Oscillation Experiments 1 · 2020. 8. 11. · Brief overview of our (experimental neutrino...

Neutrino Oscillation Experiments Part 1

Roxanne GuenetteHarvard University

SLAC Summer Institute10 August 2020

1

Organization of the lecture

• Brief overview of neutrino oscillation experiment history

• Experimental view of neutrino oscillations

• Key ingredients for such experiments

• Long-baseline neutrino experiments

➡Experimental steps

➡Past/current experiments

2

Brief overview of our (experimental neutrino oscillation) history

• History of neutrinos is not a straight and clear progression of discoveries. It is composed of several decades of confusion which culminated with the discovery of neutrino oscillation

3

• After the discovery of the neutrinos (νe (1956) and νμ (1962)), people showed increased interest in studying these new particles

• The obvious source was the Sun

Solar neutrinos

• In 1960’s, physicists had a “good” understanding of the sun fusion model

• pp and pep fusion

• Predictions of the neutrino flux by J. Bachall

• Await experimental confirmation

4

TheSun

νe

p

p

e-

FusionintheSunproducesνe

Theorypredictsnumberofνe

Justneedtobuildanexperimenttofindthem

TheSun

νe

p

p

e-

FusionintheSunproducesνe

Theorypredictsnumberofνe

Justneedtobuildanexperimenttofindthem

4

Solar neutrino detection

• In 1964, Ray Davis built a large neutrino detector

• 380 000l of perchloroethylene (cleaning fluid!)

• Neutrino interaction:

• Number of 37Ar ∝ to number of 𝜈e

• Results gave ~10 atoms of 37Ar every months

• This was 1/3 of theoretical predictions

5

Davis’detector

Whatdidheuseforhisdetector?

380,000litresofperchloroethylenecleaningfluid!

Neutrinosdetectedvia

νe + 37Cl→37Ar+e-

No.of37Aratoms∝no.ofνe interac4ons

Davis’detector






Solar neutrino detection

• In 1964, Ray Davis built a large neutrino detector

• 380 000l of perchloroethylene (cleaning fluid!)

• Neutrino interaction:

• Number of 37Ar ∝ to number of 𝜈e

• Results gave ~10 atoms of 37Ar every months

• This was 1/3 of theoretical predictions

6

Davis’detector






Davis’detector






Solar Neutrino Problem…

Follow-up solar neutrino experiments• Two experiments followed-up to address Davis’ results:

Kamiokande II (1985) and Gallex (1991)

7

Kamiokande

Davis’results

Daviscounted10argonatomseachmonth.

Equivalentto1/3numberofneutrinosexpected!

WHATISWRONG?????

Gallex,GrandSasso,Italy Kamiokande,Japan

Gallex



8

Solarneutrinoproblem



9

Solarneutrinoproblem

What’s wrong? Experiments or theory?

Neutrino oscillations?

• SuperKamiokande experiment

10

SuperK

February 5, 2016 28

AN EVENT IN SuperK

Neutrino oscillations?

• SuperKamiokande experiment

• Atmospheric neutrino detection

• 1998 -> Discovery!

11

Neutrino oscillations and the solar neutrino problem

SNO experiment (1999 - 2008)

12

TheSudburyNeutrinoObservatory

Ultra-purewater:targetlevelsgU/gH2O 4.5x10-13gTh/gH2O 37x10-14gU/gD2O 3.0x10-14gTh/gD2O 3.8x10-15

Leastradioac2vewaterCherenkovdetectorintheuniverse!


SNO experiment (1999 - 2008)

13

Added NaCl

Nudetec.onmethods

Elas2cScaSering-Sensi.vetoallflavours-Moresensi.vetoνe-Givesdirec.onofν

ChargedCurrent-Sensi.vetoonlyνe-Measuresνenergy

NeutralCurrent-Equallysensi.vetoallflavours-Measurestotal8Bνflux

Heavywaterallowsindependentmeasurementsofνeandfluxofallflavours

(CC) (NC)

Phase 1 Phase 2


SNO results

14

ResultsfromSNO

Neutrino oscillation further confirmation

Confirmed by reactor experiments (KamLand)

15

9'KJ#G2+'01'2%3'&#<(•  Powerful anti-neutrino source (E� ~ 1-10 MeV)

•  Detectors at distances ~10-1000 m

WIDG October 28th 2011 13

8"2

8"2

8"28"2

8"2

8"2

8"28"2 !"#$%&!'()'*+',&-.)/%-011 Short Baseline Reactor Experiments (Yves Déclais) 4

2'34)5,&#6)786'9),765:&;')'4)756

X section

Production spectrum

Detectected spectrum

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ABB3+f+ABBB3(


Accelerator-generated neutrinos

16


17

Now clear that neutrino oscillate!Accelerator-generated neutrinos

Neutrino oscillation: Theoretical point of view

18

Great introduction by Andre de Gouvea


19

Status of neutrino physics

(νe,νμ,ντ)

9

Neutrino Mixing

We

!e

Since ν ’s have only weakinteractions, flavour eigenstatesare defined as those states that

couple to W

What if the flavour eigenstates are rotated relative to the masseigenstates (eigenstates of Hamiltonian with well-defined mass)?

