High energy cosmic rays
ROBERTA SPARVOLI
ROME “TOR VERGATA” UNIVERSITY
AND INFN, ITALY
Nijmegen 2012
Lecture # 2 : outline

SATELLITE AND ISS EXPERIMENTS
 FUTURE ACTIVITIES
Click to edit Master text
styles
Satellite flights
PAMELA
Payload for Matter/antimatter Exploration and Lightnuclei Astrophysics
• Direct detection of CRs in space
• Main focus on antiparticles (antiprotons and positrons)
• PAMELA on board of Russian satellite Resurs DK1
• Orbital parameters:
- inclination ~70o ( low energy)
- altitude ~ 360-600 km (elliptical)
- active life >6 years ( high statistics)
Launch from Baykonur
 Launched on 15th June 2006
 PAMELA in continuous data-taking mode since then!
+
PAMELA
detectors
Main requirements:
- high-sensitivity
antiparticle
identification
- precise momentum
measurement
-
Time-Of-Flight
plastic scintillators + PMT:
- Trigger
- Albedo rejection;
- Mass identification up to 1 GeV;
- Charge identification from dE/dX.
Electromagnetic calorimeter
W/Si sampling (16.3 X0, 0.6 λI)
- Discrimination e+ / p, anti-p / e(shower topology)
- Direct E measurement for e-
Neutron detector
36 He3 counters :
- High-energy e/h discrimination
Spectrometer
microstrip silicon tracking system + permanent
magnet
It provides:
- Magnetic rigidity  R = pc/Ze
- Charge sign
- Charge value from dE/dx
GF: 21.5 cm2 sr
Mass: 470 kg
Size: 130x70x70 cm3
Power Budget:
360W
Click to edit Master text
styles
Flight data:
0.171 GV positron
Flight data:
0.169 GV electron
Antiparticles
SECONDARY ORIGIN, COMING FROM
INTERACTION OF PRIMARY CR WITH THE
INTERSTELLAR MEDIUM
Antiprotons
Antiproton/proton identification:
Negative/positive curvature in the spectrometer
 p-bar/p separation
Rejection of EM-like interaction patterns in the
calorimeter
 p-bar/e- (and p/e+ ) separation
Main issue:
Proton “spillover” background:
wrong assignment of charge-sign @ high energy due to
finite spectrometer resolution
Strong tracking requirements
•Spatial
resolution < 4mm
•R < MDR/10
Residual background subtraction
•Evaluated
with simulation (tuned with in-flight data)
•~30% above 100GeV
Antiproton
flux
• Largest energy range
covered hiterto
• Overall agreement with
pure secondary
calculation
• Experimental uncertainty
(statsys) smaller than
spread in theoretical
curves
 constraints on
propagation parameters
(Ptuskin et al. 2006) GALPROP code
• Plain diffusion model
• Solar modulation: spherical model ( f=550MV )
Adriani et al. - PRL 105 (2010) 121101
(Donato et al. 2001)
• Diffusion model with convection and
reacceleration
• Uncertainties on propagation param . and c.s.
• Solar modulation: spherical model ( f=500MV )
Antiproton-toproton ratio
Overall
agreement with
pure secondary
calculation
Very stringent
constraints
to exotic
production
mechanisms!
Adriani et al. - PRL 105 (2010) 121101
New
antiproton/pr
oton ratio
Using all data till
2010 and
multivariate
classification
algorithms 20-50%
increase in respect
to published
analysis
New
positron
fraction
data
Using all data till
2010 and
multivariate
classification
algorithms about
factor 2-3 increase in
respect to published
analysis
Positron/electron identification:
Positive/negative curvature in the spectrometer
 e-/e+ separation
EM-like interaction pattern in the calorimeter
 e+/p (and e-/p-bar) separation
Positrons
S1
CAT
TOF
SPE
CAS
S2
S3
Robust e+ identification
CALO

S4
ND
Main issue:
Interacting proton background:
 fluctuations in hadronic shower development:
p0 gg mimic pure e.m. showers
 p/e+: ~103 @1GV ~104 @100GV
Shower topology + energy-rigidity match
Residual background evaluation
Done with flight data
 No dependency on simulation

