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CHARGED PARTICLE OBSERVATION from ‘SPACE’. European Astroparticle Physics Meeting Munich, November 23-25, 2005 M. Bourquin, University of Geneva. Advantage of space and balloon experiments. Detectors are above the atmosphere : Direct measurements of CR composition - PowerPoint PPT Presentation
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CHARGED PARTICLE OBSERVATIONfrom ‘SPACE’
European Astroparticle Physics Meeting
Munich, November 23-25, 2005
M. Bourquin, University of Geneva
M. Bourquin November 2005 2
Advantage of space and balloon experiments
• Detectors are above the atmosphere :– Direct measurements of CR composition– Very precise measurements, using state-of the-art particle physics
technology
satellites and ISS ( cover the full sky when in Earth orbit)
balloons (about 5 gr/cm2 remaining)
M. Bourquin November 2005 3
Overview of experiments
Experiments Presenting Analyzed Flight Data, Active Detectors
•TRACER, ATIC, BESS, TIGER, BETS, CPDS, MARIE
Experiments Presenting Analyzed Flight Data, Passive Detectors
•RUNJOB, CAKE
Experiments With Recent Data, Analysis Underway
•BESS-Polar, CREAM
Experiments With Advanced Hardware
•PAMELA, AMS-02
New Experiments
•CALET, CREST, NUCLEON, INCA
R. Streitmatter, 29th ICRC, 2005
M. Bourquin November 2005 4
Difficulties
•for Satellites and ISS: Schedule uncertainties linked to launch uncertainties
Complex issues of space qualification and safety procedures:
Limited weight, limited power, accelerations and vibrations, pressure change, limited data transfer, temperature changes, operation without human intervention
•for Long Duration Balloon Flights:weather conditions (e.g. at South Pole !)
M. Bourquin November 2005 5
Balloon-borne Experiment Superconducting Spectrometer - POLAR
8-day, 17 hour Antarctic flight, Dec. 2004
BEFORE AFTER
M. Bourquin November 2005 6
Topics addressed by CR space experiments
• Indirect dark matter search (antiprotons, positrons, antideuterons)
• Understanding propagation processes (nuclei e.g. B, C, Fe)
• Search for primary antimatter (antinuclei)• Search for new forms of matter (e.g. strangelets)
M. Bourquin November 2005 7
Cosmic Ray Fluxes
M. Bourquin November 2005 8
AMS-01 on STS-91 Shuttle Flight
M. Bourquin November 2005 9
AMS-01 Proton Spectra
Above cutoff: cosmic rays
Sub-cutoff: trapped particles
Downward
Upward
M. Bourquin November 2005 10
Helium in near Earth Orbit with AMS-01
M. Bourquin November 2005 11
Properties of next generation magnetic spectrometers
R. Battiston, Rapporteur Talk on Direct Measurements and Origin of CR, ICRC,2003
M. Bourquin November 2005 12
ANTI ANTI
Anticoncidence system
Multiple particles rejection
TRKTRKSi Tracker + magnet
Permanent magnet B=0.4T
6 planes double sided Si strips 300 m thick
Spatial risolution ~3m
MDR = 1000 GV/c
TOFTOF Time-of-flight
Level 1 trigger
particle identification (up to 1GeV/c)
dE/dx
Plastic scintillator + PMT
Time Resolution ~ 70 ps
ANTIANTIAnticoincidence system
Defines tracker acceptance
Plastic scintillator + PMT
S4 S4 NDND
S4 and Neutron detectors
Identify hadron interactions
Plastic Scintillator
36 3He counters in a polyetilen moderator
PAMELA DETECTOR
CALOCALO
Si-W Calorimeter
Imaging Calorimeter : reconstructs shower profile discriminating e+/p and p/e- at level of
~ 10-5
Energy Resolution for e± E/E = 15% / E1/2.
Si-X / W / Si-Y structure
22 W planes
16.3 X0 / 0.6 l0
M. Bourquin November 2005 13
Pamela in Samara, Russia 4/09/05
M. Bourquin November 2005 15
The Satellite: Resurs DK1- Soyuz-TM Launcher from Baikonur
- Launch in 2005
- Lifetime >3 years
- PAMELA mounted inside a Pressurized Container, attached to Satellite
- Earth-Observation- Satellite
M. Bourquin November 2005 16R. Battiston, Rapporteur Talk on Direct Measurements and Origin of CR, ICRC,2003
M. Bourquin November 2005 17
BESS-Polar: Lower Energy, High Statistics
Measurements to lower energy.Reduced geomagnetic influenceLess material in particle pathLong Duration Flight • Technical flight Fall 2003• Antarctic flight Winter 2004-2005 • Antarctic Flight Winter 2007-2008• More than double present p-bar statistics in first flight • ~22 times present solar-minimum p-bar statistics in 2007-2008 flight
M. Bourquin November 2005 18
Courtesy M. Buénerd
M. Bourquin November 2005 19
CalorimeterPreliminary Energy Deposit
Distribution
~100 TeV incident energy
Energy deposit gives a quick check of the energy spectrum It shows a reasonable power law with data extending well above 100 TeV
M. Bourquin November 2005 20
AMS-02 on the International Space Station
M. Bourquin November 2005 21
AMS-02 Detector
TRD: e/p separation
TOF: ß and |Z|, sign(Z)
Star tracker: pointing
Magnet: 0.8 T, sign(Z)
Si tracker: p, |Z|, sign(Z)
ACC: anticoincidence system
RICH: ß and |Z|, sign(Z)
ECAL: e/p separation
M. Bourquin November 2005 22
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Antiproton Production in the Galaxy
• Primary antiprotons could originate from the annihilation of the dark matter particles (Susy neutralinos) concealed inside the galactic halo.