⎛

⎜⎜⎜⎜⎝

νe

νµ

ντ

⎞

⎟⎟⎟⎟⎠=

⎡

⎢⎢⎢⎢⎣

Ue1 Ue2 Ue3

Uµ1 Uµ2 Uµ3

Uτ1 Uτ3 Uτ3

⎤

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⎛

⎜⎜⎜⎜⎝

ν1

ν2

ν3

⎞

⎟⎟⎟⎟⎠}

• Neutrinos are the only particles of the SM defined by their flavor eigenstates

• This results in an oscillation between the flavors

Wednesday, January 19, 2011

• 𝜈 are the only particles of the SM defined by the flavor eigenstates (𝜈e, 𝜈𝜇, 𝜈𝜏)

From an experimentalist !


20

• 𝜈 are the only particles of the SM defined by the flavor eigenstates (𝜈e, 𝜈𝜇, 𝜈𝜏)

2 neutrino case

1

P⌫↵!⌫�(L, E) = sin22✓sin2

1.27�m2(eV 2)L(km)

E(GeV )

!

(1)

Probing the oscillation parameters

21

1

P⌫↵!⌫�(L, E) = sin22✓sin2

1.27�m2(eV 2)L(km)

E(GeV )

!

(1)


22

1

P⌫↵!⌫�(L, E) = sin22✓sin2

1.27�m2(eV 2)L(km)

E(GeV )

!

(1)

sin22𝜃

𝛥m2

Experimental parameters

Physics parameters to

extract


23

1

P⌫↵!⌫�(L, E) = sin22✓sin2

1.27�m2(eV 2)L(km)

E(GeV )

!

(1)

Experimental parameters

Physics parameters to

extract

sin22𝜃

𝛥m2


24

Lsun-earth = 1.5 x 108 km Eν ~ 0.001 GeV

L/E ~ 1011 Δm2 ~ 10-11

Latmo = 10 to 12000km Eν_atmo = 0.1 to 1000GeV

L/E ~ 0.01 - 105 Δm2 ~ 10-5-100

1

P⌫↵!⌫�(L, E) = sin22✓sin2

1.27�m2(eV 2)L(km)

E(GeV )

!

(1)

Llbl = 100-1000km Eν_acc ~ 1 GeV

L/E ~ 100-1000 Δm2 ~ 10-2-10-3


25

Oscillation probability

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1

P⌫↵!⌫�(L, E) = sin22✓sin2

1.27�m2(eV 2)L(km)

E(GeV )

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Where are we now?


9

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. .

PDG 26

One word about θ13

• Pre-2011: Reactor experiments such as Chooz had measured limits on sin2(2θ13) < 0.19

• Daya Bay (and Reno and Double-Chooz) measured sin2(2θ13) = 0.08 (we were only a factor ~2 away!)

• Great news for completing our understanding of oscillation as δCP is directly linked to θ13

27

Chapter 3: Long-Baseline Neutrino Oscillation Physics 3–9

and s–— = sin ◊–—:

UPMNS =

Q

ca1 0 00 c23 s230 ≠s23 c23

R

db

¸ ˚˙ ˝I

Q

cac13 0 e

≠i”CPs130 1 0

≠ei”CPs13 0 c13

R

db

¸ ˚˙ ˝II

Q

cac12 s12 0

≠s12 c12 00 0 1

R

db

¸ ˚˙ ˝III

(3.2)

The parameters of the PMNS matrix determine the probability amplitudes of the neutrino oscil-lation phenomena that arise from mixing. The frequency of neutrino oscillation depends on thedi�erence in the squares of the neutrino masses, �m

2ij

© m2i

≠ m2j; a set of three neutrino mass

states implies two independent mass-squared di�erences (the “solar” mass splitting, �m221, and

the “atmospheric” mass splitting, �m231), where �m

231 = �m

232 + �m

221. The ordering of the mass

states is known as the neutrino mass hierarchy. An ordering of m1 < m2 < m3 is known as thenormal hierarchy since it matches the mass ordering of the charged leptons in the Standard Model,whereas an ordering of m3 < m1 < m2 is referred to as the inverted hierarchy.

The entire complement of neutrino experiments to date has measured five of the mixing parame-ters [4, 5, 6]: the three angles ◊12, ◊23 and (recently) ◊13, and the two mass di�erences �m

221 and

�m231. The sign of �m

221 is known, but not that of �m

231, which is the crux of the mass hierarchy

ambiguity. The values of ◊12 and ◊23 are large, while ◊13 is smaller. The value of ”CP is unknown.The absolute values of the entries of the PMNS matrix, which contains information on the strengthof flavor-changing weak decays in the lepton sector, can be expressed in approximate form as

|UPMNS| ≥

Q

ca0.8 0.5 0.10.5 0.6 0.70.3 0.6 0.7

R

db . (3.3)

using values for the mixing angles given in Table 3.4. The three-flavor-mixing scenario for neutrinosis now well established. However, the mixing parameters are not known to the same precision asare those in the corresponding quark sector, and several important quantities, including the valueof ”CP and the sign of the large mass splitting, are still undetermined.

The relationships between the values of the parameters in the neutrino and quark sectors suggestthat mixing in the two sectors is qualitatively di�erent. Illustrating this di�erence, the value of theentries of the CKM quark-mixing matrix (analogous to the PMNS matrix for neutrinos, and thusindicative of the strength of flavor-changing weak decays in the quark sector) can be expressed inapproximate form as

|VCKM| ≥

Q

ca1 0.2 0.004

0.2 1 0.040.008 0.04 1

R

db . (3.4)

for comparison to the entries of the PMNS matrix given in Equation 3.3. As discussed in [7], thequestion of why the quark mixing angles are smaller than the lepton mixing angles is an importantpart of the flavor pattern question.