Click to edit Master text
styles
32.3 GV positron
Adriani et al. , Nature 458 (2009) 607
Adriani et al., AP 34 (2010) 1 (new results)
Positron
fraction
 Low energy
 charge-dependent
solar modulation
 High energy
 (quite robust)
evidence of
positron excess
above 10 GeV
(Moskalenko & Strong 1998)
GALPROP code
• Plain diffusion model
• Interstellar spectra
Adriani et al. , Nature 458 (2009) 607
Adriani et al., AP 34 (2010) 1 (new results)
Positron
fraction
 Low energy
 charge-dependent
solar modulation (see
tomorrow)
 High energy
 (quite robust)
evidence of
positron excess
above 10 GeV
(Moskalenko & Strong 1998)
GALPROP code
• Plain diffusion model
• Interstellar spectra
New
positron
fraction
data
Using all data till
2010 and
multivariate
classification
algorithms about
factor 2-3 increase in
respect to published
analysis
Positron Flux
Click to edit Master text
styles
A challenging puzzle for CR
physicists
Antiprotons
 Consistent with pure secondary
production
Positrons
 Evidence for an excess
Positron-excess
interpretations
(Cholis et al. 2009)
Contribution from DM
annihilation.
Dark matter
 boost factor required
 lepton vs hadron yield
must be consistent with pbar observation
Astrophysical processes
• known processes
• large uncertainties on
environmental parameters
(Blasi 2009)
e+ (and e-) produced as
secondaries in the CR
acceleration sites (e.g. SNR)
(Hooper, Blasi and Serpico,
2009)
contribution from diffuse
mature & nearby young
pulsars.
Interpretation: DM
M. Cirelli et al., Nucl. Phys. B 813 (2009) 1; arXiv: 0809.2409v3
Which DM spectra can fit the data?
DM
with
and
dominant
Click to
edit Master text
styles
annihilation
channel (possible candidate: Wino)
positrons
antiprotons
Interpretation: DM
M. Cirelli et al., Nucl. Phys. B 813 (2009) 1; arXiv: 0809.2409v3
Which DM spectra can fit the data?
DM
and
dominant
Click towith
edit Master text
styles
annihilation
channel (no “natural” SUSY candidate)
But B≈104
positrons
antiprotons
Interpretation: DM
M. Cirelli et al., Nucl. Phys. B 813 (2009) 1; arXiv: 0809.2409v3
DM with
Click
to edit Master text
channel
and
dominant annihilation
styles
positrons
antiprotons
Interpretation: DM
Click to edit Master text
styles
I. Cholis et al. Phys. Rev. D 80 (2009)
123518; arXiv:0811.3641v1
Astrophysical Explanation: SNR
Positrons (and
electrons)
Click to edit produced
Master text
asstyles
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.
P.Blasi et al., PRL 103 (2009) 051104 arXiv:0903.2794
Astrophysical Explanation: Pulsars
Are there “standard” astrophysical explanations of the
high energy positron data?
Click to edit Master text
styles
Young, nearby pulsars
Geminga pulsar
Not a new idea: Boulares, ApJ 342 (1989), Atoyan
et al (1995)
Astrophysical Explanation:
Pulsars
Click to edit Master text
styles  Mechanism:
the spinning B of the pulsar strips e- that
accelerated at the polar cap or at the outer gap emit γ that
make production of e± that are trapped in the cloud, further
accelerated and later released at τ ~ 105 years.
 Young (T < 105 years) and nearby (< 1kpc)
 If not: too much diffusion, low energy, too low flux.
 Geminga: 157 parsecs from Earth and 370,000 years old
 B0656+14: 290 parsecs from Earth and 110,000 years old.
 Diffuse mature pulsars
Astrophysical Explanation:
Pulsars
Click to edit Master text
styles
H. Yüksak et al., arXiv:0810.2784v2
Contributions of e- & e+ from Geminga
assuming different distance, age and
energetic of the pulsar
Mirko Boezio, Innsbruck,
diffuse mature &nearby young pulsars
Hooper, Blasi, and Serpico
arXiv:0810.1527
How to clarify the matter?
Click to edit Master text
styles
Courtesy of J. Edsjo
(Strong & Moskalenko 1998)
GALPROP code
(Kane et al. 2009)
• Annihilation of 180 GeV
wino-like neutralino
consistent with PAMELA
positron data
• Large uncertainties on
propagation parameters
allows to accommodate an
additional component
• A p-bar rise above 200GeV
is not excluded
(Donato et al. 2009)
• Diffusion model with
convection and reacceleration
(Blasi & Serpico 2009)
• p-bar produced as
secondaries in the CR
acceleration sites (e.g.
SNR)
consistent with PAMELA
positron data
Adriani et al. - PRL 105 (2010) 121101
Positrons
vs
antiprotons
+
Theoretical uncertainties on
“standard” positron fraction
γ = 3.54
γ = 3.34
Click to edit Master text
styles
Flux=A • E-g
T. Delahaye et al., Astron.Astrophys. 501 (2009) 821; arXiv: 0809.5268v3
Absolute fluxes of primary
GCRs
NEEDED FOR:
(a)IDENTIFY SOURCES AND ACCELERATION PROPAGATION
MECHANISMS OF COSMIC RAYS;
(b)ESTIMATE THE PRODUCTION OF SECONDARY PARTICLES,
SUCH AS POSITRONS AND ANTIPROTONS, IN ORDER TO
DISENTANGLE THE SECONDARY PARTICLE COMPONENT
FROM POSSIBLE EXOTIC SOURCES;
(c) ESTIMATE THE PARTICLE FLUX IN THE GEOMAGNETIC
FIELD AND IN EARTH'S ATMOSPHERE TO DERIVE THE
ATMOSPHERIC MUON AND NEUTRINO FLUX.
Adriani et al. , Science 332 (2011) 6025
H & He
absolute fluxes
• First high-statistics and
high-precision
measurement over three
decades in energy
• Dominated by systematics
(~4% below 300 GV)
• Low energy
 minimum solar activity
(f = 450÷550 GV)
• High-energy
 a complex structure of
the spectra emerges…
Spectral index
P & He
absolute fluxes
@ high energy
2.85
2.77 2.48
2.67
232 GV
Deviations from single
power law (SPL):
243 GV
 Spectra gradually soften
in the range 30÷230GV
 Abrupt spectral
SPL hp in the range 30÷230
GV rejected @ >95% CL
 SPL hp above 80 GV
rejected @ >95% CL

