LAGUNA and Neutrino Physics NOW 2008 Lothar Oberauer TU München, Germany.

LAGUNA and Neutrino Physics

NOW 2008Lothar Oberauer

TU München, Germany

LAGUNA Physics Large Apparatus for Grand Unification

and Neutrino Astrophysics Proton Decay Neutrinos as probes

Supernova neutrinos Solar neutrinosGeoneutrinos

Neutrino properties

LAGUNA Physics Detecting proton decay implies de

facto discovery of Grand Unification (GU)

GU: new symmetry between quarks and leptons

GU: guide of fermion masses and mixing GU: one motivation for SUSY => LSP is

Dark Matter candidate GU: motivation for See-Saw => small

masses

LAGUNA Physics Galactic Supernova neutrino burst

understanding of gravitational collapseneutrino properties: and mass hierarchymass effects on flavor transitions within the supernova and when passing through the Earthearly alert for astronomersBlack Hole formation?

Diffuse Supernova neutrinoslink to supernova rates => star formation rate; probing models of gravitational collapse

LAGUNA Physics Solar neutrinos

Search for small flux variations in timePrecise measurements of thermo nuclear fusion reactionsmeasurement of inner solar metallicity (CNO neutrinos at high statistics)

Neutrino beamsSearch for

Search for leptonic CP-violation (if is not to small)

LAGUNA Physics

Complementary to LHC and planned ILC goals

LHC: Higgs mechanism, SUSY, Rare decays

LAGUNA: Proton decay, neutrino astronomy, CP violation in leptons

LAGUNA European ApPEC roadmap recommendation:

We recommend that a new large European infrastructure is put forward, as a

future international multi-purpose facility on the 105-106 ton scale for improved

studies of proton decay and of low-energy neutrinos from astrophysical

origin

LAGUNA structure and aims Proposed and accepted in the ApPEC

meeting at Munich in November 2005 Investigate common R&D requirements Coherent work on common problems Take advantage of acquired technological

know-how in Europe Kick-off meeting at ETH Zurich 3-4 July 07 Mature design and proposals should

emerge in 2010

LAGUNA financial situation

• Design Study for future European observatory• Volume of proposal 5 M€• Approved as a whole by the European Commission (EC)• Funding: 1.7 M€• Focus on the part of the programme which cannot be performed on a national (regional) basis• Underground Sites infrastructure studies• 2008 until 2010

LAGUNA Collaboration

- Italy

LAGUNA CollaborationConsortium composed of 21 beneficiaries

9 university entities (ETHZ, U-Bern, U-Jyväskylä, U-OULU, TUM, UAM, UDUR, USFD, UA)

8 research organizations (CEA, IN2P3, MPG, IPJ PAN, KGHM CUPRUM, GSMiE PAN, LSC, IFIN-HH)

4 SMEs (Rockplan, Technodyne, AGT, Lombardi)

Additional university participants (IPJ Warsaw, U-Silesia, U-Wroclaw, U-Granada)

LAGUNA Detector types

Mt Water CherencovMEMPHIS

100kt Liquid ArgonGLACIER

50kt liquid ScintillatorLENA

MEMPHIS

TRE

MEMPHYS

1 shaft = 215 kt

water target

Possible location: extension of Frejus laboratory

Ongoing R&D for single photo detection

Synergy with HK (Japan) and UNO (USA)

MEMPHIS PROS

“Simple” DetectorLarge and useful experiences (SuperK)

CHALLENGESHuge amount of photo-sensors (>100,000)Very large underground cavitiesCosts?

Imaging with SuperK water Cherenkov detector

GLACIER: Liquid argon scintillation and electron TPC

φ≈70 m

h =20 mMax drift length

Passive perlite insulation

GLACIER

Liquid Argon TPC -> 10 to 100 kt target mass Pioneering work in ICARUS R&D

program Two independent programs:

GLACIER in Europe and LARTPC in USA

GLACIER PROS

Brilliant energy and track resolutionParticle ID and separationBasically background free for many applications

CHALLENGES“complicated” detector technologyHuge number of channels (depending on position resolution)Large span of the cavity

LENA: Liquid scintillator

LENA Low Energy Neutrino Astronomy -> 50 kt target mass R&D on liquid scintillators BOREXINO successful in measuring

solar neutrinos (7Be, 8B) DOUBLE-CHOOZ in France Hanohano project (10 kt at Hawai)

in USA

LENA

PROSMature technologyGood energy and position resolutionCavity, PMs electronics standard(size like SuperK, also number of PMs)

