Plans for future neutrino oscillation beams in Europe

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ESSνSB Project for Leptonic CP Violation Discovery based on the European Spallation Source Linac

Marcos DRACOS

IPHC-IN2P3/CNRS Université de Strasbourg

(2)

European Spallation Source

under pre-construction phase (~1.8 B€ facility)

(3)

ESS proton linac

• The ESS will be a copious source of spallation neutrons

• 5 MW average beam power

• 125 MW peak power

• 14 Hz repetition rate (2.86 ms pulse duration, 10¹⁵ protons)

• 2.0 GeV protons (up to 3.5 GeV with linac upgrades)

• >2.7x10²³ p.o.t/year

Linac ready by 2023 (full power and energy)

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How to add a neutrino facility?

• The neutron program must not be affected and if possible synergetic modifications

• Linac modifications: double the rate (14 Hz

→ 28 Hz), from 4% duty cycle to 8%.

• Accumulator (ø 143 m) needed to compress to few μs the 2.86 ms proton pulses,

affordable by the magnetic horn (350 kA, power consumption, Joule effect)

• H^- source (instead of protons)

• space charge problems to be solved

• ~300 MeV neutrinos

• Target station (studied in EUROnu)

• Underground detector (studied in LAGUNA)

• Short pulses (~μs) will also allow DAR

neutrino flux at 100 km (similar spectrum than for EU FP7 EUROν SPL SB)

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Previous Expertise

ESSνSB ESSνSB

BENE (2004-2008)

ISS (2005- 2007) ISS (2005-

2007)

EUROν (2008-2012)

EUROν

(2008-2012) LAGUNA (2008-2010)

LAGUNA (2008-2010)

LAGUNA- LBNO (2010-2014)

SNS (USA) SNS (USA)

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ESS neutrino energy distribution ESS neutrino energy distribution

at 100 km from the target and per year

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Possible locations for far detector

CERN

ESS

Kongsberg Løkken

LAGUNA sites

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The MEMPHYS WC Detector

( MEgaton Mass PHYSics)

• Proton decay

• Astroparticles

• Understand the gravitational collapsing: galactic SN ν

• Supernovae "relics"

• Solar Neutrinos

• Neutrino Oscillations (Super Beam, Beta Beam)

• Atmospheric Neutrinos

• 500 kt fiducial volume (~20xSuperK)

• Readout: ~240k 8” PMTs

• 30% optical coverage

(arXiv: hep-ex/0607026)

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Neutrino spectra

540 km (2 GeV) below ν_τ production

neutrinos anti-neutrinos

2 years 8 years

δ_CP=0

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CP Violating Observables CP Violating Observables

matter effect

⇒ accessibility to mass hierarchy

⇒ long baseline

Non-CP terms

CP violating

≠0 CP Violation⇒

be careful, matter effects also create asymmetry

atmospheric solar

interference

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Neutrino Oscillations with "large" θ

₁₃

P (ν

μ

→ ν

e

)

L/E 1^st oscillation maximum

2^nd oscillation maximum

θ₁₃=1º

("small" θ₁₃)

θ₁₃=8.8º

("large" θ₁₃)

for small θ₁₃ 1^st oscillation maximum is better

for "large" θ₁₃ 1^st oscillation maximum is dominated by atmospheric term,

CP interference CP interference

solar

solar atmospheric

atmospheric

θ₁₃=1º θ₁₃=8.8º

d_CP=-90 d_CP=0 d_CP=+90

(arXiv:1110.4583)

more sensitivity at 2^nd oscillation max.

L/E

L/E L/E

• 1^st oscillation max.: A=0.3sinδ_CP

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ESS Neutrino Super Beam ESS Neutrino Super Beam

arXiv:1212.5048 arXiv:1309.7022

14 participating institutes form 10 different countries, among them ESS and CERN

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Which baseline?

Zinkgruvan Garpenberg

• Zinkgruvan is better for 2 GeV

• Garpenberg is better for > 2.5 GeV

• systematic errors: 5%/10%

CPV MH

• Zinkgruvan is better

• atmospheric neutrinos are needed

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2nd Oscillation max. coverage 2nd Oscillation max. coverage

2^nd oscillation max.

well covered by the ESS neutrino spectrum

1^st oscillation max.

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Systematic errors

Phys. Rev. D 87 (2013) 3, 033004 [arXiv:1209.5973 [hep-ph]]

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δ CP accuracy performance

(USA snowmass process, P. Coloma)

for systematic errors see:

• Phys. Rev. D 87 (2013) 3, 033004 [arXiv:1209.5973 [hep-ph]]

• arXiv:1310.4340 [hep-ex] Neutrino "snowmass" group conclusions

"default" column

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Systematic errors and exposure

for ESSnuSB systematic errors see 1209.5973 [hep-ph] (lower limit

"default" case, upper limit "optimistic" case)

P5 requirement: 75% at 3 σ

Neutrino Factory reach

10 years 20 years

(courtesy P. Coloma)

High potentiality

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Conclusions

• For CP Violation intense neutrino beams are needed.

• Significantly better sensitivity at the 2

^nd

oscillation maximum.

• The European Spallation Source Linac will be ready in 10 years

• Neutrino Super Beam based on ESS linac is very promising.

• ESS will have enough protons to go to the 2

^nd

oscillation maximum and increase its CPV sensitivity.

• CPV: 5 σ could be reached over 60% of δ

_CP

range (ESSνSB) with large potentiality.

• Large associated detectors have a rich astroparticle physics program.

• Full complementarity with a long baseline experiment on the 1

^st

oscillation maximum using a LAr detector.

• A feasibility Design Study is now proposed.

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Backup

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Asymmetry due to matter effects Asymmetry due to matter effects

distance [km]

• E

_ν

=3 GeV

• δ

_CP

=0

Normal Hierarchy (NH) Inverted Hierarchy (IH)

good position to measure MH

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Neutrino Oscillations with "large" θ

₁₃

2^nd oscillation maximum is better

• at the 1^st oscillation max.: A=0.3sinδ_CP

• at the 2^nd oscillation max.: A=0.75sinδ_CP

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₁₃

L/E P(ν μ→ν e)

10º 30º

60º 90º 1^st oscillation max.

2^nd oscillation max.

using present oscillation parameters

more sensitive to 2^nd oscillation max.

But, to go to the 2^nd oscillation max. we must be very rich in protons…

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Physics Performance for ESSνSB

(Enrique Fernantez, Pilar Coloma)

• for 2 GeV

• optimum 300-400 km

• for 3.5 GeV

• optimum 500-600 km

• but the variation is small

• CPV discovery implies

exclusion at 5 σ of 0º and 180º

• high δ_CP resolution around these values is needed

• 1º gain around these values increase the discovery δ_CP range by ~4x5x1º (1^st approx.) δ_CP precision (unknown MH)

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Which baseline?

discovery potential

(unknown mass hierarchy)

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The MEMPHYS Detector

(Proton decay)

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The MEMPHYS Detector

(Supernova explosion)

For 10 kpc: ~10

⁵

events

SUPERK

MEMPHYS

Diffuse Supernova Neutrinos

(10 years, 440 kt)