Solar modulation
Eg: statistical analysis for
protons
Solar modulation
hardening @ ~235 GV
Standard scenario of SN blast
waves expanding in the ISM
needs additional features
H/He ratio vs R
Instrumental p.o.v.
 Systematic uncertainties
partly cancel out
(livetime, spectrometer
reconstruction, …)
Theoretical p.o.v.
 Solar modulation negligible
 information about IS
spectra down to GV region
 Propagation effects
(diffusion and
fragmentation) negligible
above ~100GV
 information about source
spectra
(Putze et al. 2010)
P/He ratio vs R
 First clear evidence of
different H and He
slopes above ~10GV
 Ratio described by a single
power law (in spite of the
evident structures in the
individual spectra)
aHe-ap = 0.078 ±0.008
c2~1.3
2H
and 1H flux
Click to edit Master text
styles
2H/1H
3He
and 4He flux
Click to edit Master text
styles
3He/4He
2H/4He
Click to edit Master text
styles
Boron and Carbon nuclei spectra
Carbon
Click to edit Master text
styles
Boron
Anisotropy studies (p up to 1 TeV)
Click to edit Master text
styles
Electrons
NEEDED FOR:
(a)RECALCULATHE THE EXPECTED POSITRON FRACTION
WITH BETTER ACCURACY
(b)CLOSEBY SOURCES?
Results from ATIC
Click to edit Master text
styles
FERMI All-Electron Spectrum
Theoretical uncertainties on “standard” positron fraction
Click to edit Master text
styles
FERMI e+ + e- flux (2009)
A. Abdo et al., Phys.Rev.Lett. 102 (2009) 181101
M. Ackermann et al., Phys. Rev. D 82, 092004 (2010)
Electrons measured with H.E.S.S.
Click to edit Master text
styles
Electron
energy
measurements
Adriani et al. , PRL 106, 201101 (2011)
spectrometer
Two independent ways to
determine electron energy:
1. Spectrometer
•
•
Most precise
Non-negligible energy
losses (bremsstrahlung)
above the spectrometer
 unfolding
calorimeter
2. Calorimeter
•
•
•
Gaussian resolution
No energy-loss correction
required
Strong containment
requirements
 smaller statistical
sample
Electron identification:
• Negative curvature in the spectrometer
• EM-like interaction pattern in the calorimeter
Electron
absolute flux
e-
Adriani et al. , PRL 106, 201101 (2011)
 Largest energy range
covered in any
experiment hitherto
with no atmospheric
overburden
 Low energy
• minimum solar activity
(f = 450÷550 GV)
 High energy
No significant
disagreement with recent
ATIC and Fermi data
 Softer spectrum
consistent with both
systematics and growing
positron component

