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Silicon Detectors for the Search of
Cosmic Antimatter and Dark Matter
Piergiorgio Picozza
INFN and University of Rome Tor Vergata
From e+/e- Colliders to High Energy Astrophysics
Trieste, September 7, 2010
Astrophysics and Cosmology
compelling Issues
Apparent absence of cosmological Antimatter
Nature of the Dark Matter that pervades the Universe
AMSPAMELA AMS
in Space
Accelerators
The Big Bang origin of the Universe requires
matter and antimatterto be equally abundant at the very hot beginning
Search for the existence of Antimatter in the Universe
Gamma Evidence for Cosmic Antimatter?
Steigman 1976, De Rujula 1996, Dolgov 2007
Osservation in the 100 MeV gamma range
Leading process:p p 0+ ………
Other processes:p p +……… μ+……… e+……… γ 1-10 MeV
e+e- γ γ 0.511 MeV
Antimatter Direct research
Observation of cosmic radiation hold out the possibility of directly observing a particle of antimatter which has escaped as a cosmic ray from a distant antigalaxy, traversed intergalactic space filled by turbulent magnetic field, entered the Milky Way against the galactic wind and found its way to the Earth.
Streitmatter, R. E., 24th ICRC , Rome, Italy, 1995Nuovo Cimento, 19, 835 (1996)
High energy particle or antinuclei
THE UNIVERSE ENERGY BUDGET
DM annihilations
DM particles are stable. They can annihilate in pairs.
Primary annihilation channels Decay Final states
σa= <σv>
Gamma Evidence for Cosmic Antimatter
and Dark Matter?
OSO-31967 - 1969
SAS-2
1972 - 1973
GRO: Comptel and EGRET
1991 - 2000
COS-B
1975 - 1982
Energy Calorimeter
Spark Chamber
Trigger Telescope
Cerenkov Counter
Anti-Coincidence
Dome
Cos-B
8/1975-4/1982SAS-2
11/1972-7/1973
EGRET
4/1991-1999
The gamma-
ray
missions
Cosmic Diffuse Gamma Spectrum
P. Sreekumar et al, astroph/9709257
Robert L. Golden R.
Balloon data : Positron fraction before 1990
leaky box
dinamic halo
m =20GeV
Tilka 89
MASS Matter Antimatter Spectrometer
MASS 1989
electron proton
The Turning Point
Calorimeter Performance
TS 93 Si-W Calorimeter
Wizard Si-W Calorimeter for Cosmic Antimatter SearchNuclear Physics B 32 (1993) 77-82
TS 93 NIM A 360 (1995) 17-21
electron positron
23
Elements of a pair-conversion
telescope
• photons materialize
into matter-antimatter
pairs:
E --> me+c2 + me-c2
• electron and positron
carry information about
the direction, energy and
polarization of the -ray
(energy measurement)
GILDA
Fermi
GLAST
CAPRICE FLIGHTSCANADA & NEW MEXICO
CAPRICE Calorimeter
• Charge sign and
momentum
• Beta selection
• Z selection
• hadron – electron
discrimination
CapriceSubnuclear physics
techniques
in space experiments
Antiproton Positron
positron to electron ratioCAPRICE 94
antiproton to proton ratioCAPRICE 98
AMS 01
AMS-01 Silicon tracker
AMS - 01
ZENIT rocket Baikonur, Kazakhstan July 10 1998
COSMOS rocket
Plesetsk, Russia July 15 2000
NINA2-MITA
89 440 km
NINA-RESURS
97 810 km
NINA MissionsNuclei P-Fe
10-200 MeV/n
Cosmic Rays: Galactic
Trapped
Solar Flares
NINA 1
NINA 2
Light Flashes on board Mir Space Station
1995 Cosmonaut Sergej Avdeev with the SilEye-1 detector on board of the Mir Station
Cosmonaut S. Avdeev during measurements with SilEye-2 apparatus on “Mir” Space Station
Antimatter Search
BESS (93, 95, 97, 98, 2000)
Heat (94, 95, 2000)
IMAX (96)
BESS LDF (2004, 2007)
AMS-01 (1998)
Wizard Collaboration
MASS – 1,2 (89,91)
TrampSI (93)
CAPRICE (94, 97, 98)
Cosmic Ray Antimatter
AntiprotonsPositrons
CR + ISM ± + x ± + x e± +
x
CR + ISM 0 + x e±
Moskalenko & Strong 1998 Positron excess?
Charge-dependent
solar modulation
Solar polarity reversal
1999/2000
Asaoka Y. Et al. 2002
¯
+
CR + ISM p-bar + …
kinematic threshold:
5.6 GeV for the reaction
pppppp
Pre-PAMELA
What did we need?
