Production and radiative decay of heavy neutrinos at the Booster Neutrino Beam

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Production and radiative decay of heavy neutrinos at the Booster Neutrino Beam

Eduardo Sa´ ul Sala, Luis ´ Alvarez Ruso

Universidad de Valencia - IFIC

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Index

1 Introduction

2 ν

h

production and decay Electromagnetic production Neutral current production Antineutrino production

Decay of the heavy sterile neutrino 3 Results

ν

h

production cross sections MiniBooNE

SBN

MicroBooNE LaR1-ND ICARUS

4 Conclusions

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Section 1 Introduction

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Neutrino paradigm

For massive neutrinos the flavor eigenstates do not coincide with the mass eigenstates

Mixing Ñ Pontecorvo–Maki–Nakagawa–Sakata matrix

|ν

α

y “ ÿ

i

U

_αi

|ν

i

y

α “ e, µ, τ ; i “ 1, 2, 3

Oscillations

P pν

α

Ñ ν

β

q “ ÿ

k,j

U

_αk^˚

U

_βk

U

_αj

U

_βj^˚

exp

˜

´i

∆m

²_kj

L 2E

¸

Questions

Dirac or Majorana

Neutrino absolute masses and Mass hierarchy Sterile neutrinos

Values of the parameters: θ

kj

, ∆m

²_kj

and δ

CP

Anomalies

(5)

Anomalies in oscillation experiments

LSND was a short baseline experiment that searched for ν

_e

appearance in a ν

_µ

flux.

An excess of ν

e

was found.

A. Aguilar et al. PRD 64.112007 (2001)

(Originally) interpreted as ν

µ

Ñ ν

e

oscillations.

(6)

MiniBooNE was created to make a further analysis of the LSND signal, and found and excess at low energies

Aguilar-Arevalo et al. PRL110.161801 (2013)

ñ Reconstructed ν energy

E

_ν^QE

“ 2m

n

E

e

´ m

²_e

´ m

²_n

` m

²_p

2 pm

n

´ E

e

` p

e

cos θ

e

q

ñ e-like backgrounds

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Oscillations: not explained by 1, 2, 3 families of sterile neutrinos.

J. Conrad et al., Adv. High Energy Phys. 2013, C. Giunti et al., PRD88 (2013)

The MiniBooNE low-energy anomaly is incompatible with neutrino oscillations

C. Giunti et al., PRD88 (2013)

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Production and radiative decay of heavy neutrinos at the Booster Neutrino Beam 8 Introduction

Heavy neutrinos

Gninenko, PRL 103 (2009)

m

h

« 50MeV, |U

µh

|

²

« 10

^´3

´ 10

^´2

, τ

h

ă 10

^´9

s

Simultaneous description of both MiniBooNE and LSND anomalies.

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Heavy neutrinos

Gninenko, PRL 103 (2009) , Masip et al., JHEP01(2013)106

m

h

“ 50MeV, τ

h

“ 5 ˆ 10

^´9

s, BR pν

h

Ñ ν

µ

γq “ 0.01

Alleviates tensions with other experiments (radiative µ capture at TRIUMF).

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We have analyzed this scenario in order to compare with MiniBooNE

measurements. Also we have predicted the signal due to this kind of processes for SBN.

ν_µ

γ ν

A A

ν_h

γ,Z

On nucleons ν

_µ

pν

µ

q ` N Ñ ν

h

pν

h

q ` N

On nuclei ν

_µ

pν

µ

q ` A Ñ ν

h

pν

h

q ` A ð coherent ν

µ

pν

µ

q ` A Ñ ν

h

pν

h

q ` X ð incoherent ν

_h

“ Dirac ν with m « 50 MeV, slightly mixed with ν

µ

A “

¹²

C (MiniBooNE, CH

2

),

⁴⁰

Ar (SBN program: SBND, MicroBooNE, Icarus)

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Section 2 ν _h production and decay

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Electromagnetic production

In general Broggini et al., Adv.High Energy Phys (2012) H

_{ef f}

“ 1

2 !

ν

_h

Λ

^hα_µ

ν

_α

` ν

α

γ

₀

“Λ

^hα_µ

‰

:

γ

₀

ν

_h

)

A

^µ

α “ e, µ, τ Imposing Lorentz and gauge inv.