To quote the discussion in [8], “while the CKM matrix is almost proportional to the identity matrixplus hierarchically ordered o�-diagonal elements, the PMNS matrix is far from diagonal and, withthe possible exception of the Ue3 element, all elements are O(1).” It is important here to note that

Volume 2: The Physics Program for DUNE at LBNF LBNF/DUNE Conceptual Design Report

Eur.Phys.J.C27:331-374,2003

Daya Bay and the Last of the angles

48

Mixing angles

Where are we now?

28

U =

1 0 00 cosθ23 sinθ230 − sinθ23 cosθ23

⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟

cosθ13 0 sinθ13e− iδ

0 1 0− sinθ13e

iδ 0 cosθ13

⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟

cosθ12 sinθ12 0− sinθ12 cosθ12 00 0 1

⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟

The PMNS Mixing Matrix 5

P. Vahle, INSS 2019

How well we know it

!

"matm

2

!

"msol

2 : 2.5%

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sin2(✓23) : 5%<latexit sha1_base64="Rpp8nkcWJEAHIOqYgL6E+R8k9gE=">AAACA3icbVA9SwNBEN2LXzF+ndppsxgCsQl3UVGsgjaWEcwH5GLY22ySJXt7x+6cEI6AjX/FxkIRW/+Enf/GTXKFJj4YeLw3w8w8PxJcg+N8W5ml5ZXVtex6bmNza3vH3t2r6zBWlNVoKELV9IlmgktWAw6CNSPFSOAL1vCH1xO/8cCU5qG8g1HE2gHpS97jlICROvaBp7m8Lxc9GDAgnaR8Mj6+xGdeIZfr2Hmn5EyBF4mbkjxKUe3YX143pHHAJFBBtG65TgTthCjgVLBxzos1iwgdkj5rGSpJwHQ7mf4wxgWjdHEvVKYk4Kn6eyIhgdajwDedAYGBnvcm4n9eK4beRTvhMoqBSTpb1IsFhhBPAsFdrhgFMTKEUMXNrZgOiCIUTGyTENz5lxdJvVxynZJ7e5qvXKVxZNEhOkJF5KJzVEE3qIpqiKJH9Ixe0Zv1ZL1Y79bHrDVjpTP76A+szx+dp5WI</latexit><latexit 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sin2(✓13) : 3.5%<latexit sha1_base64="0FwaRNLKvrRrENUvPyZS8kPZMEg=">AAACBXicbVDLSsNAFJ34rPVVdamLwVKom5C0iuKq6MZlBfuAJobJdNIOnUzCzI1QQjdu/BU3LhRx6z+4829MHwttPXDhcM693HuPHwuuwbK+jaXlldW19dxGfnNre2e3sLff1FGiKGvQSESq7RPNBJesARwEa8eKkdAXrOUPrsd+64EpzSN5B8OYuSHpSR5wSiCTvMKRo7m8r5Qd6DMgXmpXRyeXuGqeOaV83isULdOaAC8Se0aKaIa6V/hyuhFNQiaBCqJ1x7ZicFOigFPBRnkn0SwmdEB6rJNRSUKm3XTyxQiXMqWLg0hlJQFP1N8TKQm1HoZ+1hkS6Ot5byz+53USCC7clMs4ASbpdFGQCAwRHkeCu1wxCmKYEUIVz27FtE8UoZAFNw7Bnn95kTQrpm2Z9u1psXY1iyOHDtExKiMbnaMaukF11EAUPaJn9IrejCfjxXg3PqatS8Zs5gD9gfH5A4nMlfw=</latexit><latexit sha1_base64="0FwaRNLKvrRrENUvPyZS8kPZMEg=">AAACBXicbVDLSsNAFJ34rPVVdamLwVKom5C0iuKq6MZlBfuAJobJdNIOnUzCzI1QQjdu/BU3LhRx6z+4829MHwttPXDhcM693HuPHwuuwbK+jaXlldW19dxGfnNre2e3sLff1FGiKGvQSESq7RPNBJesARwEa8eKkdAXrOUPrsd+64EpzSN5B8OYuSHpSR5wSiCTvMKRo7m8r5Qd6DMgXmpXRyeXuGqeOaV83isULdOaAC8Se0aKaIa6V/hyuhFNQiaBCqJ1x7ZicFOigFPBRnkn0SwmdEB6rJNRSUKm3XTyxQiXMqWLg0hlJQFP1N8TKQm1HoZ+1hkS6Ot5byz+53USCC7clMs4ASbpdFGQCAwRHkeCu1wxCmKYEUIVz27FtE8UoZAFNw7Bnn95kTQrpm2Z9u1psXY1iyOHDtExKiMbnaMaukF11EAUPaJn9IrejCfjxXg3PqatS8Zs5gD9gfH5A4nMlfw=</latexit><latexit sha1_base64="0FwaRNLKvrRrENUvPyZS8kPZMEg=">AAACBXicbVDLSsNAFJ34rPVVdamLwVKom5C0iuKq6MZlBfuAJobJdNIOnUzCzI1QQjdu/BU3LhRx6z+4829MHwttPXDhcM693HuPHwuuwbK+jaXlldW19dxGfnNre2e3sLff1FGiKGvQSESq7RPNBJesARwEa8eKkdAXrOUPrsd+64EpzSN5B8OYuSHpSR5wSiCTvMKRo7m8r5Qd6DMgXmpXRyeXuGqeOaV83isULdOaAC8Se0aKaIa6V/hyuhFNQiaBCqJ1x7ZicFOigFPBRnkn0SwmdEB6rJNRSUKm3XTyxQiXMqWLg0hlJQFP1N8TKQm1HoZ+1hkS6Ot5byz+53USCC7clMs4ASbpdFGQCAwRHkeCu1wxCmKYEUIVz27FtE8UoZAFNw7Bnn95kTQrpm2Z9u1psXY1iyOHDtExKiMbnaMaukF11EAUPaJn9IrejCfjxXg3PqatS8Zs5gD9gfH5A4nMlfw=</latexit><latexit sha1_base64="0FwaRNLKvrRrENUvPyZS8kPZMEg=">AAACBXicbVDLSsNAFJ34rPVVdamLwVKom5C0iuKq6MZlBfuAJobJdNIOnUzCzI1QQjdu/BU3LhRx6z+4829MHwttPXDhcM693HuPHwuuwbK+jaXlldW19dxGfnNre2e3sLff1FGiKGvQSESq7RPNBJesARwEa8eKkdAXrOUPrsd+64EpzSN5B8OYuSHpSR5wSiCTvMKRo7m8r5Qd6DMgXmpXRyeXuGqeOaV83isULdOaAC8Se0aKaIa6V/hyuhFNQiaBCqJ1x7ZicFOigFPBRnkn0SwmdEB6rJNRSUKm3XTyxQiXMqWLg0hlJQFP1N8TKQm1HoZ+1hkS6Ot5byz+53USCC7clMs4ASbpdFGQCAwRHkeCu1wxCmKYEUIVz27FtE8UoZAFNw7Bnn95kTQrpm2Z9u1psXY1iyOHDtExKiMbnaMaukF11EAUPaJn9IrejCfjxXg3PqatS8Zs5gD9gfH5A4nMlfw=</latexit>

