AMS Alpha Magnetic Spectrometer

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 gt 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
The AMS detector
4
AMS Scientific goals Precision study of the
properties of Cosmic Rays
i. Fluxes of individual elements Z1-26 (0.1
GeV/n - 1 TeV/n)
He
Fe

• AMS-02(Projection)

Relative Fluxes (normalized to AMS-02 projected
value)
He
Fe
H
AMS-02
AMS-02
AMS-02
5
AMS Scientific goals Precision study of the
properties of Cosmic Rays
ii. Propagation Parameters (diffusion
coefficient, galactic winds, ...)
Secondaries / Primaries, Isotopic ratios....
iii. Cosmic Ray confinement time
Radioactive clock (10Be)
6
AMS Scientific goals Dark Matter Search

• Many candidates from Particle Physics
• SUSY neutralinos (?0)
• Kaluza-Klein bosons (B)

7
AMS Scientific goals Antimatter Search
Our Universe can have some fraction of primordial
antimatter
AMS will detect 107 He nuclei with E gt 100 GeV
8
International Participation in AMS
FINLAND
RUSSIA
HELSINKI UNIV. UNIV. OF TURKU
I.K.I. ITEP KURCHATOV INST. MOSCOW STATE UNIV.
DENMARK
UNIV. OF AARHUS
NETHERLANDS
GERMANY
ESA-ESTEC NIKHEF NLR
RWTH-I RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE
KOREA
USA
EWHA KYUNGPOOK NAT.UNIV.
AM 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
FRANCE
ROMANIA
CHINA
BISEE (Beijing) IEE (Beijing) IHEP (Beijing) SJTU
(Shanghai) SEU (Nanjing) SYSU (Guangzhou) SDU
(Jinan)
ISS UNIV. OF BUCHAREST
GAM MONTPELLIER LAPP ANNECY LPSC GRENOBLE
SWITZERLAND
ETH-ZURICH UNIV. OF GENEVA
TAIWAN
SPAIN
CIEMAT - MADRID I.A.C. CANARIAS.
ITALY
ACAD. SINICA (Taiwan) CSIST (Taiwan) NCU (Chung
Li) NCKU (Tainan) NCTU (Hsinchu) NSPO (Hsinchu)
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
MEXICO
UNAM
PORTUGAL
LAB. OF INSTRUM. LISBON
16 Countries, 56 Institutes, 500 Physicists
Y96673-05_1Commitment
9
France in AMS
RICH Detector (LPSC Grenoble)
ECAL (LAPP Annecy)
Annecy
Grenoble
Laboratoire dAnnecy-le-Vieux de Physique des
Particules (LAPP)
Laboratoire de Physique Subatomique et de
Cosmologie (LPSC)
Montpellier
GPS (LPTA Montpelier)
Laboratoire de Physique Théorique et
dAstroparticules (LPTA)
10
Spain in AMS
Superconducting Magnet Electronics
(CIEMAT-CRISA/EADS-CEDEX)
Madrid
RICH Detector (CIEMAT-IAC)
Centro de Investigaciones energeticas
Medioambientales y tecnologicas (CIEMAT)
CRISA/EADS
CEDEX
Instituto Nacional de Tecnicas aeroespaciales
(INTA)
Tenerife (Canary Islands)
Instituto de Astrofisica de Canarias (IAC)
Qualification test (INTA)
11
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

• Dual solid radiator configuration
• 92 tiles (25 mm thick) of Low refractive index
  aerogel (n1.05)
• 16 tiles (5 mm thick) of NaF (n1.33)
• Conical reflector
• Reflectivity gt 85
• Photo-detection plane

• 680 PMTs (HAMAMATSU 7600-00-M16)
• 4 X 4 pixels (4x4 mm2 each)
• Gain 106 _at_ 800 V
• QE ? 20 in the range 250-600 nm

Weight 200 Kg Power lt 100 W Acceptance
0.4 m2sr
12
IN2P3-CICYT Cooperation agreement
13
IN2P3-CICYT Cooperation agreement
14
IN2P3-CICYT Cooperation agreement

• Coordinators
• IP-Spain Dr. C. Mañá
• IP-France Dr. M. Buenerd

• Funding
• YEAR FUNDING
• 2004 7,200.00
• 2005 6,800.00
• 2006 7,350.00
• 2007 4,050.00

15
AMS integration and test at CERN
04/03/2008
16
AMS-RICH Integration at CERN
17
The Auger Observatory
18
Cosmic Ray Spectrum
AMS
Auger
LHC
Tevatron
HERA
Same cm energy
19
Fluorescence Telescopes
Arrays of particle detectors
20
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 ?

21
Neutrino bounds
Results
Photon bounds
Anisotropies
Spectrum
22
The Auger Observatory
23
The Auger Collaboration

• Argentina Mexico
• Australia Netherlands
• Bolivia Poland
• Brazil Portugal
• Czech Republic Slovenia
• France Spain
• Germany United Kingdom
• Italy USA
• Vietnam
• 17 Countries gt 100 Institutions gt 450
  Scientists

24

• France in Auger
• 32 members in 6 institutions 16
• Construction budget 3.5 M
• PMTs Photonis
• CCIN2P3 Computing Center

AstroParticle and Comology Institute Université
Paris 7, (APC) CNRS Laboratoire Physique Nucleair
et des Hautes Energies Universités Paris 6 et 7
(LPNHE)
Paris
Orsay
Institute Physique Nucleair (IPN-Orsay)
Université Paris 11 CNRS Laboratoire de
lAccélérateur Linéaire (LAL-Orsay) CNRS
Nantes
Laboratoire Physique Subatomique et des
technologies associées (SUBATEC-Nantes)
Lyon
Centre de Calcul de l'In2p3, (CCIN2P3), CNRS-IN2P3
Grenoble
Laboratoire Physique Subatomique et de Cosmologie
(LPSC) Université Joseph Fourier, INPG, 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 RD

26

• Spain in Auger
• 19 members in 5 institutions 7
• Construction budget 1 M
• Solar Panels ISOFOTON

Santiago
Instituto Gallego de Físca de Altas Energías
(IGFAE), Universidad de Santiago
Unviersidad Alcalá de Henares (UAH) Unviersidad
Complutense de Madrid (UCM)
Alcalá
Instituto Física Corpuscular CSIC-Universidad de
Valencia (IFIC) (Associated to IGFAE)
Madrid
Valencia
Granada
Universidad de Granada (UGr)
27
Brief summary of Spains involvement

• 1994-95 IGFAE Prospects for North Auger
• 1996-98 IGFAE evaluates Auger acceptance to n
• 1999-00 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, g Shower gs
es 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