Spectrometric
measurement
Calorimetric
measurements
e+ +e-
New data: PAMELA Electron &
Positron Spectra
Click to edit Master text
styles
Flux=A • E-g
g = 3.18 ±0.04
Flux=A • E-g
g = 2.70 ±0.15
(e+ + e- )
absolute flux
 Compatibility with
FERMI (and ATIC) data
 Beware: positron flux
not measured but
extrapolated from
PAMELA positron flux!
 Low energy
discrepancies due to
solar modulation
ONLY AN EXERCISE ……..
(e+ + e- )
absolute flux
 Compatibility with
FERMI (and ATIC) data
 Beware: positron flux
not measured but
extrapolated from
PAMELA positron flux!
 Low energy
discrepancies due to
solar modulation
ONLY AN EXERCISE ……..
Solar and terrestrial physics
Discovery of
geomagnetically
Trapped
antiprotons
First measurement
of p-bar trapped in
the inner belt
29 p-bars
discovered in SAA
and traced back
to mirror points
p-bar flux exceeds
GRC flux by 3
orders of
magnitude, as
expected by
models
Adriani et al. –APJ Letters 737 L29, 2011
Discovery of
geomagnetically
Trapped
antiprotons
The geomagnetically
trapped antiproton-toproton ratio measured
by PAMELA in the SAA
region (red)
compared with the
interplanetary (black)
antiproton-to-proton
ratio measured by
PAMELA,
together with the
predictions of a trapped
model.
Solar modulation: p and He spectra
Click to edit Master text
styles
He
H
Solar modulation: e+ and eClick to edit Master text
styles
All
particles
PAMELA
results
Flux (m2 s sr GeV/N)-1
107
10
6
10
5
Proton (SAA)
104
Proton (Flare)
Proton
10
3
Helium
102
2
H (rat.)
3
10
He (rat.)
Antiproton (SAA)
Carbon
Electron
Results
span 4
decades
in energy
and 13 in
fluxes
1
Boron
10-1
Positron
10-2
Antiproton
10
-3
10-4
10
-5
10
-6
10-7
10-1
1
10
102
10
3
E (GeV/N)
FERMI OBSERVATORY
Click to edit Master text
styles
Orbiting Space Station
Click to edit Master text
styles
ALPHA MAGNETIC SPECTROMETER
Search for primordial anti-matter
Indirect search of dark matter
High precision measurement of the energetic spectra
and composition of CR from GeV to TeV
AMS-01: 1998 (10 days) - PRECURSOR FLIGHT ON THE SHUTTLE
AMS-02: Since May 19th, 2011, safely on the ISS. Four days after the
Endeavour launch, that took place on Monday May 16th, the experiment has
been installed on the ISS and then activated.
COMPLETE CONFIGURATION FOR >10 YEARS LIFETIME ON THE ISS
AMS-02 : the collaboration
FINLAND
RUSSIA
HELSINKI UNIV.
UNIV. OF TURKU
I.K.I.
ITEP
KURCHATOV INST.
MOSCOW STATE UNIV.
DENMARK
NETHERLANDS
USA
A&M FLORIDA UNIV.
JOHNS HOPKINS UNIV.
MIT - CAMBRIDGE
NASA GODDARD SPACE FLIGHT CENTER
NASA JOHNSON SPACE CENTER
UNIV. OF MARYLAND-DEPRT OF PHYSICS
UNIV. OF MARYLAND-E.W.S. S.CENTER
YALE UNIV. - NEW HAVEN
UNIV. OF AARHUS
ESA-ESTEC
NIKHEF
NLR
GERMANY
RWTH-I
RWTH-III
MAX-PLANK INST.
UNIV. OF KARLSRUHE
FRANCE
ROMANIA
GAM MONTPELLIER
LAPP ANNECY
LPSC GRENOBLE
ISS
UNIV. OF BUCHAREST
SPAIN
CIEMAT - MADRID
I.A.C. CANARIAS.
MEXICO
UNAM
PORTUGAL
LAB. OF INSTRUM. LISBON
SWITZERLAND
ETH-ZURICH
UNIV. OF GENEVA
ITALY
ASI
CARSO TRIESTE
IROE FLORENCE
INFN & UNIV. OF BOLOGNA
INFN & UNIV. OF MILANO
INFN & UNIV. OF PERUGIA
INFN & UNIV. OF PISA
INFN & UNIV. OF ROMA
INFN & UNIV. OF SIENA
KOREA
EWHA
KYUNGPOOK NAT.UNIV.
CHINA BISEE (Beijing)
IEE (Beijing)
IHEP (Beijing)
SJTU (Shanghai)
SEU (Nanjing)
SYSU (Guangzhou) TAIWAN
SDU (Jinan)
ACAD. SINICA (Taiwan)
CSIST (Taiwan)
NCU (Chung Li)
NCKU (Tainan)
NCTU (Hsinchu)
NSPO (Hsinchu)
The AMS-02 detector
Click to edit Master text
styles
AMS first events
Click to edit Master text
styles
42 GeV Carbon nucleus
FIRST AMS RESULT?
Click to edit Master text
styles