sin2(✓12) : 5.5%<latexit sha1_base64="IUWhvLoyN/c310Y6j6mpbYxS2jM=">AAACBXicbVBNS8NAEN3Ur1q/oh71sFgK9RKSYlE8Fb14rGA/oKlhs922SzebsDsRSujFi3/FiwdFvPofvPlvTNoetPXBwOO9GWbm+ZHgGmz728itrK6tb+Q3C1vbO7t75v5BU4exoqxBQxGqtk80E1yyBnAQrB0pRgJfsJY/us781gNTmofyDsYR6wZkIHmfUwKp5JnHrubyvlJ2YciAeIlTmZxe4qpVdUuFgmcWbcueAi8TZ06KaI66Z365vZDGAZNABdG649gRdBOigFPBJgU31iwidEQGrJNSSQKmu8n0iwkupUoP90OVlgQ8VX9PJCTQehz4aWdAYKgXvUz8z+vE0L/oJlxGMTBJZ4v6scAQ4iwS3OOKURDjlBCqeHorpkOiCIU0uCwEZ/HlZdKsWI5tObdnxdrVPI48OkInqIwcdI5q6AbVUQNR9Iie0St6M56MF+Pd+Ji15oz5zCH6A+PzB4tRlf0=</latexit><latexit sha1_base64="IUWhvLoyN/c310Y6j6mpbYxS2jM=">AAACBXicbVBNS8NAEN3Ur1q/oh71sFgK9RKSYlE8Fb14rGA/oKlhs922SzebsDsRSujFi3/FiwdFvPofvPlvTNoetPXBwOO9GWbm+ZHgGmz728itrK6tb+Q3C1vbO7t75v5BU4exoqxBQxGqtk80E1yyBnAQrB0pRgJfsJY/us781gNTmofyDsYR6wZkIHmfUwKp5JnHrubyvlJ2YciAeIlTmZxe4qpVdUuFgmcWbcueAi8TZ06KaI66Z365vZDGAZNABdG649gRdBOigFPBJgU31iwidEQGrJNSSQKmu8n0iwkupUoP90OVlgQ8VX9PJCTQehz4aWdAYKgXvUz8z+vE0L/oJlxGMTBJZ4v6scAQ4iwS3OOKURDjlBCqeHorpkOiCIU0uCwEZ/HlZdKsWI5tObdnxdrVPI48OkInqIwcdI5q6AbVUQNR9Iie0St6M56MF+Pd+Ji15oz5zCH6A+PzB4tRlf0=</latexit><latexit sha1_base64="IUWhvLoyN/c310Y6j6mpbYxS2jM=">AAACBXicbVBNS8NAEN3Ur1q/oh71sFgK9RKSYlE8Fb14rGA/oKlhs922SzebsDsRSujFi3/FiwdFvPofvPlvTNoetPXBwOO9GWbm+ZHgGmz728itrK6tb+Q3C1vbO7t75v5BU4exoqxBQxGqtk80E1yyBnAQrB0pRgJfsJY/us781gNTmofyDsYR6wZkIHmfUwKp5JnHrubyvlJ2YciAeIlTmZxe4qpVdUuFgmcWbcueAi8TZ06KaI66Z365vZDGAZNABdG649gRdBOigFPBJgU31iwidEQGrJNSSQKmu8n0iwkupUoP90OVlgQ8VX9PJCTQehz4aWdAYKgXvUz8z+vE0L/oJlxGMTBJZ4v6scAQ4iwS3OOKURDjlBCqeHorpkOiCIU0uCwEZ/HlZdKsWI5tObdnxdrVPI48OkInqIwcdI5q6AbVUQNR9Iie0St6M56MF+Pd+Ji15oz5zCH6A+PzB4tRlf0=</latexit><latexit sha1_base64="IUWhvLoyN/c310Y6j6mpbYxS2jM=">AAACBXicbVBNS8NAEN3Ur1q/oh71sFgK9RKSYlE8Fb14rGA/oKlhs922SzebsDsRSujFi3/FiwdFvPofvPlvTNoetPXBwOO9GWbm+ZHgGmz728itrK6tb+Q3C1vbO7t75v5BU4exoqxBQxGqtk80E1yyBnAQrB0pRgJfsJY/us781gNTmofyDsYR6wZkIHmfUwKp5JnHrubyvlJ2YciAeIlTmZxe4qpVdUuFgmcWbcueAi8TZ06KaI66Z365vZDGAZNABdG649gRdBOigFPBJgU31iwidEQGrJNSSQKmu8n0iwkupUoP90OVlgQ8VX9PJCTQehz4aWdAYKgXvUz8z+vE0L/oJlxGMTBJZ4v6scAQ4iwS3OOKURDjlBCqeHorpkOiCIU0uCwEZ/HlZdKsWI5tObdnxdrVPI48OkInqIwcdI5q6AbVUQNR9Iie0St6M56MF+Pd+Ji15oz5zCH6A+PzB4tRlf0=</latexit>

