LAGUNA

Large Apparatus for Grand Unification and Neutrino AstrophysicsLaunch meeting, Heidelberg, March 2007, Lothar Oberauer, TUM

Why ?Neutrinos oscillations =>

New Particle Physics Main line besides future accelerator

experiments Baryon number violation ? => Nucleon

decay (Search for Proton Decay) Baryon asymmetry Leptogenesis ?

CP violation in leptonic sector ?(Long Baseline Neutrino Experiments)

AstrophysicsNew Neutrino Observatories wanted

Neutrinos as probes

Study of gravitational collapse (Supernova Neutrinos)

Study of star formation in the early universe (Diffuse Supernovae Neutrinos Background)

Precision study of thermonuclear fusion processes (Solar Neutrinos)

Test of geophysical models (Geoneutrinos)

LENA

Low Energy Neutrino Astronomy Diffuse Supernovae Neutrino Background Supernova Neutrinos Solar Neutrinos Geoneutrinos Proton Decay

LENA: Diffuse SN Backgrounde + p -> e+ + n

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

Rates depend on: supernova model, star formation rate, neutrino mass hierarchy

Range 20 to 220 / 10 years

“most probable” value ~ 100

M. Wurm et al., Phys. Rev D 75 (2007) 023007

Information on Supernova models & Star Formation rate (z~2)

LENA: Diffuse SN Background optical measurements will determine the SNR with high accuracy with this input, the spectral slope of the DSN can be used to distinguish between different SN explosion scenarios

comparison of count ratesin the energy bins10MeV < EB1 < 14MeV15MeV < EB2 < 25MeV

LENA: Supernova NeutrinosAssumption: Supernova II with 8 solar masses at 10 kpc distance

e flux and spectrum

e flux and spectrum

LENA: Supernova Neutrinos

Total neutrino flux

Total energy spectrum

LENA: Supernova Neutrinos

Depending on threshold: p, nu - scattering dominated by

and

pp

Threshold ~ 50 pe

(photoelectrons)

LENA: Solar Neutrinos

• High statistic ( ~ 5.4 x 103 / day ) 7Be + e + e

test of small flux fluctuations in time

• CNO and pep – neutrinos ( ~ 3 x 102 / day )

solar neutrino luminosity

contribution of CNO cycle to solar energy release

• Charged current e (13C,13N) e- reaction ( ~ 103 / year )

spectroscopy of 8B- at energies below 5 MeV

(A. Ianni et al., hep-ph/0506171)

LENA Fiducial Volume for solar : 18 x 103 m3

LENA: Solar Neutrinos

7Be pep CNO

8B

Standard MSW scenarioNon standard Interactions ?

(e.g. flavor changing neutral currents)

Friedland, Lunardini, Peña-Garay, hep-ph/0402266

CNO and the age of Globular Clusters

14N(p,)15O new value? (new result from LUNA)

Prediction CNO- altered by factor ~2

Age of Globular Clusters increased by factor 0.7 bis 1 Gy !

Measurement of CNO - : determination of metallicity in the centre of the Sun

LENA: Solar Neutrinos

Electron recoil spectrum

Requirements:

low background levels in U, Th, 210Pb

at least ~4000 m.w.e. shielding

LENA: Geo Neutrinos

• Detection via inverse beta decay

• measurement of radiogenic contribution to terrestrial heat (~ 40 TW)

• test of the Bulk Silicate Earth model

• test of unorthodox models of Earth‘s core (is there a breeder reactor ?)

LENA @ Pyhäsalmi: ~ 1.5 x 103 events / year

Scaling KamLAND result to LENA:

between 3 x 102 and 3 x 103 events / year

Rate of Geo-neutrinos in LENA

Positron spectrum (arb. units)

Uranium

Uranium + Thorium

Reactor BG

Proton Decay in Supersymmetry SU(5)

GUT scale:

Preferred decay modes:

–y (S.Raby et al, 2002) y (Babu, Pati, Wilzcek, 1998)

Proton Decay(non SUSY)

(P. Nath 2006)

Limits from SuperKamiokande:

LENA: Proton Decay

LENA: Proton Decay

LENA: Separartion e- -like events ?

Conclusions

• LAGUNA – Design study for a large future European observatory (Water, Argon, Scintillator)

design study until ~ 2011

on APpec road map for Launch after design study completed

• LENA – Physics Potential in Low Energy Neutrino Astronomy and Proton Decay

Proton Decay: T. Marrodan-Undagoitia et al., Phys. Rev. D 72 (2005) 075014

Geo-Nus: K.. Hochmuth et al., Astropart. Phys. 27 (2007) 21

DSNB: M. Wurm et al., Phys. Rev. D 75 (2007) 023007