Measuring the Mass Scale of Neutrinos
ν
J. A. Formaggio Massachusetts Institute of Technology Neutrino Oscillations
The Sudbury Neutrino Observatory MINOS Body of Evidence
Super-Kamiokande MINOS KamLAND SNO
The phenomena of neutrino oscillations is now firmly Super-Kamiokande established.
KamLAND Neutrino Oscillations
The Sudbury Neutrino Observatory MINOS sin2 (✓ )=0.0241 0.0025 13 ± Body of Evidence Reactor & Long Baseline
2 sin (✓12Super-Kamiokande)=0.307 0.016 2 ± 5 2 MINOS m =(7.54 0.26) 10 eV 12 ± ⇥ KamLAND SNO Solar
2 sin (✓23)=0.386 0.022 2 ± 3 2 The phenomena of m =(2.43 0.09) 10 eV 23 ± ⇥ neutrino oscillations is now firmly Super-Kamiokande established. Atmospheric
Camilieri, Lisi, WilkersonKamLAND Ann. Rev. 57 (2008). Fogli et al, arXiv:1205.5254 (hep-ph) More Questions
What We Don’t Know
(1) What is the absolute scale of neutrinos?
(2) What is the mass hierarchy?
(3) What is the nature of neutrino mass? More Questions
What We Don’t Know
(1) What is the absolute scale of neutrinos?
(2) What is the mass hierarchy?
(3) What is the nature of neutrino mass? More Questions
What We Don’t Know
(1) What is the absolute scale of neutrinos?
(2) What is the mass hierarchy?
(3) What is the nature of neutrino mass? Normal? Inverted? More Questions
What We Don’t Know
(1) What is the absolute scale of neutrinos?
(2) What is the mass hierarchy?
(3) What is the nature of neutrino mass?
Dirac Majorana? Just cold dark matter matter dark cold Just Neutrino Masses Newfrom Frontiers Cosmology
• Cosmology looks at the sum of neutrino masses ➙
(gravitational effect) withmass neutrino matter dark Cold
n i m ,i = = critical critical Large Scale Structure The Strategy Galaxy Surveys (a naive view) WMAP Temperature Map
Weak lensing
CMB, Polarization
Surveys (galaxy, weak)
Lyman α
Max Tegmark, 2005 CMB Polarization Lyman α Current Limits
• Limits for neutrino masses depend in part on:
Which data is used, and... • Komatsu et al 2010 • ...what assumptions are made.
Set w = -1 w ≠ -1
WMAP 7 only ∑ mν < 1.3 eV ∑ mν < 1.4 eV
WMAP7 + BAO ∑ mν < 0.58 eV ∑ mν < 1.3 eV + H0
WMAP7 + BAO ∑ mν < 0.7 eV ∑ mν < 0.9 eV + SN Current Limits
• Limits for neutrino masses depend in part on:
Which data is used, and... • Komatsu et al 2010 • ...what assumptions are made. WMAP Alone
WMAP + H0 + BAO Set w = -1 w ≠ -1
Gonzales- Garcia WMAP 7 only ∑ mν < 1.3 eV ∑ mν < 1.4 eV
arXiv: WMAP7 + BAO 1006.3795 ∑ mν < 0.58 eV ∑ mν < 1.3 eV + H0 v2
WMAP7 + BAO (and many ∑ mν < 0.7 eV ∑ mν < 0.9 eV + SN others) Current Limits
• Limits for neutrino masses depend in part on:
Which data is used, and... • Komatsu et al 2010 • ...what assumptions are made. WMAP Alone
WMAP + H0 + BAO Set w = -1 w ≠ -1
Gonzales- Garcia WMAP 7 only ∑ mν < 1.3 eV ∑ mν < 1.4 eV
arXiv: WMAP7 + BAO 1006.3795 ∑ mν < 0.58 eV ∑ mν < 1.3 eV + H0 v2
WMAP7 + BAO (and many ∑ mν < 0.7 eV ∑ mν < 0.9 eV + SN others) • Planck alone can push PLANCK neutrino limits down 1 eV.
• Host of new experiments coming to the forefront can push even lower.
PLANCK
WMAP PLANCK Systematic Effects Nonlinearities Moving • As precision demands Forward... moves to 1%, non-linear effects, degeneracies, baryons, etc. all begin to play a role.
• Numerical simulations and Moving to the semi-analytical techniques normal hierarchy used to address. Y. Y. Y. Wong, 2010 scale now requires 1% precision on the power spectrum. Degeneracies Baryon Effects S. Hannestad Phys. Rev. Lett 95 221301