From M. Tortola, Neutrino2018 and deSalas et al, 1708.01186 (May 2018)

U =


⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟


0 1 0− sinθ13e

iδ 0 cosθ13

⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟


⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟


P. Vahle, INSS 2019

How well we know it

!

"matm

2

!

"msol

2 : 2.5%






PDG

Resolution on parameters:

Where are we now?

29

U =


⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟


0 1 0− sinθ13e

iδ 0 cosθ13

⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟


⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟


P. Vahle, INSS 2019

How well we know it

!

"matm

2

!

"msol

2 : 2.5%






U =


⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟


0 1 0− sinθ13e

iδ 0 cosθ13

⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟


⎛

⎝

⎜⎜⎜

⎞

⎠

⎟⎟⎟


P. Vahle, INSS 2019

How well we know it

!

"matm

2

!

"msol

2 : 2.5%






PDG

Resolution on parameters:

Where do we go from here?

Where do we go from here? The great questions of neutrino physics• What are the absolute neutrino masses?

• What is the nature of neutrinos (Dirac or Majorana)?

• What is the mass hierarchy (ordering)

• Is θ23 maximal?

• Is there CP violation? What is 𝛿CP?

• Are there sterile neutrinos?30

Where do we go from here? The great questions of neutrino physics• What are the absolute neutrino masses?

• What is the nature of neutrinos (Dirac or Majorana)?

• What is the mass ordering (hierarchy)

• Is θ23 maximal?

• Is there CP violation? What is 𝛿CP?

• Are there sterile neutrinos?31

All answerable by studying neutrino

oscillation!

What is the mass ordering?

(𝛥m2)sol ~ 10-5 eV2

(𝛥m2)atmo ~ 10-3 eV2

32

➡ Simplify oscillation predictions significantly ➡ Constrain GUT ➡ Guidance to 0𝜈𝛽𝛽 experiments

What is the mass ordering?

(𝛥m2)sol ~ 10-5 eV2

(𝛥m2)atmo ~ 10-3 eV2

33

➡ Simplify oscillation predictions significantly ➡ Constrain GUT ➡ Guidance to 0𝜈𝛽𝛽 experiments

See lecture on Neutrinoless double beta decay

Is there CP violation? What is 𝛿CP?

Anti-Matter ⇒ Matter ???

CP violation!

34

Equal amount of matter and anti-matter(?)

Matter domination!

Chapter 3: Long-Baseline Neutrino Oscillation Physics 3–9

and s–— = sin ◊–—:

UPMNS =

Q

ca1 0 00 c23 s230 ≠s23 c23

R

db

¸ ˚˙ ˝I

Q

cac13 0 e

≠i”CPs130 1 0

≠ei”CPs13 0 c13

R

db

¸ ˚˙ ˝II

Q

cac12 s12 0

≠s12 c12 00 0 1

R

db

¸ ˚˙ ˝III

(3.2)

The parameters of the PMNS matrix determine the probability amplitudes of the neutrino oscil-lation phenomena that arise from mixing. The frequency of neutrino oscillation depends on thedi�erence in the squares of the neutrino masses, �m

2ij

© m2i

≠ m2j; a set of three neutrino mass

states implies two independent mass-squared di�erences (the “solar” mass splitting, �m221, and

the “atmospheric” mass splitting, �m231), where �m

231 = �m

232 + �m

221. The ordering of the mass

states is known as the neutrino mass hierarchy. An ordering of m1 < m2 < m3 is known as thenormal hierarchy since it matches the mass ordering of the charged leptons in the Standard Model,whereas an ordering of m3 < m1 < m2 is referred to as the inverted hierarchy.