Λ

^hα_µ

“ ˆ

γ

_µ

´ q

µ

q { q

²

˙

“f

_Q^hα

pq

²

q ` f

_A^hα

pq

²

qq

²

γ

₅

‰

´ iσ

µν

q

^ν

“f

_M^hα

pq

²

q ` if

_E^hα

pq

²

qγ

5

‰

Choice of Masip et al., JHEP 1301 (2013)

Λ

^hα_µ

“ ´iσ

µν

q

^ν

µ

^α_tr

p1 ´ γ

5

q

if µ

^α_tr

P R ñ CP conserved

(13)

Electromagnetic production

Effective lagrangian of the interaction, Masip et al., JHEP01(2013)106:

L

ef f

“ 1

2 µ

ⁱ_tr

rν

h

σ

µν

p1 ´ γ

5

q ν

i

` ν

i

σ

µν

p1 ` γ

5

q ν

h

s B

^µ

A

^ν

, Inclusive process ν

_i

pkq ` Appq Ñ ν

h

pk

¹

q ` Xpp

¹

q

νipkq νhpk¹q

Appq

γpqq

Xpp¹q

iM “ i e µ

ⁱtr

2 pq

²

` iq upk

¹

q q

α

σ

^αµ

p1 ´ γ

5

qupkq xX|J

µ

|N y .

(14)

General expression for the inclusive cross section:

dσ

dk

¹⁰

dΩ “ | ~ k

¹

|

|~ k|

α pµ

ⁱ_tr

q

²

16 π q

⁴

L

_µν

W

^µν

Leptonic tensor

L

µν

“ 1 4 Tr “

p { k

¹

` m

h

qσ

µα

p1 ´ γ

5

q { k p1 ` γ

5

qσ

νβ

‰ q

^α

q

^β

Hadronic tensor

W

^µν

” 1 2M

˜ ź

i

ż d

³

p

¹_i

p2πq

³

2E

_i¹

¸

p2πq

³

δ

^p4q

pk ` p ´ k

¹

´ p

¹

qH

^µν

H

^µν

“ ÿ

polar.

xX|J

^ν

|N y

^˚

xX|J

^µ

|N y

(15)

QE scattering on nucleons

νµpkq νhpk¹q

N ppq N pp¹q

γpqq

dσ

dt “ α pµ

ⁱ_tr

q

²

4 ps ´ M

²

q

²

t

²

1 1 ´

_4M^t2

`G

²_E

R

_E

´ G

²_M

R

_M

˘ , G

_E

, G

_M

are the Sachs form factors

R

E

“ ´ t `2s ` t ´ 2M

²

˘

2

` m

²_h

t p4s ` tq ´ 4m

⁴_h

M

²

R

_M

“ t

4M

²

”

´4t

´ `M

²

´ s ˘

2

` s t

¯

` 2m

²_h

t `2s ` t ´ 2M

²

˘

´2m

⁴_h

`t ´ 2M

²

˘‰

(16)

Coherent scattering on scalar nucleus

νµpkq ν_hpk¹q

Appq App¹q

γpqq

dσ

dt “ α pµ

ⁱ_tr

q

²

4 ps ´ M

_A²

q

²

t

²

F

²

R

_E

R

_E

“ ´t `2s ` t ´ 2M

_A²

˘

2

` m

²_h

t p4s ` tq ´ 4m

⁴_h

M

_A²

F pq

²

q “ ż

d

³

r e

^i~q¨~r

ρp~rq

(17)

Incoherent scattering on scalar nucleus

Case of QE interaction with the nucleons forming the nucleus.

νµ νh

A X

γ

ν_µpkq

ν_hpk¹q

ν_µpkq N¹pp ` qq

N ppq

γpqq γpqq

Nieves, Amaro, Valverde, PRC70.055503 (2004)

With the local density approximation.

W^µν“ 1 α

ż d³r 4π²Θpq⁰qe²

ż d³p

4π²A^µνδ`p⁰` q⁰´ E p~p ` ~qq˘ np~pq p1 ´ n p~p ` ~qqq 4p⁰pp⁰` q⁰` Ep~p ` ~qqqΘpp⁰q

A^µν“ Tr

"„

γ^νF1´ i

2Mσ^ναqαF2



`

p ` {q ` M{ N

˘

„

γ^µF1` i

2Mσ^µβqβF2



` {p ` MN

˘

*

Fj“ FjpGE, GMq

(18)

Incoherent scattering on scalar nucleus

Case of QE interaction with the nucleons forming the nucleus.

