Lino Miramonti – 8 Feb 2007 – Campinas - Sao Paulo (Brasil)1 European underground laboratories...

Lino Miramonti – 8 Feb 2007 – Campinas - Sao Paulo (Brasil) 1

European underground laboratories for Astroparticle Physics

Lino Miramonti – 8 Feb 2007

Campinas - Sao Paulo (Brasil)


Particle physics

Astrophysics&

CosmologyAstroparticle

physics

What Astroparticle Physics is?

Detects particles coming from space for particle physics studies

Employs knowledges and techniques from particle physics in order to study cosmological and astrophysical aspects


Neutrino Physics (Solar, Supernova, Atmospherics, Geoneutrinos, neutrinos from reactors and from accelerators, etc..)

Cosmic Ray Physics Rare Processes (double beta decay, proton decay etc..) Dark Matter (WIMP’s) Gravitational Waves Nuclear Physics (Cross section measurements of astrophysics interest) …….

Very little cross sections and/or

very rare processes

means to shield the detector apparatus from cosmic radiation

Typical studies of astroparticle physics are:

Undergroundlaboratories


UndergroundLaboratories

in Europe


LNGSLNGS - Laboratori Nazionali delGran Sasso, Italy

http://www.lngs.infn.it/


3 main halls A B C 100 x 18 m2 (h.20 m)

Muon Flux (μ m-2 day-1) 24

Neutron Flux (> 1 MeV) (10-6 n cm-2 s-1) O(1)

Radon (Bq/m3) 0(100)

Operating Institution

Istituto Nazionale di Fisica Nucleare (INFN)

Location Gran Sasso Tunnel (Abruzzi, Italy)

Excavation 1987

Underground area 3 halls A B C (100m x 18m x h 20m) + service tunnels

Depth 1400 m (3800 mwe)

Total volume 180000 m3

Surface > 6000 m2

Permanent staff 66 (physicists, technicians, administration)

Scientists users 450


Completed experiments

Atm ν, Monopoles MACRO (Streamer tubes + Liquid scintillators)Solar neutrinos GALLEX / GNO (~ 30 T Gallium radiochemical detector)ββ Heidelberg-Moscow (~ 11 kg enriched 76Ge detectors)

Mibeta (~ 7 kg Bolometers TeO2)Dark Matter DAMA (~ 100 kg NaI detectors)


Running experiments

ββ Cuoricino (~ 41 kg TeO2 crystals)Dark Matter CRESST (Sapphire cryodetector & CaWO4 crystals (phonons+scintillation))

LIBRA (~ 250 kg NaI crystals)WARP (Liquid Argon)HDMS (Ge detector 73Ge enriched)XENON10 (10 kg Xe TPC)

Supernova neutrinos LVD (Streamer tubes + Liquid scintillator)Nuclear astrophysics LUNA (Accelerator 50-400 kV)


Under construction

CERN-GS beam ν OPERA (Emulsion)ICARUS (~ 600 T Liquid Argon)

Solar Neutrinos Borexino (~ 300 T Liquid scintillator)

Planned & proposed

ββ CUORE (~ 750 kg Te02)GERDA (76Ge)COBRA (116Cd and 130Te)

Nuclear astrophysics LUNA-IIIGravitational waves LISA R&DDark matter Liquid Ar (TPCs)

XENON100 (100 kg Xe TPC)


LSMLSM - Laboratoire Souterrainde Modane, France

http://www-lsm.in2p3.fr/


Operating Institutions

CEA/DSM & CNRS/IN2P3

Location Fréjus Tunnel (Italian-French border)

Excavation 1983

Underground area

1 main hall (30m x 10m x 11m) + gamma spectroscopy hall (70 m2) + 2 secondary halls of 18 m2 and 21 m2

Depth 1700 m (4800 mwe)

Surface > 400 m2

Permanent staff 4

Scientists users 100

1 Main hall 30 x 10m2 (h 11m) + gamma spectr. hall (70 m2) + 2 secondary halls of 18 m2 and 21 m2



Radon (Bq/m3) O(10)


Completed experiments

p decay & Atm ν Frejus proton decay exp (Fe and flash chamber).ββ NEMO-I (prototype NemoIII)

NEMO-II (prototype NemoIII)TGV (Stack of Ge detectors with sheets of DBD candidates)

Dark Matter EDELWEISS-I (1 kg Ge bolometer heat+ionization)

Running experiments and Under construction

ββ NEMO-III (Tracking + calorimeter)Dark Matter EDELWEISS-II (10 to 35 kg Ge heat+ioniz.)