The entire complement of neutrino experiments to date has measured five of the mixing parame-ters [4, 5, 6]: the three angles ◊12, ◊23 and (recently) ◊13, and the two mass di�erences �m

221 and

�m231. The sign of �m

221 is known, but not that of �m

231, which is the crux of the mass hierarchy

ambiguity. The values of ◊12 and ◊23 are large, while ◊13 is smaller. The value of ”CP is unknown.The absolute values of the entries of the PMNS matrix, which contains information on the strengthof flavor-changing weak decays in the lepton sector, can be expressed in approximate form as

|UPMNS| ≥

Q

ca0.8 0.5 0.10.5 0.6 0.70.3 0.6 0.7

R

db . (3.3)

using values for the mixing angles given in Table 3.4. The three-flavor-mixing scenario for neutrinosis now well established. However, the mixing parameters are not known to the same precision asare those in the corresponding quark sector, and several important quantities, including the valueof ”CP and the sign of the large mass splitting, are still undetermined.

The relationships between the values of the parameters in the neutrino and quark sectors suggestthat mixing in the two sectors is qualitatively di�erent. Illustrating this di�erence, the value of theentries of the CKM quark-mixing matrix (analogous to the PMNS matrix for neutrinos, and thusindicative of the strength of flavor-changing weak decays in the quark sector) can be expressed inapproximate form as

|VCKM| ≥

Q

ca1 0.2 0.004

0.2 1 0.040.008 0.04 1

R

db . (3.4)

for comparison to the entries of the PMNS matrix given in Equation 3.3. As discussed in [7], thequestion of why the quark mixing angles are smaller than the lepton mixing angles is an importantpart of the flavor pattern question.

To quote the discussion in [8], “while the CKM matrix is almost proportional to the identity matrixplus hierarchically ordered o�-diagonal elements, the PMNS matrix is far from diagonal and, withthe possible exception of the Ue3 element, all elements are O(1).” It is important here to note that

Volume 2: The Physics Program for DUNE at LBNF LBNF/DUNE Conceptual Design Report

And more…

35

Beaucoup de questions à répondre

• Masse:

• Paramètres d’oscillation:

• Neutrinos sont-ils Dirac ou Majorana?

• Y at-il des neutrinos stériles? 10-5

10-4

10-3

10-2

10-1

1

10

10 210 310 410 510 610 710 810 9

10 1010 1110 12

0 1 2 3 4generation

mas

s (eV

)

t

b!

µ

c

s

d u

e

"3"2

"1

TeV

GeV

MeV

keV

eV

meV

FIGURE 1. Masses of all known fundamental fermions. The arrows are meant to represent, qualita-tively, our current knowledge of the neutrino masses.

WHAT WE KNOW AND DON’T KNOW ABOUT NEUTRINOS

Neutrinos change flavor. This means that a neutrino produced in a well-defined weakeigenstate "# can be detected in a distinct weak eigenstate "$ 1 after propagating a

1 Weak eigenstates are labeled by the flavor of the charged lepton involved in the charged current weakprocess responsible for either producing or detecting neutrinos, i.e., #,$ = e,µ ,!, . . ..

De Gouvea A. Proceedings of X Mexican Workshop of Particles and Fields, 2006

!  Quelle est la masse? !  Pourquoi une si petite masse? !  Quelle est la hiérachie?

!  Est-ce que le mélange atmosphérique (θ23) est max?

!  θ13? !  Y a-t-il violation CP?

Understanding particle masses and mixing anglesLooking at the Standard Model, we see a lot of unexplained structure.

Quark mixing:0

@� ⇥ ·⇥ � �

· � �

1

A

Lepton mixing:0

@� � ⇥� � ��

1

A

Joachim Kopp Aspects of Theoretical Neutrino Physics 5


Quark mixing:0

@� ⇥ ·⇥ � �

· � �

1

A

Lepton mixing:0

@� � ⇥� � ��

1

A



Quark mixing:0

@� ⇥ ·⇥ � �

· � �

1

A

Lepton mixing:0

@� � ⇥� � ��

1

A



Quark mixing:0

@� ⇥ ·⇥ � �

· � �

1

A

Lepton mixing:0

@� � ⇥� � ��

1

A


Quark mixing

Lepton mixing

How do we do oscillation experiments?

36

How do we set an oscillation experiment?

• Need a neutrino source (sets the type of ν and Eν)

37



• Need a neutrino detector technology

38




• Choose a baseline (sets the parameters phase space)

39

The Hunt for⌫ CP

Violation:Future

Prospects

Mary BishaiBrookhavenNational

Laboratory

IntroductionCP in ⌫ SMCPV and otherNew Physics

CurrentExperimentalLandscapeT2KNO⌫ANear TermProspects

FutureExperimentalLandscapeDUNEHyperK

Conclusion

The Deep Underground Neutrino Experiment(DUNE) (1300km Baseline)

39 / 53

ν

ICRR, Univ. of Tokyo KEK / JAEA

Super-Kamiokande J-PARCNear Detectors

Neutrino Beam

295 km

Mt. Noguchi-Goro 2,924 m

Mt. Ikeno-Yama 1,360 m

1,700 m below sea level

Mayly Sanchez - ISU

T H E N O VA E X P E R I M E N T I N A N U T S H E L L• Upgraded NuMI beam of muon

neutrinos or antineutrinos at Fermilab running at 700kW.

• Highly active liquid scintillator 14-kton detector off the main axis of the beam.