CHALLENGESKeep purity like BOREXINO but for 50 kt(relevant for solar neutrino detection in the sub-MeV range)

Sensitivities on Proton Decay p -> e+

Water Cherenkov MEMPHIS ca. 1035 y (5000 kt y exposure)Limit SK-I and II: xy

p -> K+ Liquid Argon GLACIER ca. 1035 y (1000 kt y exposure)Liquid Scintillator LENA ca. 5 x 1034 y (500 kt y exposure)Limit SK-I: xy

Sensitivity on Supernova MEMPHIS mainly sensitive on e

Approx. rate for 1 Mt:

~ 40 events @ 1 Mpc

Prop. < 10% per year

~ 4 events @ 3.3 Mpc

Prop. ~ 15% per year

~ 0.4 events @ 10 Mpc

Prop. ~ 80% per year

Sensitivity on Supernova

Sensitive on e !

Important for neutronisation phase

Sensitive on oscillation parameter and mass hierarchy

Sensitivity on Supernova

DSNB Detection via inverse beta decay Free protons as target

nepe • Threshold 1.8 MeV

• E~ Ee - Q ( spectroscopy)

• suppress background via delayed coincidence method

n + p D + (2.2 MeV)

• position reconstruction => fiducial volume (suppress external background)

Delayed signal (~200 s)

Prompt signal

LENA at Pyhäsalmi (Finland)

dependent on SN model(assumed fSN=2.5)

LL:LL: 113113KRJ:KRJ: 100100TBP:TBP: 6060

dependent on SNR

ffSNSN=0.7=0.7 17 17ffSNSN=2.5=2.5 100 100ffSNSN=4.2=4.2 220 220

DSN event rate in 10yrsinside the energy window

from 9.7 to 25 MeV

background events: 13~25% of events are due to v’soriginating from SN @ z>1!

TU München

Outline DSNB Background Event Rates Spectroscopy

Solar Neutrinos

8B neutrinos: MEMPHIS, GLACIER, LENA

CNO and pep: LENA (~ 300 / d)

7Be: LENA (~ 6000/ d)

Precise measurement of LMA prediction

Accurate measurement of inner solar metallicity

Search for small flux variations

GEO Neutrinos LENA

rate between 3 x 102 and 3 x 103 per year (at Pyhäsalmi, Finland)

Background ~ 240 per year in

[1.8 MeV – 3.2 MeV] from reactor neutrinos< 30 per year due to 210Po alpha-n reaction on 13C (Borexino purity assumed)~ 1 per year due to cosmogenic background (9Li - beta-neutron cascade)

Can be statistically subtracted

Long baseline oscillations

CPsign(M2)

e e

High Intensity conventional neutrino source.

“Superbeams”

Time scale > 2014 (?)

New neutrino source. “Betabeams, nu-factory”

Time scale ~ 2020 (?)

31

Laboratorio Subterraneo de Canfranc, Spain

LSCLSC

Laboratori Nazionali delGran Sasso, Italy

LNGS

SUNLABPolkowice-Sieroszowice,

Poland

Institute of UndergroundScience in Boulby mine, UK

IUS

Laboratoire Souterrainde Modane, France

L=630 L=630 kmkm

L=130 L=130 kmkm

L=2300

L=950

L=732 L=732 kmkm

L=1050 L=1050 kmkm

Long baseline oscillations

Study J-Parc -> Okinoshima

Distance 653 km

Power 1.66 MW

Measurement 5 years

(arXiv:0804.2111)

Similar results for ~ 300 kt Water Cherenkov (fiducial mass)

LENA and Reactor neutrinos

At Frejus ~ 17,000 events per year High precision on solar oscillation

parameter: m2

12

S.T. Petcov, T. Schwetz, Phys. Lett. B 642, (2006), 487

J. Kopp et al., JHEP 01 (2007), 053

LENA and indirect Dark Matter search

Light Wimp mass between 10 and 100 MeV

Annihilation under neutrino emission in the Sun

Monoenergetic electron-antineutrino detection in LENAS. Palomares-Ruiz, S. Pascoli, Phys. Rev. D 77, 025025 (2008)

Conclusions

LAGUNA started July 2008 Physics program aims on GUT (p-

decay), LE astrophysics, oscillations High discovery potential Site studies for 7 candidates until 2010 LAGUNA is European but open for

world wide cooperation