Matter/antimatter asymmetry in the Universe?The CR antimatter component and

its direct detection

Baikal summer school, July 2005

P.Spillantini, University and INFN, Florence, Italy

GeV|

TeV|

PeV|

EeV|

ZeV|

High Z[ENTICE, ECCO]

Light elements and Isotopes

[ACE]

Antiparticlesand Antinuclei

[BESS, PAMELA, AMS]

Elemental Composition[CREAM, BEAR,

ACCESS?,NUCLEON?, INCA?, PROTON-5?]

Direct detectionBalloons &

Satelites

Indirect detection (EAS)

[arrays & florescence]

Extreme Energy CR

AUGER, TUS, EUSO,KLYPVE?,OWL??

Nucleus

Star

galaxy

Cluster of galaxies

Super-cluster

??

Anti-Nucleus

Anti-Star

Anti-galaxy

Anti-Cluster of galaxies

Anti-Super-cluster

Anti - ??

Antiparticles and CR

difficulties needed

for antip: secondary production

high energy ( 100 GeV/n)

high energy ( 1 TeV)

long diffusion timelong pathgalactic wind

for antiN:

CP violation Sakharov conditions

All Matter Universe

Matter and antimatterin separated domains

Symmetric Cosmologies

Asymmetric Cosmologies

Both possible inBig Bang theories

It is possible rely only on observationsantip spectrum

antiN search

From e.m. observations Only local asymmetry(~10-8 of the Universe volume)

(no assumption onantiHe spectrum)

AMS STS-91 (1998 )(antiHe spectrum same shape of He spectrum)

ANTIMATTER LIMITS

Antiproton Positron

International Space Station “FREEDOM”

Hubble Space

Telescope

CGRO AXAF(CXO)

HST SIRTF

+ Particle-Antiparticle Superconducting Magnet Facility (ASTROMAG)

+Very Long

Base Interferometer

(VLBI)

+

Advanced Composition

Explorer (ACE)

Experiments approved for the first phase of the ASTROMAG facility

WIZARD: antiparticle spectra, antinuclei, etc..(USA, Italy, Sweden, Germany)

LISA: elemental and isotopic spectra, etc. (USA, other??)

MAGIC-SCINATT: elemental composition at knee (USA, Japan)

Balloon Flights

-- BESS (93, 95, 97, 98, BESS (93, 95, 97, 98,

2000)2000)

-- Heat (94, 95, 2000) Heat (94, 95, 2000)

-- IMAX (96) IMAX (96)

-- [BESS Long duration flights [BESS Long duration flights

(2004)](2004)]

(Wizard Coll.)

- - MASS – 1,2 (89,91)MASS – 1,2 (89,91)

--TrampSI (93)TrampSI (93)

-- CAPRICE (94, 97, 98) CAPRICE (94, 97, 98)

-- [ [ in flight (2004?)] in flight (2004?)]

New Generation ofAntimatter Researches

in Cosmic Rays

a) Longer duration ballooning b) Experiments in space

payload

services

HeAir Air

Class A Balloons2.8 Mm3 @ 5 g/cm2

lifting power ~ 11t

Balloon 5 tservices 3 tpayload 3 t

Open Balloons

Km

0 C°-100

40

Atmospheric temperature versus Altitude

0

BESS - Polar

New Generation ofAntimatter Researches

in Cosmic Rays

b) Experiments in space

PAMELA

Positrons 50 MeV - 270 GeV

Antiprotons 80 MeV – 190 GeV

Limit on antinuclei ~7 10-8 (He /He)

Electrons 50 MeV – 2TeV

Protons 80 MeV – 700 GeV

Nuclei < 300 GeV/n (Z 8)

study of the solar modulation after the 23rd solar cycle maximum.

GF 20.5 cm2 srMass 480 KgDimensions cm3 120 x 40x45 Power Budget 345W

Spillover of p on antip = 0.2 of the antip flux

Distortion of the secondary positron fraction induced by a signal from a heavy neutralino.

Distortion of the secondary antiproton flux induced by a signal from a heavy Higgsino-like neutralino.

P.Picozza and A.Morselli,astro-ph/0103117

standard

Expected data from Pamela for two years of operation are shown in red.

BESS (2004+2006 LDB flights)

ANTIMATTER LIMITS

AMS STS-91 (1998 )(antiHe spectrum same shape of He spectrum)

(2005-8 )

Razzo Soyuz

(no assumption onantiHe spectrum)

AMS STS-91 (1998 )(antiHe spectrum same shape of He spectrum)

BESS (2004+2006 LDB flights)

AMS 02 (2005-8)

(2003-6 )

ANTIMATTER LIMITS

End of the movie!!