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