charged particle observation from ‘space’ european astroparticle physics meeting munich,...

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)


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


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 !)


Balloon-borne Experiment Superconducting Spectrometer - POLAR

8-day, 17 hour Antarctic flight, Dec. 2004

BEFORE AFTER


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)


Cosmic Ray Fluxes


AMS-01 on STS-91 Shuttle Flight


AMS-01 Proton Spectra

Above cutoff: cosmic rays

Sub-cutoff: trapped particles

Downward

Upward


Helium in near Earth Orbit with AMS-01


Properties of next generation magnetic spectrometers

R. Battiston, Rapporteur Talk on Direct Measurements and Origin of CR, ICRC,2003


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

Pamela in Samara, Russia 4/09/05


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


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


Courtesy M. Buénerd


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


AMS-02 on the International Space Station


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


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.


Antiproton fluxesA M Lionetto, A Morselli and V Zdravkovic (2005)


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


Dark matter search with antiprotonsSecondary antiproton flux Distorsion by WIMP

(examples with 964 GeV and 777 GeV neutralino, P. Ullio, astro-ph 9904086)


Positron spectra: PAMELA expectation for DC model

DRB

DC

A.Lionetto, A.Morselli, V.Zdravkovic

JCAP09(2005)010 [astro-ph/0502406]


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


Description of CR propagationDiffusion models have several free parameters to be fixed by observations


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


Antimatter search - antihelium

Pamela (2004-2007)

Bess Polar (20 days)


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


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)


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.


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 ,,,


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?

http://greybook.cern.ch/programmes/experiments/RE1.html








http://greybook.cern.ch/programmes/experiments/RE2A.html

http://greybook.cern.ch/programmes/experiments/RE2B.html


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)

charged particle observation from ‘space’ european astroparticle physics meeting munich,...

Documents

upward slide

remaining slide

strangelets slide

shuttle flight slide

university of geneva

balloon experiments

cream experiments

cake experiments