• Functionally identical detectors: Near Detector (ND) site at Fermilab and Far Detector (FD) 810 km away at Ash River, MN.

• NOvA observes disappearance of muon neutrinos and antineutrinos, appearance of electron neutrinos and antineutrinos and potential suppression of neutral current interactions.

!5

baseline

NOνA Far Detector

NOνA Near Detector

longest← →

810 km

How do we study oscillation?

• Need to pick a channel (we pick as many as possible!)

40

P



• Compare the neutrino energy spectrum to oscillation predictions

41

Muon Neutrino Disappearance

spectrum ratio

Monte Carlo(Input parameters: sin22θ = 1.0, Δm2 = 3.35x10-3 eV2 )

Unoscillated

Oscillated

νμ spectrum

P. Vahle, INSS 2019 13

P fun → Un) = I -

[email protected]

→

IP.Vahle

P



• Compare the neutrino energy spectrum to oscillation predictions

• Fit the oscillated spectrum to extract the oscillation parameters

42

Fit oscillation probability

sin22𝜃𝛥m

2

P

Muon Neutrino Disappearance

spectrum ratio

Monte Carlo(Input parameters: sin22θ = 1.0, Δm2 = 3.35x10-3 eV2 )

Unoscillated

Oscillated

νμ spectrum

P. Vahle, INSS 2019 13

P fun → Un) = I -

[email protected]

→

IP.Vahle

Extract parameters

Wait: More complicated story…


43

We never know very precisely the neutrino flux

Booster Neutrino Beam




44

We don’t understand very well neutrino interactions (cross sections)

νμ μ-

n p

W

Simple CCνμ interaction

4.1 Nuclear E↵ects

n

p

np

p

n

p

n

Charge Exchange

(In)elastic

Scattering

p

p n CCQE Interaction

Intranuclear Medium

Pion Production

Elastic Scattering

Pion Absorption

n

Hadron Absorption

pn

Figure 18: Illustration of FSIs in an INC model approach. The incoming muon neutrino ⌫µ rep-resented by the black arrow followed by the dashed black line interacts via a charged-current quasi-elastic interaction with a neutron of an argon nucleus in the first stepof the IA. The produced negatively charged muon (indigo) and the positively chargedproton (light blue) traverse through the nuclear medium and are subject to nuclear e↵ects(nuclear binding energy, Coulomb distortion, etc.). In the second step of the IA, theproton can undergo various types of fsis which may lead to more FSIs such as (in)elasticscattering, pion production, hadron absorption and charge exchange. Pions ⇡+, ⇡�, ⇡0 inthis figure are shown in dark, lighter and light green, respectively.

has su�cient energy, pions can be produced inside the nucleus called pion production. All theseFSIs become more di�cult to separate with increasing energy of the incident neutrino, becausemultiple combinations of FSIs may lead to the same final state particles. The reinteractions hadronsexperience on their way out of the nucleus modify observable kinematic variable distributionsin most detectors significantly. The sensitivity of an experiment to FSIs strongly depends on thedetector technology, the neutrino energy range and the particular physics measurement [7]. In orderto infer the interaction from the final state hadron(s) that escaped the nucleus, FSIs are modelled(see section 5.1.4) and used to understand and reconstruct the primary neutrino-nucleus interaction

35

From Lars Bathe-Peters

Complicated by nuclear effects…





45

Need to disentangle different physics effects (matter effects, mass ordering, delta CP)





• Fit the oscillated spectrum to extract the oscillation parameters

46

Fit the three neutrino-oscillation probability simultaneously to the different channels or energy spectra

How do we plan future oscillation experiments?• To answer the remaining big questions of neutrino physics, we

need long-baseline oscillation experiments

47



• Choose a baseline (sets the parameters phase space)more on this at the next lecture…

see for example LArTPC from Monday’s lecture

Neutrino beam

A typical long-baseline neutrino experiment

48

1) Neutrino beam (numu)

2) Near Detector(s)

4) Far Detector(s)

3) Baseline

DUNE


49

1) Neutrino beam (numu)

Can reverse the horn current to produce an anti-neutrino beam

Initial ND Data

¨ Discrepancy between Data/MC changes energy with different beam tunes, suggests production of Hadrons off the target is to blame.

¨ After adjusting hadron production, data/MC discrepancies ~5-10% level

LE 10 ME HE

(Refs: Z. Pavlovich, UT Austin, 2008, Phys. Rev. D77 (2008) 072002)

33 P. Vahle, INSS 2019


50

2) Near Detector(s)• Usually identical technology to the far detector (or with some target overlap)

• First goal is to provide the un-oscillated spectrum

• Second goal is to cancel* neutrino interaction and flux uncertainties* This is not 100% possible as flux in ND is different than FD and some effects prevents a full cancellation

3) Baseline (next lecture)

Phys. Rev. D77 (2008) 072002


51

4) Far Detector(s)

• Need very large detectors since flux decreases by 1/r2!Oscillation Sensitivity Calculations

E. Worcester: Neutrino 2018 15

•  Reconstructed spectra based on GEANT4 beam simulation, GENIE event generator, and Fast MC using detector response parameterized at the single particle level •  Efficiency tuned using hand

scan results •  Order 1000 νe appearance

events in ~7 years of equal running in neutrino and antineutrino mode

•  Simultaneous fit to four spectra to extract oscillation parameters

•  Systematics approximated using normalization uncertainties

•  GLoBES configurations arXiv:1606.09550

νe

νµ νµ

DUNE Conceptual Design Report (CDR) arXiv:1512.06148

νe

• High precision neutrino energy spectra

Real-life long-baseline experiments

• Several long-baseline experiments have paved the way in studying neutrino oscillations

