Pyhäsalmi (site review) W. H. Trzaska on behalf of the Finnish LAGUNA team.

Slides:



Advertisements
Similar presentations
Fossil Fuels.
Advertisements

TIERRAS: an AIRES package to simulate high energy cosmic ray showers underground and underwater Matías Tueros Instituto de Física La Plata – Universidad.
AGASA Results Max-Planck-Institut für Physik, München, Germany Masahiro Teshima for AGASA collaboration at 3 rd Int. Workshop on UHECR, Univ. Leeds.
Underground Facilities Stub 2 Stub 2a,3 ‘H’ Area JIF Area The underground research facilities have evolved since dark matter studies began at Boulby. There.
Neutrino emission =0.27 MeV E=0.39,0.86 MeV =6.74 MeV ppI loss: ~2% ppII loss: 4% note: /Q= 0.27/26.73 = 1% ppIII loss: 28% Total loss: 2.3%
Cosmic Rays with the LEP detectors Charles Timmermans University of Nijmegen.
Particle Physics Design Group Studies Big Liquid Argon Neutrino Detector Subgroup Particle Physics Design Group Studies: The BLAND Subgroup BLAND.
EAS EXPERIMENT ON BOARD OF THE AIRBUS A380 J. N. Capdevielle, F. Cohen, PCC, College de France K. Jedrzejczak, B. Szabelska, J. Szabelski, T. Wibig The.
Low Energy Neutrino Astrophysics
AGASA update M. Teshima ICRR, U of CfCP mini workshop Oct
An accelerator beam of muon neutrinos is manufactured at the Fermi Laboratory in Illinois, USA. The neutrino beam spectrum is sampled by two detectors:
Searching for Atmospheric Neutrino Oscillations at MINOS Andy Blake Cambridge University April 2004.
Experimental Status of Geo-reactor Search with KamLAND Detector
Gravitational waves LIGO (Laser Interferometer Gravitational-Wave Observatory ) in Louisiana. A laser beam is.
21-25 January 2002 WIN 2002 Colin Okada, LBNL for the SNO Collaboration What Else Can SNO Do? Muons and Atmospheric Neutrinos Supernovae Anti-Neutrinos.
INDIA-BASED NEUTRINO OBSERVATORY (INO) STATUS REPORT Naba K Mondal Tata Institute of Fundamental Research Mumbai, India NUFACT Scoping Study Meeting at.
The neutrons detection involves the use of gadolinium which has the largest thermal neutron capture cross section ever observed. The neutron capture on.
Neutrino emission =0.27 MeV E=0.39,0.86 MeV =6.74 MeV ppI loss: ~2% ppII loss: 4% note: /Q= 0.27/26.73 = 1% ppIII loss: 28% Total loss: 2.3%
O Reactor antineutrinos in the world V. Chubakov 1, F. Mantovani 1, B. Ricci 1, J. Esposito 2, L. Ludhova 3 and S. Zavatarelli 4 1 Dip. di Fisica, Università.
LENA Low Energy Neutrino Astrophysics L. Oberauer, Technische Universität München LENA Delta EL SUD Meeting.
The ANTARES experiment is currently the largest underwater neutrino telescope and is taking high quality data since Sea water is used as the detection.
Fermilab Neutrino Beamline to DUSEL Mike Martens Fermilab PAC November 3, 2009.
EHE Search for EHE neutrinos with the IceCube detector Aya Ishihara for the IceCube collaboration Chiba University.
Jun Cao Institute of High Energy Physics, Beijing Daya Bay Neutrino Experiment 3rd International Conference on Flavor Physics, Oct. 3-8, 2005 National.
1 LENA Low Energy Neutrino Astronomy NOW 2010, September 6, 2010 Lothar Oberauer, TUM, Physik-Department.
The Elementary Particles. e−e− e−e− γγ u u γ d d The Basic Interactions of Particles g u, d W+W+ u d Z0Z0 ν ν Z0Z0 e−e− e−e− Z0Z0 e−e− νeνe W+W+ Electromagnetic.
Lino MiramontiJune 9-14, 2003, Nara Japan 1st Yamada Symposium Neutrinos and Dark Matter in Nuclear Physics.
Eun-Ju Jeon Sejong Univ. Sept. 09, 2010 Status of RENO Experiment Neutrino Oscillation Workshop (NOW 2010) September 4-11, 2010, Otranto, Lecce, Italy.
L. MoscaEPIPHANY Conf 6-8 Jan EPIPHANY Conference at Cracow “Physics in Underground Laboratories and its connection with LHC” - 6 to 8 January 2010.
O n t h e T r a c k o f M o d e r n P h y s i c s Wolfgang Pauli was a scientist with "NO" in his mind. Pauli's exclusion principle, that two electrons.
LAGUNA Large Apparatus for Grand Unification and Neutrino Astrophysics Launch meeting, Heidelberg, March 2007, Lothar Oberauer, TUM.
KamLAND : Studying Neutrinos from Reactor Atsuto Suzuki KamLAND Collaboration KEK : High Energy Accelerator Research Organization.
The NOvA Experiment Ji Liu On behalf of the NOvA collaboration College of William and Mary APS April Meeting April 1, 2012.