νµ νh

A X

γ

νµpkq

νhpk¹q

νµpkq N¹pp ` qq

N ppq

γpqq γpqq

With the local density approximation.

W^µν“ 1 α

ż d³r 4π²Θpq⁰qe²

ż d³p

4π²A^µνδ`p⁰` q⁰´ E p~p ` ~qq˘ np~pq p1 ´ n p~p ` ~qqq 4p⁰pp⁰` q⁰` Ep~p ` ~qqqΘpp⁰q

Occupation number:

np~ pq “ Θ pk

F

´ |~ p|q ; k

^N_F

prq “ `3π

²

ρ

^N

prq ˘

1{3

(19)

Neutral current production

Effective lagrangian of the interaction:

L

I

“ ´ g 2 cos θ

W

j

^µ

Z

µ

; j

^α

“ 1

2 ν

µ

γ

^α

p1 ´ γ

5

qν

µ

, Inclusive process ν

i

pkq ` Appq Ñ ν

h

pk

¹

q ` Xpp

¹

q,

νipkq νhpk¹q

Appq

Uµh

Zpqq

Xpp¹q

ν

_h¹

“ cos θ ν

h

` sin θ ν

µ

, ν

_µ¹

“ ´ sin θ ν

h

` cos θ ν

µ

, with sin θ “ U

µh

iM “ ´i U

µh

G

_F

? 2 upk

¹

qγ

^µ

p1 ´ γ

5

qupkq xX|J

µ

|N y .

(20)

General expression for the inclusive cross section:

dσ

dk

¹⁰

dΩ “ | ~ k

¹

|

|~ k|

|U

µh

|

²

G

²_F

32 π

²

L

_µν

W

^µν

Leptonic tensor

L

µν

“ Tr “

p { k

¹

` m

h

qγ

µ

p1 ´ γ

5

q { k γ

^ν

p1 ´ γ

5

q ‰ Hadronic tensor

W

^µν

” 1 2M

˜ ź

i

ż d

³

p

¹_i

p2πq

³

2E

_i¹

¸

p2πq

³

δ

^p4q

pk ` p ´ k

¹

´ p

¹

qH

^µν

H

^µν

“ ÿ

polar.

xX|J

^ν

|N y

^˚

xX|J

^µ

|N y

(21)

QE scattering on nucleons

Process ν

µ

` N Ñ ν

h

` N dσ

dt “ |U

µh

|

²

G

²_F

16 π M

²

k

²₀

“F

₁²

R

₁

` F

₂²

R

₂

` F

1

F

₂

R

_{1 2}

` F

_A²

R

_A

` F

_P²

R

_P

`F

A

F

₁

R

_{A 1}

` F

A

F

₂

R

_{A 2}

` F

A

F

_P

R

_{A P}

s ,

F

₁

, F

₂

, F

_A

, F

_P

are the weak nucleon form factors for neutral currents.

R1“ ´ m²_hp2s ` tq ` 2pM²´ sq²` 2st ` t²

R2“ 1 8M²

“´4m⁴_hM²` t²pm²_h` 8M²´ 4sq ´ tpm²_h` 2M²´ 2sq²‰

R1 2“2t²´ m²_hpm²_h` tq

RA“m²_hp4M²´ 2s ´ tq ` 2M⁴´ 4M²ps ` tq ` 2s²` 2st ` t²

RP“m²_ht pt ´ m²_hq 2M²

RA 1“RA 2“ 2tp2s ` t ´ m²_h´ 2M²q RA P“2m²_hpt ´ m²_hq

(22)

Coherent scattering on scalar nucleus

νµpkq νhpk¹q

Appq App¹q

Zpqq

dσ

dt “ |U

µh

|

²

G

²_F

32 π M

_A²

k

₀²

F

_W²

´

m

⁴_h

´ m

²_h

p4s ` tq ` 4

” `M

_A²

´ s ˘

2

` st ı¯

F

_W

is te weak form factor of the nucleus,

F

W

pQ

²

q “ F

p

pQ

²

q `1 ´ 4 sin

²

θ

W

˘ ´ F

n

pQ

²

q 2

F

_N

pq

²

q “ ż

d

³

r e

^i~q¨~r

ρ

_N

p~ rq

(23)

Incoherent scattering on scalar nucleus

Case of QE interaction with the nucleons forming the nucleus.

