ams (alpha magnetic spectrometer) & auger observatory enrique zas instituo gallego de física de...
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AMS (Alpha Magnetic Spectrometer) &
Auger Observatory
Enrique Zas
Instituo Gallego de Física de Altas Energías
Santiago de Compostela
January 12, 2009
AMS ExperimentThe purpose of the AMS Experiment is to install a Particle
Physics Detector on the ISS to perform high precision measurements of the primary cosmic radiation
AMS on the ISS• Orbit Altitude 350 km• Power 2 kW• Weight ~ 7 T• Exposure > 3 years
The AMS detector will have capabilities to identify the cosmic ray nuclei with Z 26 and to measure their energy spectrum up to the TeV region.
ParticleEnergy Range
p+ 1 TeV
He,….,Fe 1 TeV/n
Light Isotopes 10 GeV/n
P- 350 GeV
e+ 350 GeV
Anti - He,C,... 1 TeV/n
e- 1 TeV
1 TeV
The AMS detector
SubdetectorsRange/
Precision
Magnet BL2 0.78 Tm2
TrackerPlanes 8
(p) / p 1.5 %
TRD & EMC e/p - < 10-6
RICH () / 0.1 %
AMS Scientific goals: Precision study of the properties of Cosmic Rays
Relative Fluxes (normalized to AMS-02 projected value)
AMS-02AMS-02 AMS-02
H He Fe
(Projection)
H
(Projection)
He Fe
• AMS-02(Projection)
i. Fluxes of individual elements Z=1-26 (0.1 GeV/n - 1 TeV/n)
(Projection)
iii. Cosmic Ray confinement time
(Projection)
D/p
(Projection)
Secondaries / Primaries, Isotopic ratios....
Radioactive clock (10Be)
AMS Scientific goals: Precision study of the properties of Cosmic Rays
ii. Propagation Parameters (diffusion coefficient, galactic winds, ...)
Many candidates from Particle Physics: • SUSY neutralinos (0) • Kaluza-Klein bosons (B)• …
00 qq, WW, ZZ, ,ll
structures in the spectra of
e+, p, D, γ
AMS Scientific goals: Dark Matter Search
AMS will detect 107 He nuclei with E > 100 GeV
Our Universe can have some fraction of primordial antimatter:
AMS Scientific goals: Antimatter Search
International Participation in AMSInternational Participation in AMS
USAA&M FLORIDA UNIV.JOHNS HOPKINS UNIV.MIT - CAMBRIDGENASA GODDARD SPACE FLIGHT CENTERNASA JOHNSON SPACE CENTERUNIV. OF MARYLAND-DEPRT OF PHYSICSUNIV. OF MARYLAND-E.W.S. S.CENTERYALE UNIV. - NEW HAVEN
MEXICO
UNAM
DENMARKUNIV. OF AARHUS
FINLAND
HELSINKI UNIV.UNIV. OF TURKU
FRANCE
GAM MONTPELLIERLAPP ANNECYLPSC GRENOBLE
GERMANYRWTH-IRWTH-IIIMAX-PLANK INST.UNIV. OF KARLSRUHE
ITALYASICARSO TRIESTEIROE FLORENCEINFN & UNIV. OF BOLOGNAINFN & UNIV. OF MILANOINFN & UNIV. OF PERUGIAINFN & UNIV. OF PISAINFN & UNIV. OF ROMAINFN & UNIV. OF SIENA
NETHERLANDSESA-ESTECNIKHEFNLR
ROMANIAISSUNIV. OF BUCHAREST
RUSSIAI.K.I.ITEPKURCHATOV INST.MOSCOW STATE UNIV.
SPAIN
CIEMAT - MADRIDI.A.C. CANARIAS.
SWITZERLANDETH-ZURICHUNIV. OF GENEVA
CHINA BISEE (Beijing)IEE (Beijing)IHEP (Beijing)SJTU (Shanghai)SEU (Nanjing)SYSU (Guangzhou)SDU (Jinan)
KOREA
EWHAKYUNGPOOK NAT.UNIV.
