A. Yu. Smirnov International Centre for Theoretical Physics, Trieste, Italy Latsis Symposium 2013,...

A. Yu. SmirnovInternational Centre for Theoretical Physics, Trieste, Italy

Latsis Symposium 2013 , ``Nature at the Energy Frontiers’’ ETH Zurich, June 3 – 6, 2013

Neutrinos and LHC

Smallness is related to existence of new physics at high energy scales

Mnew ~

(VEW ) 2

mn

GUT scaleLeptogenesis

Studying neutrino mass and mixing

probe of new

physics at these

scales

TeV scale mechanisms of neutrino mass generation ?

Atmospheric neutrinos in Ice Cube E = 4 102TeV

~ 1010 - 1016 GeV s = (1 TeV )2

Cosmic neutrinos ( ?) with

E ~ 103 TeV

Discovery of the 1-3 mixing

All well established/confirmed results are described by

Discovery of

cosmic neutrinos

of high energies ?

Reactor, Galllium

LSND, MiniBooNE

New solar neutrino anomaly

Additional

radiation in

the Universe

Connected ?

1 eV sterile neutrino: not a small perturbation of the 3n picture

- Mass hierarchy

- CP violation

- absolute scale

- nature

(Majorana?)Theory beyondWeinberg operator?

January 2012

August 2012

M.G Aarsten, et al. arXiv:1304.5356 [astro-ph.HE]

E = 1.14 +/- 0.17 PeV

E = 1.04 +/- 0.16 PeV

Atmospheric neutrino background: 0.082 +/- 0.004 (stat) +0.041/–0.057(syst.)p-value 2.9 10-2 (2.8s)``Hint’’ of cosmic neutrinos or Excess at lower energies 0.02 – 0.3 PeV 28 events (7 with muons) are observed ~ ~ 11 expected

New physics with atmospheric neutrinos

Centers of two cascades

MSW-effect

Oscillations

Can be resonantly enhanced in matter

Parametric efects

In wide energy range: from 0.3 MeV to 30 GeVconfirming standard oscillation picture with standard dispersion relations

Daya Bay

MINOS

KAMLAND

15 years after discovery: routinely detect oscillation effects

nm nt

ne

n2

n1

MA

SS n1

n2

n3

n3

MA

SS

Dm223Dm2

32

Dm221

Dm221

Inverted mass hierarchyNormal mass hierarchy

?

Dm232 = 2.4 x 10-3 eV2

Dm221 = 7.5 x 10-5 eV2

Two large mixings

(cyclic permutation)

For antineutrinos spectra are

different (distribution of the nm

and nt - flavors in n1 and n2)

due to possible CP-violation

1-3 mixing

Symmetry: TBM?

sin2 q13

0.0 0.010 0.020 0.030 0.040

RENO, 1s

Fogli et al, 1s

T2K 90%

QLC

Double Chooz, 1s

Daya Bay, 1s

- m t breaking

mass ratioGonzalez-Garcia et al, 1s

sin2 q23

0.30 0.35 0.40 0.45 0.50 0.55 0.60 0.65 0.70

MINOS, 1s

SK (NH), 90%

Fogli et al, 1s

SK (IH), 90%

QLC

Gonzalez-Garcia et al, 1s

symmetry

``Naturalness

’’Absence of

Fine tunning

of mass

matrix

Dm21

2 Dm32

2

O(1)

sin2q13

~ ½sin2qCQuark- Lepton ComplementarityGUT, family symmetry

~ ½cos2 2q23

nm - nt – symmetryviolation

The same 1-3 mixing with completely different implications

q13 + q12 = q23

Mixing

anarchy

> 0.025

Self-complementarity

~ ¼ sin2q12sin2q23Analogy

with quark

mixing

relation

q13 = 21/2( /4p -

q23)

1/3 – |Ue2|2 ~ sin2q13

Large scale structure

of the Universe

S m < 0.23 eV (68 % CL)

SDSS

KATRIN

meeff < 2.2 0.2 eV (90%

CL)

Cosmology (Planck BAO)