νµ ν_h

A X

Z

νµpkq

νhpk¹q

νµpkq N¹pp ` qq

N ppq

Zpqq Zpqq

With the local density approximation.

W^µν “ 1 4π

ż

d³r θpq⁰q ż d³p

4π²A^µνδ`p⁰` q⁰´ E p~p ` ~qq˘ nppq p1 ´ n p~p ` ~qqq p⁰pp⁰` q⁰` Ep~p ` ~qqqθpp⁰q

A^µν“Tr

"„

γ^νF1´ i

2Mσ^ναqαF2` γ^νγ5FA´q^ν Mγ5FP



`

{p ` {q ` MN

˘

ˆ

„

γ^µF1` i

2Mσ^µβq_βF2` γ^µγ5FA`q^µ Mγ5FP



` p ` M{ N

˘

*

(24)

Antineutrino production

Electromagnetic production

The antisymmetric part of L

_µν

changes sign but W

_µν

is symmetric Ñ same results as neutrino electromagnetic interaction.

Neutral current production

The antisymmetric part of L

µν

changes sign:

QE scattering with nucleons Ñ change of sign in the antisymmetric terms.

Coherent scattering with scalar nucleus Ñ same result as neutrino neutral current scattering.

Incoherent scattering with scalar nucleus Ñ change of sign in the antisymmetric

terms.

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Decay of the heavy sterile neutrino

νh

ν

γ

m

h

„ 50 MeV τ „ 5 ˆ 10

^´9

s

dΓ d cos θ

γ

“ pµ

ⁱ_tr

q

²

m

³_h

32π p1 ˘ cos θ

γ

q ;

"

EM ` N C´

θ

γ

is the angle of the photon respect the ν

h

spin direction.

Electromagnetic production flips quirality Ñ ν

hR

Neutral current production keeps quirality Ñ ν

hL

At high energies („ 1 GeV) contributions of other helicity components are

negligible.

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Number of photons inside the detector,

Nγ“ Mdet

Vdet

NANP OT

ÿ

t

ft

ż

dEνφpEνq ż

dk₀¹d cos θhdϕh

dσ dk¹₀d cos θhdϕh

ż d³r P

P pk¹₀, r, θ, ϕ, θh, ϕhq “ 1 ´ e^´∆l^λ

λ “ τ0c k₀¹ m_h

d 1 ´ m²_h

pk₀¹q²; τ0“ 1 Γ

We can calculate the energy and the angular distributions of the photons:

ν_µ νh

νµ νh

Detector

γ νi

γ ν_i

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Section 3 Results

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Parameters

Choice of parameters from M. Masip et al, JHEP 1301 (2013):

Mass of the heavy neutrino, m

h

“ 50 MeV Mixing angle, |U

µh

|

²

“ 3 ˆ 10

^´3

Lifetime, τ

h

“ 5 ˆ 10

^´9

s Branching ratio, BR

i

“

^pµ

i trq² ř

i

pµⁱ_trq²

Ñ BR

µ

“ 10

^´2

(29)

ν _h production cross sections

EM: dominated by the coherent mechanism

QE on proton Coherent on¹²C Incoherent on12C Total on¹²C

0.0 0.5 1.0 1.5 2.0 2.5 3.0

0 1 2 3 4 5

0.0 0.5 1.0 1.5 2.0 2.5 3.0

0 1 2 3 4 5

Eν(GeV) σ(×10-40cm2)

NC: dominated by the incoherent mechanism

QE on proton Coherent on¹²C Incoherent on¹²C Total on¹²C

0.0 0.5 1.0 1.5 2.0 2.5 3.0

0.0 0.1 0.2 0.3 0.4 0.5 0.6

0.70.0 0.5 1.0 1.5 2.0 2.5 3.0

0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7

Eν(GeV) σ(×10-40cm2)

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MiniBooNE

Fermi National Accelerator Laboratory is a with 149 m of diameter.

A 8 GeV protons beam is generated in FNAL and focused to a beryllium target.

A secondary beam of mesons is produced and filtered with magnetic fields

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MiniBooNE

Cherenkov detector.

Spherical tank with 12.2 m of diameter.