52

Outline

• Brief introduction to T2K• Data collection progress

• Preliminary 2018 data analysis results

• Future developments

• Conclusions

Imperial College London

Morgan O. WasckoNeutrino 20182018 / 06 / 04 2

NOVA AND DUNE -NOVA’S LATEST RESULTS ON THREE- FLAVOR NEUTRINO OSCILLATIONS -DUNE STATUS, RESULTS AND PLANS

drhgfdjhngngfmhgmghmghjmghfmf

ZELIMIR DJURCIC (FOR NOVA AND DUNE COLLABORATIONS) High Energy Physics Argonne National Laboratory

Lake Louise Winter Institute 2019, February 10-16, Chateau Lake Louise, Canada

Recent Results from MINOS and MINOS+

Adam AurisanoUniversity of Cincinnati

For the MINOS and MINOS+ Collaborations

XXVIII International Conference on Neutrino Physics and

Astronomy4 June 2018

Heidelberg, Germany

MINOS

53

Credit: Alan Stonebraker

On-axis experiment

NuMI beam (FNAL) Eν ~ 7 GeV (Minos+)

735m baseline

ND: 1kt iron tracker FD: 5.4 kt iron tracker

2005-2012 MINOS+ 2012-2016

νµ→νµ

MINOS

54

νµ→νµ

arXiv:1511.06178 [hep-ex]

MINOS event display

MINOS (LBL) oscillation results

• νμ disappearance allows for measurements of Δm232 and sin2θ23

55

arXiV:2006.15208

MINOS (LBL) oscillation results

56T.Caroll, Neutrino 2020

T2K

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Outline




• Conclusions



Off-axis experiment

J-PARC beam Eν ~ 600 MeV

295m baseline

ND: ND280 (off-axis) INGRID (on-axis) FD: 25kt water Cherenkov (SuperK)



T2K Near Detector pit houses both the

off-axis (ND280) andon-axis (INGRID)

detectors

19 m

37 m

0 deg

2.5 deg

SuperK ND280

2009-…

νµ→νe

T2K

58

Outline




• Conclusions



Off-axis experiment

J-PARC beam Eν ~ 600 MeV

295m baseline

ND: ND280 (off-axis) INGRID (on-axis) FD: 25kt water Cherenkov (SuperK)



T2K Near Detector pit houses both the

off-axis (ND280) andon-axis (INGRID)

detectors

19 m

37 m

0 deg

2.5 deg

SuperK ND280

2009-…

νµ→νeT2K ν beam

T2K

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Outline




• Conclusions



νµ→νe

µ→e

SuperK events

ND280 event

T2K oscillation results

60

Outline




• Conclusions



Nature,580, p.339–344(2020)

• First observation of νμ→νe appearance (with 6 events!) 2011

• Best constraint on sin2θ23

• Indication of δCP = 3π/2 (or -π/2)

• Prefers Normal Mass Ordering

NOvA

61





Mayly Sanchez - ISU

T H E N O VA E X P E R I M E N T I N A N U T S H E L L• Upgraded NuMI beam of muon

neutrinos or antineutrinos at Fermilab running at 700kW.

• Highly active liquid scintillator 14-kton detector off the main axis of the beam.

• Functionally identical detectors: Near Detector (ND) site at Fermilab and Far Detector (FD) 810 km away at Ash River, MN.

• NOvA observes disappearance of muon neutrinos and antineutrinos, appearance of electron neutrinos and antineutrinos and potential suppression of neutral current interactions.

!5

baseline

NOνA Far Detector

NOνA Near Detector

longest← →

Off-axis experiment

NuMI beam (FNAL) Eν ~ 2 GeV

735m baseline

ND: 0.3 kt liquid scintillator FD: 14kt liquid scintillator

2014-…

νµ→νe

NOvA

62





νµ→νe

NOvA oscillation results

63





• First observation of νμ→νe appearance 2018

• Best constraint on Δm232

• Favors different δCP than T2K

• Prefers Normal Mass Ordering

Opera

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νµ→ν𝝉

On-axis ν𝝉 experiment

CNGS beam (CERN) Eν ~ 17 GeV

732m baseline

1.3kt emulsion + lead detector

2008-2012

Opera

65

Finding the ντ

13

OPERAOPERA

Finding the ντ

14

OPERA

νµ→ν𝝉

Opera

66

Finding the ντ

14

OPERA

νµ→ν𝝉

Opera

67

Finding the ντ

15

OPERA

νµ→ν𝝉

Opera

68

νµ→ν𝝉

10 events observed! in 4 years…

Phys. Rev. Lett. 120, 211801 (2018)

• First observation of νμ→ν𝝉 appearance 2018

https://link.aps.org/doi/10.1103/PhysRevLett.120.211801

Summary

• We saw that the history of neutrino oscillation was not straight forward

• We got a feel for how oscillation can be studied and we focused on long-baseline neutrino oscillation experiments as those can address the remaining questions

• We reviewed several long-baseline neutrino experiments

Next Lecture: • What can we expect for the future? How can we propose the

most optimal experiments to answer remaining questions? • What about short-baseline oscillations?

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THANK YOU!

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