Measurements at higher energies
Better knowledge of background
High statistics
Continuous monitoring of solar modulation
Long Duration Flights
Antimatter and Dark Matter
Space MissionsPAMELA
15-06-2006
AMS-02
02-2011
Fermi/GLAST
11-6-2008
AGILE
23-04-2007
PAMELAPayload for Antimatter Matter Exploration
and Light Nuclei Astrophysics
PAMELA Instrument
GF ~21.5 cm2sr
Mass: 470 kg
Size: 130x70x70 cm3
100MDR ~ 1.2 TeV
Mirko Boezio, COSPAR, Bremen, 2010/07/18
The tracking system
Main tasks:• Rigidity measurement
• Sign of electric charge
• dE/dx
Characteristics:• 6 planes double-side (x&y view) microstrip Si sensors
• 36864 channels
• Dynamic range 10 MIP
Performances:• Spatial resolution: 3 4 m
• MDR ~1.2TV (from flight data)SPECTROMETER
PAMELA
PAMELA Si-W Calorimeter
Flight data: 0.632 GeV/cantiproton annihilation
Mirko Boezio, COSPAR, Bremen, 2010/07/18
Flight data: 0.763 GeV/cantiproton annihilation
Flight data: 84 GeV/c
interacting antiproton
Flight data: 92 GeV/c
positron
Mirko Boezio, COSPAR, Bremen, 2010/07/18
Flight data: 14.7 GV
Interacting nucleus
(Z = 8)
Antimatter and Dark Matter Search
ANTIPROTONS
Antiproton Flux(0.06 GeV - 180 GeV)
Donato et al. (ApJ 563 (2001) 172)
Ptuskin et al. (ApJ 642 (2006) 902)
Adriani et al., astro-ph 1007.0821 PRL in press
Systematics
errors included
Antiproton to proton ratio (0.06 GeV - 180 GeV)
Donato et al. (PRL 102 (2009) 071301)
Simon et al. (ApJ 499 (1998) 250) Ptuskin et al. (ApJ 642 (2006) 902)
Adriani et al., astro-ph 1007.0821 PRL in press
Systematics
errors included
Wino Dark Matter in a non-thermal Universe
G. Kane, R. Lu, and S. Watson
arXiv:0906.4765v3 [astro-ph.HE)
Trapped antiprotons in SAA
GCR
Trapped
PAMELA
Trapped antiprotons in SAA
Trapped
GCR
PAMELA
Positrons
Positron to Electron Fraction
Secondary productionMoskalenko & Strong 98
Adriani et al, Astropart. Phys. 34 (2010) 1 arXiv:1001.3522 [astro-ph.HE]
A Challenging Puzzle for CR Physics
P.Blasi, PRL 103 (2009) 051104; arXiv:0903.2794Y. Fujita arxiv .0904.5298Positrons (and electrons) produced as secondaries in the sources (e.g. SNR) where CRs are accelerated.But also other secondaries are produced: significant increase expected in the p/p and B/C ratios.
I. Cholis et al., Phys. Rev. D 80 (2009) 123518; arXiv:0811.3641v1
Contribution from DM annihilation.
D. Hooper, P. Blasi, and P. Serpico, JCAP 0901:025,2009; arXiv:0810.1527Contribution from diffuse mature &nearby young pulsars.
Antiprotons in CRs are in agreement with secondary production
A Challenging Puzzle for Dark Matter
Cosmic Ray Spectra
Cosmic Rays Propagation in the
Galaxy
Electrons
Electron (e-) Spectrum
All electrons
e+ + e-
All electron spectrum
96 CsI(Tl)8 layers
ATIC GLAST
HESS
All three ATIC flights are consistent
ATIC-4 with 10 BGO layers has improved
e , p separation. (~4x lower background)
“Bump” is seen in all three flights.
ATIC 1+2
“Source on/source off” significance of bump for ATIC1+2 is
about 3.8 sigmaJ Chang et al. Nature 456, 362 (2008)
Significance for ATIC1+2+4 is 5.1 sigma
ATIC 1+2+4
Preliminary
ATIC 1
ATIC 2
ATIC 4
Preliminary
Fermi (e++ e-)
M. Ackermann et al. astro-ph 1008.3999
Fermi (e++ e-)
M. Ackermann et al. astro-ph 1008.3999
The Completed AMS Detector on ISSTransition Radiation
Detector (TRD)
Silicon Tracker
Electromagnetic Calorimeter (ECAL)
Magnet
Ring Image Cerenkov Counter (RICH)
Time of Flight Detector (TOF)
Size: 3m x 3m x 3mWeight: 7 tons
AMS-02 new configuration
Combining searches in different channels could
give (much) higher sensitiviy to SUSY DM signals
antiprotons
positrons
gamma rays
anti deuterons
Unique
Feature
of
AMS
The Future
Gamma Space
Experiments
W. B. Atwood Talk
AGILE
23-04-2007Fermi/GLAST
11-6-2008
AGILE
the most compact
instrument for high-
energy astrophysics
It combines for the first
time a gamma-ray
imager (30 MeV- 30 GeV)
with a hard X-ray
imager (18-60 keV) with
large FOVs (1-2.5 sr) and
optimal angular
resolution
AGILE in orbit
April 23, 2007
ISRO Sriharikota base, PSLV-C8
Dark Matter Fermi
astro-ph 0912.0973
Third EGRET Catalog 1991-2000, 270 sources , 1.5
M ’s
AGILE 2.5 yr gamma ray map
FERMI Catalog (11 months, 1451 sources)
arXiv:1002.2280
http://fermi.gsfc.nasa.gov/ssc/data/access/lat/1yr_catalog/
Many Thanks
Guido!