View
45
Download
2
Category
Tags:
Preview:
DESCRIPTION
ABSOLUTE neutrino mass measurements. Markus Steidl. Content. Why measuring ABSOLUTE neutrino mass(es). Status & Perspectives. Cosmology. 0 n 2 b decay. 1 n 1 b decay. Complimentarity of Methods. Why measuring ABSOLUTE neutrino mass(es)…. Why measuring ABSOLUTE neutrino mass(es)…. - PowerPoint PPT Presentation
Citation preview
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
222i
iei mUm
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
i
ii
eiee meUm i2 i
imM
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
222i
iei mUm
In case of evidence
Summary
i
imM
i
ii
eiee meUm i2
222i
iei mUm
In all 3 fields expect high significant data within next ~5 years!
Recommended