806 tons of mineral oil, CH

2

.

MiniBooNE measurements were made with:

6.46 ˆ 10

²⁰

POT in neutrino mode.

11.27 ˆ 10

²⁰

POT in antineutrino mode.

ν mode νμ

νμ

0.0 0.5 1.0 1.5 2.0

0.0 0.5 1.0 1.5 2.0 2.5 3.0

(ϕ×10-11/cm2/POT/50MeV)

ν mode νμ

νμ

0.0 0.5 1.0 1.5 2.0 2.5 3.0

0.0 0.5 1.0 1.5

Eν(GeV) (ϕ×10-11/cm2/POT/50MeV)

Aguilar-Arevalo et al, PRD 79 (2009)

(32)

MiniBooNE

Cherenkov detector.

Spherical tank with 12.2 m of diameter.

806 tons of mineral oil, CH

2

.

MiniBooNE measurements were made with:

6.46 ˆ 10

²⁰

POT in neutrino mode.

11.27 ˆ 10

²⁰

POT in antineutrino mode.

http://www-boone.fnal.gov/for_

physicists/data_release

(33)

Neutrino mode

Energy and angular distributions

Total QE on protons Coherent on¹²C Incoherent on¹²C MiniBooNE excess

0.0 0.5 1.0 1.5 2.0

0 100 200 300

0.0 0.5 1.0 1.5 2.0

0 100 200 300

Eγ(GeV)

dN dEγ[Events/(0.1GeV)] Total

QE on protons Coherent on¹²C Incoherent on¹²C MiniBooNE excess

-1.0 -0.5 0.0 0.5 1.0

0 200 400 600 800

-1.0 -0.5 0.0 0.5 1.0

0 200 400 600 800

Cos(θγ) dN dCos(θγ)(Events/0.2)

Energy and angular distributions with efficiency

Total

MiniBooNE excess

0.0 0.5 1.0 1.5 2.0

-20 0 20 40 60 80

0.0 0.5 1.0 1.5 2.0

-20 0 20 40 60 80

Eγ(GeV) dN dEγ[Events/(0.1GeV)]

Total

MiniBooNE excess

-1.0 -0.5 0.0 0.5 1.0

0 10 20 30 40 50 60 70

-1.0 -0.5 0.0 0.5 1.0

0 10 20 30 40 50 60 70

(34)

Neutrino mode

Energy and angular distributions

0.0 0.5 1.0 1.5 2.0

0 100 200 300

0.0 0.5 1.0 1.5 2.0

0 100 200 300

Eγ(GeV)

-1.0 -0.5 0.0 0.5 1.0

0 200 400 600 800

-1.0 -0.5 0.0 0.5 1.0

0 200 400 600 800

Energy and angular distributions with efficiency

Total

MiniBooNE excess

0.0 0.5 1.0 1.5 2.0

-20 0 20 40 60 80

0.0 0.5 1.0 1.5 2.0

-20 0 20 40 60 80

Eγ(GeV)

dN dEγ[Events/(0.1GeV)] _Total

MiniBooNE excess

-1.0 -0.5 0.0 0.5 1.0

0 10 20 30 40 50 60 70

-1.0 -0.5 0.0 0.5 1.0

0 10 20 30 40 50 60 70

(35)

Neutrino mode

Energy and angular distributions

0.0 0.5 1.0 1.5 2.0

0 100 200 300

0.0 0.5 1.0 1.5 2.0

0 100 200 300

Eγ(GeV)

-1.0 -0.5 0.0 0.5 1.0

0 200 400 600 800

-1.0 -0.5 0.0 0.5 1.0

0 200 400 600 800

Energy and angular distributions with efficiency

Total

MiniBooNE excess

0.0 0.5 1.0 1.5 2.0

-20 0 20 40 60 80

0.0 0.5 1.0 1.5 2.0

-20 0 20 40 60 80

Total

MiniBooNE excess

-1.0 -0.5 0.0 0.5 1.0

0 10 20 30 40 50 60 70

-1.0 -0.5 0.0 0.5 1.0

0 10 20 30 40 50 60 70

(36)

Antineutrino mode

Energy and angular distributions

0.0 0.5 1.0 1.5 2.0

0 100 200 300 400 500

0.0 0.5 1.0 1.5 2.0

0 100 200 300 400 500

Eγ(GeV)