Oscillations

m > Dm312 > 0.045 eV

m2 m3

Dm21

2 Dm32

2

~ 0.18>

Direct kinematic measurements (future)

NH

Dm21 m1

~ = 1.6 10-

2

Dm212

2 Dm32

2

IH

The weakest hierarchy Strong degeneracy symmetry

mee = Sk Uek2 mk ei ( )f k

x

p

p

n

n

e

e

n mee

W

W

mee = Ue12 m1 + Ue2

2 m2 eia + Ue32 m3

eib76Ge 76Se + e + e Qee = 2039 keV

5 detectors, 71.7 kg yr

mee = (0.29 – 0.35) eV

Heidelberg-Moscow

EXO-200

mee < (0.14 – 0.38) eV

Xe- Observatory136Xe

m1

Heidelberg-Moscow

GERDA II

CUORE

GERDA I

NEMO

GERDA II

Cuoricino

EXO-200

Upper bounds, boxes – uncertainties of NME

S M Bilenky C Giunti arXiv:1203.5250 [hep-ph]

EXO-200: mee < (0.14 – 0.38) eV

H-M: mee = (0.29 – 0.35) eV

KamLAND-Zen

EXO and Kamland-ZenAlmost exclude H-M (interpretation in terms of light Majorana neutrinos

Phase I in absense of signal for 20 kg year: T1/2 > 1.9 1025 yr (90%

CL)

GERmanium Detector Array

3s range: (0.69 – 4.19) 1025 yr

T1/2 = 1.19 1025 yr

Heidelberg- Moscow:

Can confirm but not exclude completely

Blind analysis, the box should be opened now

Phase II: 37.5 kg y: 0.09 – 0.29 eV

Phase III: 1 ton 0.01 eV

In spite of 1-3 mixing determination…

~ 10-9 – 1019 GeV

from symmetry

and hierarchy

far from real understanding this new physics?

anarchyto

Still at the cross-roads

from eV to Planck

Phenomenology: to a large extend elaborated

Discovery of new physics BSM in some other sectors would have …..

Some interesting developments along different linesFrom minimalistic scenario of nuMSM to sophisticated structures at several new scales

P. F. HarrisonD. H. PerkinsW. G. Scott

Utbm = U23(p/4) U12

- maximal 2-3 mixing- zero 1-3 mixing- no CP-violation

Utbm = 2/3 1/3 0- 1/6 1/3 - 1/2 - 1/6 1/3 1/2

n2 is tri-maximally mixed n3 is bi-maximally mixed

- sin2q12 = 1/3

L. Wolfenstein

Uncertainty related to sign of 2-3 mixing: q23 = /4 p - /4 p Symmetry from mixing matrix

In the first approximation

0.15

0.62

0.78

Sn

Mixing appears as a result of different ways of the flavor symmetry breaking in the neutrino and charged lepton (Yukawa) sectors. This leads to different residual symmetries

Gf

Gl GnResidual symmetriesof the mass matrices

Mn Ml 1n

A4T’S4 T7

?T Sn

Symmetry transformatiosin mass bases

Generic symetries which do not depend on values of masses to get TBM

Z2 x Z2

Zm

Sn Mn S nT =

MnIn this framework bounds on mixing can be obtained without explicit model-building

In flavor basis SiU

( UPMNS Si UPMNS

+ T ) p = I

D. Hernandez, A.S.1204.0445

Explicitly

(SiU T) p = I (SiU T) p = (WiU) p = I

The main relation: connects the mixing matrix and generating elements of the group in the mass basis

Equivalent to

Tr ( UPMNS Si UPMNS + T ) = a Tr (WiU) = a

a = Sj lj

ljp = 1

lj - three eigenvalues of WiU

j = 1,2,3

Transformations should be taken in the basis where CC are diagonal

In flavor basis

Also S. F. Ge, D. A. Dicus, W. W. Repko, PRL 108 (2012) 041801

|Ubi|2 = |Ugi|2 |Uai|2 =

For column of the mixing matrix:

