimate future dreams

(Gravitational effects onGalaxy shapes)

Not earlier than 10 years:

Other ideas:21 cm surveys

Content

Why measuring ABSOLUTE neutrino mass(es)

02decay 11 decayCosmology

Status & Perspectives

Complimentarity of Methods

Neutrinoless Double Beta Decay

Neutrino must be massive

Neutrino must be MAJORANA particles

22 well established

PR

L 9

5, 1

823

02

(20

05

)

100Mo, 82Se, 48 Ca, 76Ge, 116Cd, 136Xe …

Neutrinoless Double Beta Decay

Measurement of half-live:

Additional systematic uncertainity in -mass due to

difficult accessible nuclear matrix elements.

arXiv:nucl-th/0305005v1

Cancellations due to non-zero CP phases,

Possible difference to single Beta masses (see section complimentarity of methods)

Shell model

Reject Backgrounds (Natural impurities, cosmogenics)state of the art: Ge-experiments (goal 10-3 (cts/kg y)

Excellent Energy Resolutions (Reject 22n)

High Isotope abundances, large Q-values

50meV ~ 1 ton scale

Measure several isotopes with different techniques

Claim of evidence (2004)

Current experiments

NEMO

Vertex

76Ge -experiments

Source = Detector

Enriched HP Ge-crystals

Bg‘s in region < 0.1 cts/kg/y

m < 0.33-1.35 eV 8.9 kg y

Physics Letters B 586, 198 (2004).

m < 0.32-1 eV

m = 0.24-0.58 eV 72 kg y

36 kg y

Under controversial discussion,

Next generation of Ge-experiments under

way

Nuclear Physics B Proceedings Supplements 100, 309(2001), hep-ph/0102276

Physical Review D 65, 092007 (2002)

Good energy resolution

GERDA

(commissioning 2009

Needs 1y meas. time to check )

Well established technology

Selection of experiments (non-Ge)

NEMO

Vertex

Future: SUPERNEMO Future: CUORE

CUORICONO

40,7 kg tower of TeO2

Bolometric readout at 10 mK

Bg: 0.2 c/keV/kg/y

mee < 0.2-0.7 eV

Passive isotope on thin foils surrounded by Geiger mode drift cells for electron tracking and plastic scintillatorfor energy measurement.

@ Modane Laboratory @ Gran Sasso Lab

Today‘s most sensitive

Limits

Energy Resolution

mee < 0.7-2.8 eV 100Mo

Future experiments (some of them …)

GERDAMAJORANA

Joined effort for 1 t GeCommon attempt to achieve Bg < 0.1 c/t/y~20meV in 5y live time

SUPERNEMO

136Xe (enriched) (1t-10t) 33-5 meV

741 kg TeO2;start in 2011if Bg<1c/t/y in 5y14-47 meV

100-200 kg Se or Nd~ 2016: 50-100 meV

Massive attack on 50 meV scale (exploring inverted hierarchy scale),and/or excluding it

Large variety on:

Detector technologies

Isotopes

191 kg CaF2Start 2009, goal 50 meV

+ : SNO+, COBRA, KIEV, XMass …

CUORE

EXO

CANDLES III MOON

Several tons of 100Mo~ 30 meV

Content

Why measuring ABSOLUTE neutrino mass(es)

02 decay 11 decayCosmology

Status & Perspectives

Complimentarity of Methods

phase space determines energy spectrumtransition energy E0 = Ee + E (+ recoil corrections)

KINEMATIC MEASUREMENT• DIRECT• MODEL-INDEPENDANT

-decay

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Bolometers

Karlsruhe Tritium Neutrino Experiment

KATRIN

KATRIN Sensitivity

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

Status

1,5 years ago

Status STATUS KATRIN Installation Inner Electrode

May08

Experiments for systematic error of -mass measurement (e.g.spectrometer characteristics) start early 2009

Content

Why measuring ABSOLUTE neutrino mass(es)

02 decay 11 decayCosmology

Status & Perspectives

Complimentarity of Methods

Complimentarity of Methods

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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 m)

A Neutrinoless Universe

Mass varying neutrinos

Majorana or Dirac ?

Access to CP phases in PMNS matrix

Elagroy et al., arXiv:0709.4152v2 [astro-ph]

Hannestad et al. PRL 95, 221301 (2005)

M inconsistent to mee or m

mee inconsistent to m

In any case

Beacom et al. Phys.Rev.Lett. 93 (2004) 121302

e.g. Päs et al. arXiv:astro-ph/0311131v2

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In case of evidence

Summary

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