-1.0 -0.5 0.0 0.5 1.0

0 200 400 600 800 1000

-1.0 -0.5 0.0 0.5 1.0

0 200 400 600 800 1000

Energy and angular distributions with efficiency

Total

MiniBooNE excess

0.0 0.5 1.0 1.5 2.0

-10 0 10 20 30

0.0 0.5 1.0 1.5 2.0

-10 0 10 20 30

Total

MiniBooNE excess

-1.0 -0.5 0.0 0.5 1.0

0 20 40 60

-1.0 -0.5 0.0 0.5 1.0

0 20 40 60

(37)

Parameters

Choice of parameters from M. Masip et al, JHEP 1301 (2013):

Mass of the heavy neutrino, m

_h

“ 50 MeV Mixing angle, |U

µh

|

²

“ 3 ˆ 10

^´3

Lifetime, τ

h

“ 5 ˆ 10

^´9

s Branching ratio, BR

_i

“

^pµ

i trq² ř

i

pµⁱ_trq²

Ñ BR

µ

“ 10

^´2

does not explain the MiniBooNE excess of events ñ χ

²

{DoF “ 127{54

(38)

Production and radiative decay of heavy neutrinos at the Booster Neutrino Beam 33 Results

MiniBooNE

Parameters and limits

LSND compatible limits for the parameters by Gninenko, PRD 83, 015015 (2011):

Mass of the heavy neutrino, m

h

:

Lower bound: m

h

ě 40 MeV Ñ KARMEN experiment.

Upper bound: m

h

ď 80 MeV Ñ LSND ν

h

production suppressed by phase space factor.

Mixing angle:

Lower bound: |U

µh

|

²

ě 10

^´3

Ñ muon lifetime.

Upper bound: |U

µh

|

²

ď 10

^´2

Ñ LEP experiments Z Ñ νν

h

decay Lifetime:

Upper bound: τ

h

ď 10

^´8

s Ñ Gninenko LSND results

m

_h

“ 68.6 MeV

|U

µh

|

²

“ 10

^´2

τ

h

“ 2.5 ˆ 10

^´9

s

BR

µ

“ 8.4 ˆ 10

^´4

ô EM ν

h

production strongly suppressed

(39)

Parameters and limits

LSND compatible limits for the parameters by Gninenko, PRD 83, 015015 (2011):

Mass of the heavy neutrino, m

h

:

Lower bound: m

h

ě 40 MeV Ñ KARMEN experiment.

Upper bound: m

h

ď 80 MeV Ñ LSND ν

h

production suppressed by phase space factor.

Mixing angle:

Lower bound: |U

µh

|

²

ě 10

^´3

Ñ muon lifetime.

Upper bound: |U

µh

|

²

ď 10

^´2

Ñ LEP experiments Z Ñ νν

h

decay Lifetime:

Upper bound: τ

h

ď 10

^´8

s Ñ Gninenko LSND results Our fit: χ

²

{DoF “ 101{54

m

_h

“ 68.6 MeV

|U

µh

|

²

“ 10

^´2

τ

h

“ 2.5 ˆ 10

^´9

s

BR

µ

“ 8.4 ˆ 10

^´4

ô EM ν

h

production strongly suppressed

(40)

Fitted parameters

Neutrino mode

Total

MiniBooNE excess

0.0 0.5 1.0 1.5 2.0

-20 0 20 40 60 80

0.0 0.5 1.0 1.5 2.0

-20 0 20 40 60 80

Eγ(GeV)

MiniBooNE excess

-1.0 -0.5 0.0 0.5 1.0

0 10 20 30 40 50 60

-1.0 -0.5 0.0 0.5 1.0

0 10 20 30 40 50 60

Antineutrino mode

Total

MiniBooNE excess

0.0 0.5 1.0 1.5 2.0

-10 0 10 20 30

0.0 0.5 1.0 1.5 2.0

-10 0 10 20 30

Total

MiniBooNE excess

-1.0 -0.5 0.0 0.5 1.0

-10 0 10 20 30 40

-1.0 -0.5 0.0 0.5 1.0

-10 0 10 20 30 40

(41)

SBN

(42)

MicroBooNE

LArTPC detector (large liquid argon time projection chamber).

TPC of 2.3 m ˆ 2.6 m ˆ 10.4 m.