1 – a 4 sin2 (pk/m)

k, m, p integers which determine symmetry group

S4

D. Hernandez, A.S.

d = 1030

ka = 0

a = 0

If symmetry transformations Sn depend on specific mass spectrum, Relations include also masses and Majorana CP phases

D. Hernandez, A Y S. 1304.7738 [hep-ph]

sin2 2q23 = sin d = cos k = m2 /m1 = 1

ur , ub , uj , n dr , db , dj , e

urc, ub

c, ujc,

nc

drc, db

c, djc,

ec

RH-neutrino

S

S

S

S

S SS

S

S

S- Enhance mixing- Produce zero order structure- Randomness (if needed)

SS

S

S

SS

S

SS

SSSS

SS

S

S

S

S

Hidden sector

SO(10) GUT + …

High scale mass seesaw

Explains smallness of neutrino mass and difference of q- and l- mixings

Possibly some Hidden sector at GUT - Planck scales

Flavor symmetries at very high scales, above GUT?

Old does not mean wrong

Tests of the low (TeV) -scale mechanisms of neutrino mass generation

R-parity violation

Low scale Seesaw

Of different types

at LHC

RH neutrinos at LHC

Tests of BSM framework which can lead to the neutrino mass generation

Tests of the physics framework SUSY, extraD …

No good motivations

Search for mediators of seesaw, accompanying particles

Radiative mechanisms

lType-Ii

l l j j

x

q

q l

NWR

bi-leptons with the same-sign

SenjanovicKeung

WR*

q

qbb0n

s (jj l) = mN2

No missing energyPeaks at

s (jj ll) = mW

2

Also opposite sign leptons

nn

P.S Bhupal Dev, et al, 1305.0056 [hep-ph]

Mix with active neutrinos

ns

No weak interactions:- singlets of the SM symmetry group

LightRH-components

of neutrinos

may have Majorana masses maximal mixing?

Sov. Phys. JETP 26 984 (1968)

Pisa, 1913

Dear Dr. Alexei Yu. Smirnov, Please pay attention to our upcoming Special Issue on "Research in Sterility" which will be published in the"Advances in Sexual Medicine" , an open access journal. We cordially invite you to submit your paper …

LSND MiniBooNE

Gallex,GNO

SAGE

G.Mention et al, arXiv: 1101.2755P Huber

Dm412 = 1 - 2

eV2

nm

nt

ne

n2

n1

n4

mas

s

Dm231

Dm221

n3

Dm241

ns

P ~ 4|Ue4 |2|Um4 |2

restricted by short baseline exp. BUGEY, CHOOZ, CDHS, NOMAD

LSND/MiniBooNE: vacuum oscillations

With new reactor data:

Dm412 = 1.78

eV2Ue4 = 0.15 Um4 = 0.23

P ~ 4|Ue4|2 (1 - |Ue4|2)

For reactor and source experiments

- additional radiation in the universe- bound from LSS?

( 0.89 eV2)

All positive evidences vs null results

Tension between disappearance data and νμ → νe LSND-MiniBooNE signals

J. Kopp , P. A. N. Machado, M. Maltoni, T. Schwetz, 1303.3011 [hep-ph]

cosmology

0PERA

OPERA, Collaboration 1303.3953 [hep-ex]

Controversialsituation

Neff = 3.30 (95 % CL) + 0.54- 0.51

Neff = 3.30 +/- 0.27 (68% CL)

Inconclusive

Effective number of neutrino species

BBN

Neff = 3.68 (68 % CL) + 0.80- 0.70

Y. I. Izotov and T X Thuan Astrophys J 710 (2010) L67

After Planck

Planck +WP+highL+BAO

Neff = 3.62 (95 % CL) + 0.50- 0.48 Planck +WP+highL +

H0

NESSiE

Neutrino Experiment with Spectrometers in Europe, Charged Current (CC) muon neutrino and antineutrino interactions. two magnetic spectrometers located in two sites:"Near" and "Far" from the proton target of the CERN-SPS beam. complemented by an ICARUS-like LAr target For (NC) and electron neutrino CC interactions reconstruction.