Present and future detectors for Geo-neutrinos: Borexino and LENA Applied Antineutrino Physics Workshop APC, Paris, Dec L. Oberauer, TU München.
L. Oberauer, Paris, June 2004   Measurements at Reactors Neutrino 2004 CdF, Paris, June chasing the missing mixing angle.
Krasnoyarsk underground neutrino laboratory V.P. Martemiyanov for NEUTRINO GROUP of Kurchatov Institute.
Application of neutrino spectrometry
Alexander Kappes Erlangen Centre for Astroparticle Physics for the ANTARES collaboration IAU GA, SpS 10, Rio de Janeiro, Aug Status of Neutrino.
J T Volk Fermilab April 2008 Ground Motion Studies at Fermi National Accelerator Laboratory James T Volk Applications Physicist II Vladimir Shiltsev, Shavkat.
Underground Physics Research in Finland
Mass Hierarchy Study with MINOS Far Detector Atmospheric Neutrinos Xinjie Qiu 1, Andy Blake 2, Luke A. Corwin 3, Alec Habig 4, Stuart Mufso 3, Stan Wojcicki.
The Daya Bay Reactor Neutrino Experiment R. D. McKeown Caltech On Behalf of the Daya Bay Collaboration CIPANP 2009.
1 GEMMA: experimental searches for neutrino magnetic moment JINR: V. Brudanin, V. Egorov, D. Medvedev, M. Shirchenko, E. Shevchik, I. Zhitnikov, V. Belov.
Detection of the Diffuse Supernova Neutrino Background in LENA & Study of Scintillator Properties Michael Wurm DPG Spring Meeting, E15.
HAWC Science  Survey of 2  sr (half the sky) up to 100 TeV energies Probe knee in cosmic ray spectrum Identify sources of Galactic cosmic rays  Extended.
PHY418 Particle Astrophysics
Double Chooz Near Detector Guillaume MENTION CEA Saclay, DAPNIA/SPP Workshop AAP 2007 Friday, December 14 th, 2007
June 6, 2006 CALOR 2006 E. Hays University of Chicago / Argonne National Lab VERITAS Imaging Calorimetry at Very High Energies.
Daya Bay Reactor Neutrino Experiment On behalf of the DayaBay collaboration Virginia Polytechnic Institute and State University Joseph ykHor YuenKeung,
Cosmic ray physics in ALICE Katherin Shtejer Díaz For the ALICE Collaboration LatinoAmerican Workshop on High Energy Physics: Particles and Strings, Havana,
E. W. Grashorn and A. Habig, UMD, for the MINOS Collaboration The Detectors of The Main Injector Neutrino Oscillation Search (MINOS) Experiment The MINOS.
  Measurement with Double Chooz IDM chasing the missing mixing angle e  x.
ENERGY RESOURCES 14-2 Objective: To know some of Earth’s natural resources can be used for energy, usually through conversion to electricity.
2 July 2002 S. Kahn BNL Homestake Long Baseline1 A Super-Neutrino Beam from BNL to Homestake Steve Kahn For the BNL-Homestake Collaboration Presented at.
2 protons 2 neutrons Energy of a nucleus The mass of a helium nucleus is slightly smaller (
NUMI NUMI/MINOS Status J. Musser for the MINOS Collatoration 2002 FNAL Users Meeting.
NEVOD-DECOR experiment: results and future A.A.Petrukhin for Russian-Italian Collaboration Contents MSU, May 16, New method of EAS investigations.
The Large High Altitude Air Shower Observatory LHAASO.
High Energy Observational Astrophysics. 1 Processes that emit X-rays and Gamma rays.
Pump Storage Power Plant Pyhäsalmi Concept - Background and current status Ari Aalto LAGUNA – LBNO General Meeting Paris
1 Cosmic Ray Physics with IceTop and IceCube Serap Tilav University of Delaware for The IceCube Collaboration ISVHECRI2010 June 28 - July 2, 2010 Fermilab.
Observation Gamma rays from neutral current quasi-elastic in the T2K experiment Huang Kunxian for half of T2K collaboration Mar. 24, Univ.
CHANDLER Detector Neutronics Modeling Alireza Haghighat William Walters Nuclear Science and Engineering Lab (NSEL) Nuclear Engineering Program, Mechanical.
LAGUNA Design of a pan- European Infrastructure for Large Apparatus studying Grand Unification and Neutrino Astrophysics Guido Nuijten.
The “Carpet-2” multipurpose air shower array of the Baksan Neutrino Observatory INR of RAS A.U. Kudzhaev Institute for Nuclear Research, Russian Academy.
HAWC Science Survey of 2p sr up to 100 TeV energies Extended Sources
Daya Bay Neutrino Experiment
EMMA-experiment (Experiment with MultiMuon Array) Juho Sarkamo
Intae Yu Sungkyunkwan University (SKKU), Korea KNO 2nd KNU, Nov
Low Energy Neutrino Astrophysics
Presentation transcript:

Pyhäsalmi (site review) W. H. Trzaska on behalf of the Finnish LAGUNA team

 125 km 2 of the lake (Pyhä-järvi = Holy-lake)  6000 inhabitants around the shores 60 % in Pyhäsalmi and Ruotanen 60 % in Pyhäsalmi and Ruotanen The deepest mine in Europe The deepest mine in Europe  In 1993, after administrative decision, Pyhäjärvi became the 5 th largest town in Finland (by area)! Located close to the geometrical center of Finland; Half way between Jyväskylä and Oulu

Productivity of the Pyhäsalmi mine

EMMA Experiment with MultiMuon Array - a cosmic ray experiment located in the mine

50 m 1-layer 3-layer Parking etc. 10 m EMMA (at the depth of 75 m)  50 m 

CUPP Surfrace Lab

CUPP Surface Lab

What is required of a LAGUNA site?  Quality of the rock  Ready infrastructure  Low background from nuclear power plants (essential for geo- and supernova diffusion neutrinos)  Seismic stability  Presence of scientific activity on site  Experienced industrial partner

Bedrock zones on Earth:  Red: very old bedrock, hard crystalline rock usually very good usually very good  Green: mobile belts (mountains, etc.), hard rock fair / variable fair / variable  White: sedimentary covers (soft rock) often bad often bad

Seismic levels

Pyhäsalmi mine

This tunnel would be extended 500 m to the proposed LENA site

Dry, room temperature conditions at the 1400m level (below the ground)

Samples drilled from the LENA tunnel

All 3 LAGUNA detectors could be placed in Pyhäsalmi

All caverns are within mine territory! MEMPHYS GLACIER

Nuclear power plants in Europe (2008)

Reactor neutrinos Fuel composition: 235 U, 238 U, 239 Pu, 241 Pu Reactor: -Produces electron antineutrinos -Production rate: ~2e20 GW -1 s -1 -prop. to thermal power Propagation through the Earth -Neutrino oscillation -Matter effects negligible Detection: -via inverse  -decay (E thr ≈ 1.8 MeV) Background for geo- and supernova diffusion neutrinos

Neutrino Background from Power Plants based on 2008 data Measured spectra of reactor neutrinos for U-235,Pu-239 and Pu-241 were used. For U-238 calculated spectra were used. Event rates were calculated for a KamLand-type scintillator det.

Olkiluoto 3 (to open in 2012) EPR (European Pressurized water Reactor) 4.3 GW Thermal 1.6 GW Electrical

Geo- luminosity of the Earth U-238: Total: 6.65 Above E thr : 0.43 Th-232: Total: 5.30 Above E thr : Luminosities [x /s ]

Effect of reactor neutrinos on Geo-neutrino background Geo -window U + Th: MeV U only: MeV

Rockplan Ltd – Finnish industrial partner Underground coal storage for Helsingin Energia, m3 District cooling station for Helsingin Energia, m3 SALMISAARI underground coal storage

The underground silos are each 65 m-high x 40 m-diameter with circular plan cross-section. The volumetric capacity of each silo is m3. The Salmisaari coal transport tunnel will be re-equipped to charge the silos and a newly-mined conveyor retrieval tunnel will be used to discharge the coal. SALMISAARI underground coal storage

Summary: Phyäsalmi fulfills all LAGUNA requirements  Quality of the rock (the best)  Low reactor background (the lowest)  Low seismic activity (the lowest)  Ready infrastructure (all in place)  Clear legal status (signed MoU; all excavation within the mine area)  All LAGUNA detectors can be located in Pyhäsalmi (the only site with this distinction?)  Experienced industrial partner (Rockplan Ltd.)  Competitive excavation & operation costs (yes!)  Local support (enthusiastic!)

Thank you for your attention! ν

Backup

Reactor background vs. calculated Geo-neutrino flux [events/a/kton] (1.8 – 3.3 MeV)

What can be deduced from muons registered underground? 50 GeV cutoff  Energy of the initial CR particle Muon density at the core Muon density at the core  Approximate Z (but not on the event-by-event basis) Lateral distribution Lateral distribution

Example of muon distribution induced by a 4 PeV proton

Simulated change of p / Fe ratio from 80/20 to 20/80 reconstructed by EMMA after 12 months running