• Secondary antiprotons are produced through the spallation of CR protons on the interstellar materiel. Spectrum peaks at about 2 GeV
• Presently antiprotons have very large propagation uncertainties, which has to be understood to search for effects due to primary antimatter.
M. Bourquin November 2005 27
Antiproton fluxesA M Lionetto, A Morselli and V Zdravkovic (2005)
M. Bourquin November 2005 28
Antiproton spectra: Pamela expectation for Diffuse and Convection model in 3 yr
Antiproton spectra: PAMELA expectation for DC model
A.Lionetto, A.Morselli, V.Zdravkovic, JCAP09(2005)010
M. Bourquin November 2005 29
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Dark matter search with antiprotonsSecondary antiproton flux Distorsion by WIMP
(examples with 964 GeV and 777 GeV neutralino, P. Ullio, astro-ph 9904086)
M. Bourquin November 2005 31
Positron spectra: PAMELA expectation for DC model
DRB
DC
A.Lionetto, A.Morselli, V.Zdravkovic
JCAP09(2005)010 [astro-ph/0502406]
M. Bourquin November 2005 32
Dark matter search with positrons: AMS-02Neutralinos induce a distortion of the spectrum
Sensitivity after one year of data P. Maestro, based on models by Baltz and Edsjö
GeVm 3.130GeVm 336
M. Bourquin November 2005 33
Description of CR propagationDiffusion models have several free parameters to be fixed by observations
M. Bourquin November 2005 34
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10Be/9Be – radioactive clock
10Be (t1/2 = 1.51 Myr) is the lightest radioactive secondary isotope having a half-life comparable with the CR confinement time in the Galaxy.
In diffusion models, the ratio 10Be/9Be is sensitive to the size of the halo and to the properties of the local interstellar medium
1 year
AMS will separate 10Be from 9Be for0.15 GeV/n < E < 10 GeV/n after 3 years will collect 105 10Be
M. Bourquin November 2005 36
Antimatter search - antihelium
Pamela (2004-2007)
Bess Polar (20 days)
M. Bourquin November 2005 37
Search for New Particles
AMS-01 reported an anomalous event (Z/A = 0.114), background probability < 10-3
Compatible with a strangelet from a ‘color locked’ model.
Ф ~ 10-5 (m2 sr sec)-1
Properties:
AMS-02: statistics x
103
M. Bourquin November 2005 38
18-9-2004 Jes Madsen 29
Why are strangelets interestingas ultra-high energy cosmic rays?
Madsen & Larsen, PRL 90 (2003) 121102
2. Less susceptible to GZK-cut-off from high-Lorentz-factor interactions with 2.7K CMB-photons because of
High A
Low Z/A
18-9-2004 Jes Madsen 26
Why are strangelets interestingas ultra-high energy cosmic rays?
Madsen & Larsen, PRL 90 (2003) 121102
1. ZSTRANGELET >> ZNUCLEUS possible
Better acceleration in known sources
(EMAX = RMAX Z; RMAX magn.field x size)
Rigidity R = p/Z (= E/Z if relativistic)
M. Bourquin November 2005 39
Conclusions
1. The new space experiments are quite impressive detectors:
Pamela, AMS-02, BESS, CREAM
• They will collect very precise data on charged CR.• They are unavoidable for a full understanding of
propagation processes to unravel new physics.
M. Bourquin November 2005 40
2. Propagation uncertainties still require multi-messenger observations
Ex: Dark matter searches : importance of simultaneous measurements of
Be prepared to compare results between CR experiments and gamma rays experiments
and with LHC experiments!
Dep ,,,
M. Bourquin November 2005 41
Several Astroparticle experiments are ‘Recognized’ at CERN:
RE1(AMS) Alpha Magnetic Spectrometer (AMS) for Extraterrestrial Study of Antimatter, Matter and Missing Matter on the International Space Station
RE3(AUGER PROJECT) The Pierre Auger Observatory Project
RE4(L3+C) L3 + Cosmics Experiment
RE5(EXPLORER) The Gravitational Wave Detector EXPLORER
RE6(ANTARES) ANTARES: An Undersea Neutrino telescope
RE7(GLAST) GLAST
RE8(LISA) LISA
RE9(NESTOR) NESTOR-Neutrino Extended Submarine Telescope with Oceanographic Research
RE2A(CAPRICE) Cosmic AntiParticle Ring Imaging Cerenkov Experiment
RE2B(PAMELA) Search for Antimatter in Space
3. How make European teams more competitive and to reduce expenditures by pooling resources?
M. Bourquin November 2005 42
Create an European Astroparticle Centre at CERN ?
It is planned to establish at CERN an
AMS Payload Operations and Control Centre (POCC)
and
a Science Operations Centre (SOC)
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