arXiv: 1304.7127 [physics.ins-det]

NUCIFER Very short baseline reactor experiment

Source experiments

SCRAAM

OscSNS BooNE

Accelerator SBL experiments MicroBooNE (LArTPC),

Tens kilocurie source 50 kCi 144Ce - 144Pr (3 MeV) or 106Ru - 106 Rh (3.54 MeV)

MiniBooNE + SciBooNE

BOREXINO, KamLAND, SNO+

M. Cribier et al, 1107.2335 [hep-ex]]

SOX 51Cr G Bellini et al 1304.7721

H Nunokawa O L G PeresR Zukanovich-FunchalPhys. Lett B562 (2003) 279

S Choubey JHEP 0712 (2007) 014

nm - ns oscillations with Dm2 ~ 1 eV2 are enhanced in matter of the Earth in energy range 0.5 – few TeV

IceCube

This distorts the energy spectrum and zenith angle distribution of the atmospheric muon neutrinos

S Razzaque and AYS , 1104.1390, [hep-ph]

Possible distortion of the zenith angle distribution due to sterile neutrinos

Varying |Ut0|2

< 3% stat. error

no sterile

IC79

Less than 5% puls

A. Gross, 1301.4339 [hep-ex]

CC interactions, muon tracks

A Esmaili, AYS

With 5% uncorrelated systematics

nmnt

ne

n2

n1

n0

mas

s Dm231

Dm221

n3

Dm2dip

ns

- additional radiation in the Universe if mixed in n3

Very light sterile neutrino

- solar neutrino data

Motivated by

no problem with LSS (bound on neutrino mass)

m0 ~ 0.003 eV

can be tested in atmospheric neutrinos with DC IceCube

sin2 2a ~ 10-3

sin2 2b ~ 10-1

DE scale?

M2 MPlanck

M ~ 2 - 3 TeV

pp 7Be CNO 8B

ne - survival probability from solar neutrino data vs LMA-MSW solution

HOMESTAKE low rate

.pep

SNO

SNO+

m0 ~ 0.003 eV

M2 MPlanck

m0 =

M ~ 2 - 3 TeV

P. de Holanda, AYS

L R

NormalMass hierarchy

3- 10 kev - warm dark matter - radiative decays X-rays

Few 100 MeV

- generate light mass of neutrinos- generate via oscillations lepton asymmetry in the Universe- can beproduced in B-decays (BR ~ 10-10 )

split ~ few kev

M. Shaposhnikov et al

Phenomenology of

sterile neutrinos

nBAU

WDM

Everything below EW scale small Yukawa couplings

EW seesaw

Neutrino mass hierarchy

CP-violation

deviation of

2-3 mixing

from maximal Absolute

mass scale

Majorana

nature Searches for bb0n- decay

Checks of existence of sterile neutrinos

Study of geo-neutrinos

Solar neutrinos: DN - asymmetry, CNO, spectral upturn

Detection of high energy cosmic neutrinos

Neutrinos and

cosmology:

connections of

neutrinos to the dark

Universe

Detection of Galactic SN neutrinosrelic SN

neutrinos

Reconstruction of the mass and mixing spectrum

Astrophysics

Majoran

aphases

Earth matter effectEnergy spectrsNOvA

Neutrino beam Fermilab-PINGU(W. Winter)

Sterile neutrinos may help?

NH IHnu antinu

Strong suppression of the ne peak NH ne n3

in neutrino channels NH in antineutrino IH

Shock wave effect

in the antineutrino

channel only NH

in the neutrino channel only IH

If the earth matter effect is observed for antineutrinosNH is established!

Permutation of the electron and non-electron neutrino spectra

Neutrino collectiveeffects

Time rise of the anti-ne burst initial phase IH

more in IH case,spectral splits at high energies IH

P. Serpico et al

Earth matter effects

G Fuller et alB Dasgupta et al

A. Dighe, A. S.

C. Lunardini

G. Fuller, et alR. Tomas et al

The neutrino oscillation probability at baselines of 295 (left), 810 (middle), and 7500 km (right) as a function of the neutrino energy. The red (blue) band corresponds to the normal (inverted) mass hierarchy and the band width is obtained by varying the value of . The probabilities for look similar with the hierarchies interchanged. Note the different scales of the axes.