Y96673-05_1Commitment
PORTUGAL
LAB. OF INSTRUM. LISBON
ACAD. SINICA (Taiwan)CSIST (Taiwan)NCU (Chung Li)NCKU (Tainan)
NCTU (Hsinchu)NSPO (Hsinchu)
TAIWAN
16 Countries, 56 Institutes, 500 Physicists16 Countries, 56 Institutes, 500 Physicists
France in AMS
Montpellier
Grenoble AnnecyLaboratoire d’Annecy-le-Vieux de Physique des Particules (LAPP)
Laboratoire de Physique Théorique et d’Astroparticules (LPTA)
Laboratoire de PhysiqueSubatomique et de Cosmologie
(LPSC)
RICH Detector(LPSC Grenoble)
ECAL(LAPP Annecy)
GPS(LPTA Montpelier)
Madrid
Instituto de Astrofisica de Canarias (IAC)
Tenerife (Canary Islands)
Spain in AMS
Centro de Investigaciones energeticas Medioambientales y tecnologicas (CIEMAT) CRISA/EADS
Instituto Nacional de Tecnicas aeroespaciales (INTA)
CEDEX
RICH Detector(CIEMAT-IAC)
Superconducting Magnet Electronics (CIEMAT-CRISA/EADS-CEDEX)
Qualification test(INTA)
► Dual solid radiator configuration
• 92 tiles (25 mm thick) of Low refractive index aerogel (n=1.05)
• 16 tiles (5 mm thick) of NaF (n=1.33)
► Conical reflector
Reflectivity > 85%
► Photo-detection plane
Weight ~ 200 KgPower < 100 WAcceptance = 0.4 m2sr
47 cm
64x64 cm2
114 cm
134 cm
IN2P3-CICYT Cooperation agreement• Institutes: LPSC (Grenoble)
CIEMAT (Madrid)
• Purpose: Additional travel funds to perform common activities in the construction of the AMS-RICH Detector
680 PMT´s (HAMAMATSU 7600-00-M16)• 4 X 4 pixels (4x4 mm2 each)• Gain ~ 106 @ 800 V• QE 20 % in the range 250-600 nm
Activities Location
Assembly of the Unit cells (PMT´s, Front-End Electronics, HV divider)
LPSC (Grenoble)
Characterization of the Unit cells (Gain calibration and Thermal response)
LPSC (Grenoble)
Assembly of Light guides on the Unit cells
CIEMAT (Madrid)
-35°
55°
IN2P3-CICYT Cooperation agreement
Activities Location
Characterization of the radiator material (Aerogel refractive index)
LPSC (Grenoble)
Characterization of the radiator material (Aerogel transmittances and ageing studies)
CIEMAT (Madrid)
Assembly of the Radiator Plane CIEMAT (Madrid)
RICH Collaboration MeetingsLPSC (Grenoble)CIEMAT (Madrid)
XY
Optical bench
IN2P3-CICYT Cooperation agreement
• Funding
YEAR FUNDING
2004 7,200.00 €
2005 6,800.00 €
2006 7,350.00 €
2007 4,050.00 €
• Coordinators
IP-Spain: Dr. C. MañáIP-France: Dr. M. Buenerd
IN2P3-CICYT Cooperation agreement
AMS integration and test at CERN
04/03/2008
AMS-RICH Integration at CERN
The Auger Observatory
Cosmic Ray Spectrum
LHCTevatron
HERA
Same cm energy
AugerAMS
Arrays of particle detectors
Fluorescence Telescopes
Crucial feature: Hybrid •Improve reconstruction •Calibrate techniques•Study performance•Check algorithms•Shower max Composition•...
Auger Science Objectives• Enhance statistical sample 2 x 3000 km2 array • Uniform Exposure North & South Observatories• Intercalibration, accuracy Hybrid: Array &
Fluorescence• Composition, accuracy FADC 40MHz &
GPS 10ns timing
• Flourescence
– Calorimetric E (Xmax)
– Acceptance(E)
– Corrections(t)
• Absorption
• Cherenkov
– 10% duty cycle
– Fluor yield(T,p)
– Future (satellite)
• EAS arrays
– 1 layer calorimeter
– Geometric Acceptance
– Corrections
• Fluctuations
• Sampling
– Depth(T,p)
– 100% duty cycle
– Limited size ?
Results
Photon bounds
Neutrino bounds
Anisotropies
Spectrum
The Auger Observatory
Detector Tank # 1600Friday 13 June 2008
The Auger Collaboration
Argentina Mexico
Australia Netherlands
Bolivia* Poland
Brazil Portugal
Czech Republic Slovenia
France Spain
Germany United Kingdom
Italy USA
Vietnam*
17 Countries > 100 Institutions > 450 Scientists
France in Auger•32 members in 6 institutions 16%
• Construction budget 3.5 M$• PMT’s Photonis• CCIN2P3 Computing Center
Grenoble Laboratoire Physique Subatomique et de Cosmologie (LPSC)Université Joseph Fourier, INPG, CNRS-IN2P3
Paris
Lyon
Institute Physique Nucleair (IPN-Orsay) Université Paris 11 CNRSLaboratoire de l’Accélérateur Linéaire (LAL-Orsay) CNRS
AstroParticle and Comology Institute Université Paris 7, (APC) CNRSLaboratoire Physique Nucleair et des Hautes Energies Universités Paris 6 et 7 (LPNHE)
Orsay
NantesLaboratoire Physique Subatomique et des technologies associées (SUBATEC-Nantes)
Centre de Calcul de l'In2p3, (CCIN2P3), CNRS-IN2P3
• South: – PMT bases– Station electronics (Unified Board)– CDAS
• North– DAQ board– PMT base and FE electronics– PMT and electronics enclosure
Responsabilities• CDAS (task-leader)• SDE (task-leader)• Monitoring (task-leader)• Data management• Task leader of several analysis groups• Co-coordination of analysis tasks• Co-coordination of detector tasks• Future:
– North task force– Radio R&D
Madrid
Spain in Auger •19 members in 5 institutions 7%
• Construction budget 1 M$• Solar Panels ISOFOTON
Unviersidad Alcalá de Henares (UAH)Unviersidad Complutense de Madrid (UCM) Instituto Física Corpuscular CSIC-Universidad de Valencia (IFIC)
(Associated to IGFAE)
Instituto Gallego de Físca de Altas Energías (IGFAE), Universidad de Santiago
Universidad de Granada (UGr)
Valencia
Granada
Alcalá
Santiago
Brief summary of Spain’s involvement
• 1994-95 : IGFAE Prospects for North Auger • 1996-98 : IGFAE evaluates Auger acceptance to • 1999-00 : IGFAE develops analysis for inclined (HP) • 2002 : Spain joins through USC • 2005: UAH and UCM enter • 2007: UGR and IFIC join
Inclined showers Protons, nuclei, :Shower ’s e+’s and e-’s
do not reach ground level Only muons
• South: – Solar panels– Contributions
• Auger Access• XLF/CLF• AMIGA/BATATA
Responsabilities
• Task leader of several analysis groups• Simulation Production Manager• Monitoring of Power systems• Future:
– Atmospheric Monitoring North
– Amiga
– Grid node
– Power systems North