Cylindrical deposit with 170 tons of liquid argon (active mass: 86.6 tons).

Same L{E as MiniBooNE approx.

Run plan of 6.6 ˆ 10

²⁰

POT.

ν

μ

ν

μ

0.0 0.5 1.0 1.5 2.0 2.5 3.0

Zarko Pavlovic, private communication.

(43)

MicroBooNE, parameters of Masip et al.

Neutrino mode

Total Coherent on⁴⁰Ar Incoherent on⁴⁰Ar

0.0 0.5 1.0 1.5

0 20 40 60 80 100 120

0.0 0.5 1.0 1.5

0 20 40 60 80 100 120

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150 200 250 300 350

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150 200 250 300 350

Antineutrino mode

0.0 0.5 1.0 1.5

0 20 40 60 80 100 120 140

0.0 0.5 1.0 1.5

0 20 40 60 80 100 120 140

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150 200 250 300 350

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150 200 250 300 350

(44)

MicroBooNE, fitted parameters

Neutrino mode

0.0 0.5 1.0 1.5

0 20 40 60

0.0 0.5 1.0 1.5

0 20 40 60

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150

Antineutrino mode

0.0 0.5 1.0 1.5

0 5 10 15 20 25 30 35

0.0 0.5 1.0 1.5

0 5 10 15 20 25 30 35

-1.0 -0.5 0.0 0.5 1.0

0 20 40 60 80 100 120

-1.0 -0.5 0.0 0.5 1.0

0 20 40 60 80 100 120

(45)

Neutrino mode

0.0 0.5 1.0 1.5

0 20 40 60

0.0 0.5 1.0 1.5

0 20 40 60

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150

Prediction for SM predominant photon emission from ∆p1232q Ñ nγ, Wang,

Alvarez-Ruso, Nieves, PRC89.015503 (2014)

(46)

LaR1-ND

LArTPC detector (large liquid argon time projection chamber).

TPC of 5 ˆ 4 ˆ 4 m.

Active mass: 112 tons.

Run plan of 6.6 ˆ 10

²⁰

POT.

ν

μ

ν

μ

0.0 0.5 1.0 1.5 2.0 2.5 3.0

0 20 40 60 80

(47)

LaR1-ND, fitted parameters

Neutrino mode

0.0 0.5 1.0 1.5

0 500 1000 1500 2000 2500 3000

0.0 0.5 1.0 1.5

0 500 1000 1500 2000 2500 3000

-1.0 -0.5 0.0 0.5 1.0

0 1000 2000 3000

4000-1.0 -0.5 0.0 0.5 1.0

0 1000 2000 3000 4000

Antineutrino mode

0.0 0.5 1.0 1.5

0 200 400 600 800 1000 1200

0.0 0.5 1.0 1.5

0 200 400 600 800 1000 1200

-1.0 -0.5 0.0 0.5 1.0

0 500 1000 1500 2000 2500

-1.0 -0.5 0.0 0.5 1.0

0 500 1000 1500 2000 2500

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ICARUS

LArTPC detector (large liquid argon time projection chamber).

TPC of 18 ˆ 3 ˆ 2 m.

2 TPC of 238 tons.

Run plan of 6.6 ˆ 10

²⁰

POT.

ν

μ

ν

μ

0.0 0.5 1.0 1.5 2.0 2.5 3.0

0.0 0.5 1.0 1.5

(49)

At each TPC of ICARUS, fitted parameters

Neutrino mode

0.0 0.5 1.0 1.5

0 50 100 150

0.0 0.5 1.0 1.5

0 50 100 150

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150 200 250 300 350

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150 200 250 300 350

Antineutrino mode

0.0 0.5 1.0 1.5

0 10 20 30 40 50 60 70

0.0 0.5 1.0 1.5

0 10 20 30 40 50 60 70

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150 200 250

-1.0 -0.5 0.0 0.5 1.0

0 50 100 150 200 250

(50)

Section 4 Conclusions

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Conclusions

The origin of MiniBooNE anomaly is still not understood.

Production and radiative decay of heavy sterile neutrino could be a solution.

We have made an analysis of this scenario using our understanding about neutrino interactions with matter.

In the range of parameter values consistent with LSND anomaly this scenario does not fully describe MiniBooNE anomaly, but could be sizable contribution.

We can predict the impact in SBN measurements and test the model.

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