M. Blennow and A Y Smirnov Advances in High Energy Physics Volume 2013 (2013), Article ID 972485

WC, V = 0.99 MtFid. V = 0.56 Mt   99,000, 20 inch PMTs 20% photocoverage JPARC beam, off-axisBaseline 295 km 

Segmented scimtillator detector 14 kTNuMI beamoff-axis (14 mrad) baseline 810 km

CP/MH/astro

CP/MH/osc. parameters

MH/astro

ICAL Iron calorimeterscintillator

MH: 2 - 3 s in half d space

MEMPHYS: CERN - Fréjus tunnel. Two WC tanks 65 m (d) x 103 m (h)

LBNO

LBNE

The LENA (Low-Energy Neutrino Astronomy) 50 kt of liquid scintillator (LSc) tank 32 m x 100 m height.

Oscillation physics with Huge atmospheric neutrino detectors

ANTARES

DeepCore

Oscillations at high energies 10 – 100 GeV in agreement with low energy data

no oscillation effect at E > 100 GeV

Ice Cube

Oscillations 2.7s

M G Aarten et al [IceCube Collaboration]arXiv: 1305.3909

ANTARES

Ice C

ube

Precision IceCube NextGeneration Upgrade

OscillationResearch withCosmics with the Abyss

20 new strings (~60 DOMs each) in 30 MTon DeepCore volume

Few GeV threshold in inner 10 Mton volume

Existing IceCube strings

Existing DeepCore strings

New PINGU strings

PINGU v6Denser array

Energy resolution ~ 3 GeV

125m

75m

26m

6 m vertical

DC: h = 350 m d =250

nm + n m+ h

muon track

cascade

Em qm Eh En = Em + Eh Eh Em q m qn

105 events/year

E. Akhmedov, S. Razzaque, A. Y. S.arXiv: 1205.7071

Stot ~ s n1/2

s q ~ 1/E0.5

sE = 0.2E

s q ~ 0.5/E0.5

Smearing with Gaussian reconstruction functions characterized by (half) widths

sE = A E

n

s q = B (mp / E n)1/2

S tot = [S ij Sij2 ]1/2

Improvements of reconstruction of the neutrino angle leads to substantial increase of significance without degeneracy of parameters

sE , GeV 2.3 7.8

E , GeV 10 – 20 20 – 50

Tyce De Young, March 2013

s q 8.3o 4.3o

3, 14o

with experimental smearing

sE = (0.7 En)1/2 y0 = 20o

y-integrated

bad nu – nubar separation

bad angular resolution

Mathieu Ribordy, A. Y .S., 1303.0758 [hep-ph]

Increases significance by 30 – 70 %

sin2 q32, true = 0.42

sin2 q32, fit = 0.50

Shape does not change the amplitude changes

Large significance at low energies

Difficult with PINGU but can be done with next updateWith E ~ 0.1 GeV

The last mixing angle the 1-3 mixing is measured. Strong impact on phenomenology , theory and future experimental programs.

Critical check of the 0nbb - decay observation claim

Studies of atmospheric neutrinos may allow to establish mass hierarchy , measure oscillation parameters, perform searches for sterile neutrinos, non-standard interactions . The fastest, cheapest, reliable way?

Theory: still at the cross-roads. The same 1-3 mixing from different relations with different implications. TBM, Flavor symmetries…?

Sterile neutrinos: challenge for

everything. Ice Cube can help

IceCube: hint for detection of cosmic neutrinos of high energies or new physics in neutrino interactions?