LSCLSC - Laboratorio Subterraneo de Canfranc, Spain

Tobazo's peak http://ezpc00.unizar.es/lsc/index2.html


Canfranc railway

tunnel entrance

Operating Institutions

Zaragoza University

Location Railway tunnel of Somport (Canfranc, Pyrenes) 7.5 km

Excavation 1986 [lab1] – 1994 [lab3]

Underground area

2 small halls [lab1] + Main hall [lab3]

Depth 900 m (2450 mwe) [lab3]

Surface 118 m2 [lab3]

Permanent staff 7

Scientists users 35

2 small halls [Lab1] 36 m2 + 1 Main hall [Lab3] 20 x 5 m2 (h 4.5 m)

Mobile Lab (now dismounted)

Now used only to store materials



Radon (Bq/m3) O(100)


Completed & Running experiments

ββ IGEX-2β (~ 9 kg enriched Ge detectors)Dark Matter IGEX-DM (~ 2 kg enriched Ge detectors)

ANAIS (NaI Crystals)ROSEBUD (Bolometers: Sapphire, Ge, BGO, CaW04)

Under construction

ββ GEDEON (Set of Ge crystals 30-90 kg) Dark Matter ROSEBUD I (Bolom and Scint)

ArDM (Liq Ar)


Main HallMain Hall40 x 15 m (h=11 m)

RAILWAY TUNNEL

ROAD TUNNEL Ultra-Low

backgroundFacility15 x 10 m (h=8 m)

Old Laboratoy

20 x 5 m(h=4.5 m)

installations, clean rooms

& offices

Access gallery

The new Canfranc Underground Laboratory

Characteristic of the new LSC

Depth 900 m (2450 mwe)

Main experimental hall

600 m2 (oriented to CERN)

Low background lab

150 m2

Clean room 45 m2 (100/1000 type)

General services

135 m2

Offices 80 m2


IUSIUS – Boulby Mine Laboratory, UK

http://hepwww.rl.ac.uk/ukdmc/ukdmc.html


Operating Institution

Institute for Underground Physics University of Sheffield

Location Potash mine, Boulby (UK)

Excavation 1988 (Stub 2) – 1995 (Stub 2a) – 1998 (H area) – 2003 (JIF area)

Depth 850 m (2250 mwe) to 1300 m (3600 mwe)

Surface 3000 m2

Permanent staff 2

Scientists users 30

[Stub2] 300 m2 + [Stub2a] 150 m2 + [H area] + 900 m2 + [JIF area] 2500 m2



Radon (Bq/m3) O(10)


Completed Experiments

Dark Matter NaIAD (~ 65 kg NaI Advanced Detector)ZEPLIN-I (~ 3.1 kg Liquid Xe scintil. Detector)

Running experiments and Under construction

Dark Matter ZEPLIN-II (~ 30 kg Liquid Xe scintil. Detector)DRIFT (Low pressure Xe gaseous TPC)ZEPLIN-III ( 6 kg Liq Xe + 3D reconstruction)


CUPPCUPP - Centre for Underground Physics in Pyhäsalmi, Finland

http://cupp.oulu.fi/


The project to host an underground laboratory in the mine was started in 1993, and the Centre for Underground Physics in Pyhäsalmi (CUPP) was physically established in 2001.

The old part of the mine:There will be plenty of free space to host and storage experiments

The new mine started to operate in July 2001. It extends to the depth of 1440 m (4000 mwe).

The largest cavern that can be easily constructed is 100 x 15 x 20 m3. An example of the layout


Neutron Flux (> 1 MeV) (10-6 n cm-2 s-1) ?

Radon (Bq/m3) O(100)


SULSUL – Solotvina Underground Laboratory, Ukraine

http://lpd.kinr.kiev.ua/


It was constructed in 1984 by the Institute for Nuclear Research (Ukrainian National Academy of Sciences).

It is situated on the west of Ukraine, in Solotvina near the border with Romania.

1 Main hall 30 x 20 m2 (h 8 m) + 4 small halls 3 x 6 m2 (h 3 m)

Primordial Radionuclides

Due to a low radioactive contamination of salt, the natural gamma background in the SUL is 10-100 times lower than in other underground laboratories


Neutron Flux (> 1 MeV) (10-6 n cm-2 s-1) 0(1)

Radon (Bq/m3) ?


