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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.

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Presentation on theme: "AMS (Alpha Magnetic Spectrometer) & Auger Observatory Enrique Zas Instituo Gallego de Física de Altas Energías Santiago de Compostela January 12, 2009."— Presentation transcript:

1 AMS (Alpha Magnetic Spectrometer) & Auger Observatory Enrique Zas Instituo Gallego de Física de Altas Energías Santiago de Compostela January 12, 2009

2 AMS Experiment The 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.

3 Particle Energy Range p+p+ 1 TeV He,….,Fe1 TeV/n Light Isotopes10 GeV/n P-P- 350 GeV e+e+ Anti - He,C,...1 TeV/n e-e- 1 TeV  The AMS detector Subdetectors Range/ Precision MagnetBL Tm 2 Tracker Planes8  (p) / p 1.5 % TRD & EMC e/p -  < RICH  (  ) /  0.1 %

4 AMS Scientific goals: Precision study of the properties of Cosmic Rays Relative Fluxes (normalized to AMS-02 projected value) AMS-02 H HeFe ( Projection ) H He Fe AMS-02 (Projection) i. Fluxes of individual elements Z=1-26 (0.1 GeV/n - 1 TeV/n)

5 (Projection) iii. Cosmic Ray confinement time (Projection) D/p (Projection) Secondaries / Primaries, Isotopic ratios.... Radioactive clock ( 10 Be) AMS Scientific goals: Precision study of the properties of Cosmic Rays ii. Propagation Parameters (diffusion coefficient, galactic winds,...)

6 Many candidates from Particle Physics: SUSY neutralinos ( 0 ) Kaluza-Klein bosons (B) …  0  0  qq, WW, ZZ, ,ll  structures in the spectra of e +, p, D, γ AMS Scientific goals: Dark Matter Search

7 AMS will detect 10 7 He nuclei with E > 100 GeV Our Universe can have some fraction of primordial antimatter: AMS Scientific goals: Antimatter Search

8 International Participation in AMS USA A&M FLORIDA UNIV. JOHNS HOPKINS UNIV. MIT - CAMBRIDGE NASA GODDARD SPACE FLIGHT CENTER NASA JOHNSON SPACE CENTER UNIV. OF MARYLAND-DEPRT OF PHYSICS UNIV. OF MARYLAND-E.W.S. S.CENTER YALE UNIV. - NEW HAVEN MEXICO UNAM DENMARK UNIV. OF AARHUS FINLAND HELSINKI UNIV. UNIV. OF TURKU FRANCE GAM MONTPELLIER LAPP ANNECY LPSC GRENOBLE GERMANY RWTH-I RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE ITALY ASI CARSO TRIESTE IROE FLORENCE INFN & UNIV. OF BOLOGNA INFN & UNIV. OF MILANO INFN & UNIV. OF PERUGIA INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF SIENA NETHERLANDS ESA-ESTEC NIKHEF NLR ROMANIA ISS UNIV. OF BUCHAREST RUSSIA I.K.I. ITEP KURCHATOV INST. MOSCOW STATE UNIV. SPAIN CIEMAT - MADRID I.A.C. CANARIAS. SWITZERLAND ETH-ZURICH UNIV. OF GENEVA CHINA BISEE (Beijing) IEE (Beijing) IHEP (Beijing) SJTU (Shanghai) SEU (Nanjing) SYSU (Guangzhou) SDU (Jinan) KOREA EWHA KYUNGPOOK NAT.UNIV. Y _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 Physicists

9 France in AMS Montpellier Grenoble Annecy Laboratoire d’Annecy-le- Vieux de Physique des Particules (LAPP) Laboratoire de Physique Th é orique et d ’ Astroparticules (LPTA) Laboratoire de Physique Subatomique et de Cosmologie (LPSC) RICH Detector (LPSC Grenoble) ECAL (LAPP Annecy) GPS (LPTA Montpelier)

10 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)

11 ► 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 Kg Power < 100 W Acceptance = 0.4 m 2 sr 47 cm 64x64 cm 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 M16) 4 X 4 pixels (4x4 mm 2 each) Gain ~ V QE  20 % in the range nm

12 ActivitiesLocation 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

13 ActivitiesLocation 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 PlaneCIEMAT (Madrid) RICH Collaboration Meetings LPSC (Grenoble) CIEMAT (Madrid) X Y  Optical bench IN2P3-CICYT Cooperation agreement

14 Funding YEARFUNDING 20047, € 20056, € 20067, € 20074, € Coordinators IP-Spain: Dr. C. Mañá IP-France: Dr. M. Buenerd IN2P3-CICYT Cooperation agreement

15 AMS integration and test at CERN 04/03/2008

16 AMS-RICH Integration at CERN

17 The Auger Observatory

18 Cosmic Ray Spectrum LHC Tevatron HERA Same cm energy Auger AMS

19 Arrays of particle detectors Fluorescence Telescopes Crucial feature: Hybrid Improve  reconstruction Calibrate techniques Study performance Check algorithms Shower max Composition...

20 Auger Science Objectives Enhance statistical sample 2 x 3000 km 2 array Uniform Exposure North & South Observatories Intercalibration, accuracy Hybrid: Array & Fluorescence Composition, accuracy FADC 40MHz & GPS 10ns timing Flourescence –Calorimetric E (X max ) –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 ?

21 Results Photon bounds Neutrino bounds Anisotropies Spectrum

22 The Auger Observatory Detector Tank # 1600 Friday 13 June 2008

23 The Auger Collaboration ArgentinaMexico Australia Netherlands Bolivia*Poland Brazil Portugal Czech RepublicSlovenia France Spain Germany United Kingdom Italy USA Vietnam* 17 Countries > 100 Institutions > 450 Scientists

24 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 CNRS Laboratoire de l’Accélérateur Linéaire (LAL-Orsay) CNRS AstroParticle and Comology Institute Université Paris 7, (APC) CNRS Laboratoire Physique Nucleair et des Hautes Energies Universités Paris 6 et 7 (LPNHE) Orsay Nantes Laboratoire Physique Subatomique et des technologies associées (SUBATEC-Nantes) Centre de Calcul de l'In2p3, (CCIN2P3), CNRS-IN2P3

25 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

26 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

27 Brief summary of Spain’s involvement : IGFAE Prospects for North Auger : IGFAE evaluates Auger acceptance to : IGFAE develops analysis for inclined (HP) 2002 : Spain joins through USC 2005: UAH and UCM enter 2007: UGR and IFIC join

28 Inclined showers Protons, nuclei,  : Shower  ’s e + ’s and e - ’s do not reach ground level Only muons

29 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


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