Race for thre neutrino mass hierarchy and CP has started

New important developments (new phase) in the field can

be related to Multi-megaton mass scale under

ice,underwater detectors with low (~1 GeV) energy

threshold (PINGU, ORCA)

indirect connection

Light activeneutrinos

Mechanism of neutrino mass generation

new particles

Mixing pattern

Flavor symmetries

ensure stability of DM particles

play the role of DM

right handed neutrinos

Z2

New neutrinostates

HDM

Warm DM

Directconnection

of the Universe

Dark

Energy

Neutrinos and gravitino as DMW. Buchmueller

Everything from one

P. F. HarrisonD. H. PerkinsW. G. Scott

Utbm = U23(p/4) U12

- maximal 2-3 mixing- zero 1-3 mixing- no CP-violation

Utbm = 2/3 1/3 0- 1/6 1/3 - 1/2 - 1/6 1/3 1/2

n2 is tri-maximally mixed n3 is bi-maximally mixed

- sin2q12 = 1/3

L. Wolfenstein

Symmetry from mixing matrix

0.15

0.62

0.78

Dominant approach

Form invariance

D. Hernandez, A.S.to be submitted

- bounds on moduli of matrix elements- elements of a given column j determined by

index of S - two relations corresponding to real and imaginary

of a- the column j is completely determined

Tr (WiU) = Tr ( UPMNS Si UPMNS + T )

Sa (2|Uaj|2 – 1) e = a

ifa

|Uej|2 =

aR cos (fe /2) + cos (3fe /2) – aI sin (fe /2) 4 sin (fe m /2) sin (fte /2)

f ab = fa - fb

aR cos (fm /2) + cos (3fm /2) – aI sin ( fm /2)

4 sin (fe m /2) sin (fmt /2) |Umj|2 =

Interesting possibilities

2/31/61/6

For i =1 Trimaximal 1

1/31/31/3

For i = 2 Trimaximal 2

1/41/21/4

T (SiU T) = WiU

Another class of possibilities: with (m – p) permutation

corrections wash out sharp difference of elements of the dominant mt-block and the subdominant e-line

Values of elements gradually decrease from mtt to mee

This can originate from power dependence of elements on large expansion parameter l ~ 0.7 – 0.8 . Another complementarity: l = 1 - qC

Froggatt-Nielsen?

Number of photo-electons

Also excess of events at lower energies:

27 events are observed12 are expected

Atm. Neutrino Background: 0.082 +/- 0.004 (stat) + 0.041 / – 0.057(syst.)

0 mDT 0

mD 0 MDT

0 MD m

mn = mDT MD

-1T m MD-1 mD

Beyond SM: many heavy singlets…string theory

R.N. MohapatraJ. Valle

Three additional singlets S which couple with RH neutrinos

nnc

S

allows to lower the scales of the neutrino mass generation

m << MD

explains intermediate scale for the RH neutrinos

m ~ MPl, M ~ MGU

m - scale of B-L violation

m = 0 massless neutrinos

M ~ MGU2/MPl ~ 10-14 GeV

violation of universality, unitarity

Inverse seesaw

Cascade seesawm >> MD

(2 – 4) 10-3 eV

0.5 - 2 eV

1 - 10 keV

40 - 70 MeV - LSND, MiniBooNE

- Warm Dark matter- Pulsar kick

- Solar neutrinos- Extra radiation in the Universe

- LSND, MiniBooNE- Reactor anomaly- Ga-calibration experiments- Extra radiation

ns

1 eV

1 keV

1 MeV

10-3 eV

M. Smy

No distortion of the energy spectrum at low energies : the upturn is disfavored at (1.1 – 1.9) s level

Increasing tension between Dm2

21 measured by KamLAND and in solar neutrinos 1.3s level This is how new physics may show

up

nm nt

ne

n2

n1

n1

n2

n3

n3

MA

SS

w32wij = Dm2

ij /2E

D31 ~ 2D32

Inverted hierarchyNormal hierarchy

Oscillations

Mass states can be marked by ne - admixtures

w31

Cosmolog

y

w31

w32

w31 > w32 w31 < w32

makes the e-flavor heavier changes two spectra differently

Fourier analysis

w

S. Petcov M. Piai

Matter effect

bb-decay

J. Kopp , P. A. N. Machado, M. Maltoni, T. Schwetz, 1303.3011 [hep-ph]