The principal scientific goal of the Laboratory is search for rare or forbidden processes in nuclear and particle physics, mainly for double beta (2β) decay of atomic nuclei.

the CARVEL (CAlcium Research for VEry Low neutrino mass) proposal is developed for 2β0ν decay of 48Ca with 48CaWO4 crystal scintillators (~100 kg ) with sensitivity of

T1/2 ≥ 1027 yr andmν ≤ 0.04-0.09 eV

116CdWO4 detectors


France Commissariat a l’Energie Atomique, Centre National de la Recherche Scientifique

Italy Istituto Nazionale di Fisica Nucleare, Istituto di Fotonica e Nanotecnologie Trento, European Gravitational Observatory

Germany Max Planck Institut für Kernphysik, TechnischeUniversität München, Max Planck Institut für Physik Muenchen, Eberhardt,Karls Universität Tubingen

Spain Zaragoza University

UK Sheffield University,Glasgow University,London University

Czech Rep Czech Technical Univ. in Prague

Denmark University of Southern Denmark

Netherland Leiden University

Finland University of Jyväskylä

Slovakia Comenius University Bratislavia

Greece Aristot University of Thessaloniki

Integrated Large

Infrastructures for

Astroparticle Science

ILIAS is an initiative supported by the European Union with the aim to support the European large infrastructures operating in the astroparticle physics sector.


The ILIAS project is based on 3 groups of activitiesactivities:

• Networking Activities(N2) Deep Underground science laboratories(N3) Direct dark matter detection(N4) Search on double beta decay(N5) Gravitational wave research(N6) Theoretical astroparticle physics

• Joint Research Activities (R&D Projects)

(JRA1) Low background techniques for Deep Underground Science(JRA2) Double beta decay European observatory(JRA3) Study of thermal noise reduction in gravitational wave detectors

• Transnational Access Activities

(TA1) Access to the EU Deep Underground Laboratories


JRA1 JRA1 ((Joint Research Activities 1)): : Low background techniques for deep underground sciences ( (LBT-DUSLLBT-DUSL))

ObjectivesObjectives::

Background identification and measurement (Background identification and measurement ( intrinsicintrinsic, , inducedinduced, , environmentalenvironmental))

Background rejection techniques (Background rejection techniques (shieldingshielding, , vetoesvetoes, , discriminationdiscrimination))

A vast R&D programme on the improvement and implementation of ultra-low background techniques will be carried out cooperatively in the European Underground Laboratories.

Working packages

WP1: Measurements of the backgrounds in the underground labs

WP2: Implementation of background MC simulation codes

WP3: Ultra-low background techniques and facilities

WP4: Radiopurity of materials and purification techniques


RADIOCHEMICALIntegrated in energy and time

CHERENKOVLess than 0.01% of the solar neutrino flux is been measured in real time.

Italy (INFN & Universiy of Milano Genova, Perugia LNGS) USA (Princeton Univ., Virginia Tech.)Russia (RRC KI, JINR, INP MSU, INP St. Petersburg) Germany (Hiedelberg MPI, Munich Technical University)France (College de France)Hungary (Research Institute for Particle & Nuclear Physics)Poland (Institute of Physics, Jaegollian University, Cracow)

The main goal of Borexino is to measure in real time the low energy (< 1 MeV) component of solar neutrinos.

Radiocontaminants < 10-16 g/g (238U and 232Th equivalent) !

Background from natural radioactivity


Survival probability (LMA-Solution)

MeV

Vacuum oscillations

Beside solar ν Borexino could study: neutrinos coming from the Earth (Geoneutrinos),neutrinos coming from Supernova, magnetic moment of neutrino [with artificial source 51Cr]

7Be

Oscillation in matter(MSW)

Not still studied in direct way

Direct observation of vacuum oscillations

51Cr (E = 751 keV) Activity = 2.5 MCi


BOREXINO: subsystemsScintillator purification systems:Water extractionVacuum distillationSilicagel adsorption

DI Water plant

Storage tanks: 300tons of PC

Borexino detector

Control roomCounting room

CTF


Core of the detector: 300 tons of liquid scintillator (PC+PPO) contained in a nylon vessel of 8.5 m diameter. The thickness of nylon is 125 µm.

1st shield: 1000 tons of ultra-pure buffer liquid (pure PC) contained in a stainless steel sphere of 13.7 m diameter (SSS).

2200 photomultiplier tubes pointing towards the center to view the light emitted by the scintillator.

2nd shield: 2400 tons of ultra-pure water contained in a cylindrical dome.

200 photomultiplier tubes mounted on the SSS pointing outwards to detect Cerenkov light emitted in the water by muons.


eLieBe 77

Eν = 862 keV (monochromatic)

ΦSSM = 4.8 · 109 ν s-1 cm2

e

xRecoil nuclear energy of the e-

expected rate (LMA hypothesis) is 35 counts/day in the 250-800 keV energy range

)1(10 244 MeVatcm

ee xx

Elastic Scattering


18 m


Cleen Room (on top of the Water Tank) for the insertions of lasers

and sources for calibrations.


100 PMTs

4 tons of scintillator

4.5m thickness of water shield

Muon-veto detector

CTF is a prototype of Borexino. Its main goal was to verify the capability to reach the very low-levels of contamination needed for Borexino

Lino Miramonti – 8 Feb 2007 – Campinas - Sao Paulo (Brasil)1 European underground laboratories...

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