So far no physics results given by the
collaboration to the science community;
 First results expected for the the
4th International Conference on Particle
and Fundamental Physics in Space
(SpacePart), which will take place at CERN
from November 5th to November 7th 2012.
Click to edit Master text
styles
Future
experiments
CALET:
78 Calorimetric Electron Telescope
CGBM
Main Telescope: Calorimeter (CAL)
• Electrons: 1 GeV – 20 TeV
• Gamma-rays: 10 GeV – 10* TeV
(Gamma-ray Bursts: > 1 GeV)
• Protons and Heavy Ions:
several tens of GeV – 1,000* TeV
• Ultra Heavy Ions： over the rigidity cut-off
Gamma-ray Burst Monitor (CGBM)
• X-rays/Soft Gamma-rays: 7keV – 20MeV
CAL
(* as statistics permits)
Science objectives:
 Nearby cosmic-ray sources through electron spectrum in the trans-TeV region
 Signatures of dark matter in electron and gamma-ray energy spectra in the 10
GeV – 10 TeV region
 Cosmic ray propagation in the Galaxy through p – Fe energy spectra, B/C ratio,
and UH ions measurements
 Solar physics through electron flux below 10 GeV
 Gamma-ray transient observations
CALET Payload Overview
CGBM/
SGM
Click to edit Master text
styles
FRGF( Flight
Releasable
Grapple Fixture)
CGBM/
HXM
ASC (Advanced
Stellar Compass)
CAL/CH
D
GPSR
(GPS
Receiver)
 Launch carrier: HTV-5
 Launch target date: CY 2014
 Mission period: More than 2 years
(5 years target)
 Data rate:
 Medium data rate: 300 kbps
 Low data rate: 20 kbps
MDC (Mission
Data Controller)
CAL/IMC
CAL/TAS
C
 Mass: 650kg (Max)
 Standard Payload Size
 Power: 500W (Max)
Main Telescope: CAL (Calorimeter)
450 mm
 CHD (Charge Detector):
 Double layer segmented
plastic scintillator array
(14 x 2 layer with a unit of
32mm x 10mm x 450mm)
 Charge measurement
(Z=1 – 40)
Click to edit Master text
styles
Shower particles
 IMC (Imaging Calorimeter):
 7 layers of tungsten plates with 3 r.l.
separated by 2 layers of scintillating
fiber belts which are readout by MAPMT.
 Arrival directions, Particle ID
 TASC (Total Absorption Calorimeter):
 12 layers of PWO logs (19mm x
20mm x 326mm) with total thickness
of 27 r.l. The top layer is used for
triggering and readout by PMT. Other
layers are readout by PD/APD.
 Energy measurement, Particle ID
Gamma-400 on Russian satellite
It will combine for the first time photon and particle (electrons and nuclei)
detection in a unique way
Click to edit Master text

styles
Excellent Silicon Tracker (30 MeV – 300 GeV),
breakthrough angular resolution 4-5 times better than
Fermi-LAT at 1 GeV
 improved sensitivity compared with Fermi-LAT by a factor of
5-10 in the energy range 30 MeV – 10 GeV

 Heavy Calorimeter (25 X0) with optimal energy
resolution and particle discrimination
Electron/positron detection up to TeV energies
 Nuclei detection up to 1015 eV energies

Click to edit Master text
styles
Counts estimation, electrons
G400 configuration: CsI(Tl), 20x20x20 crystals
Size: 78.0x78.0x78.0 cm3 – gap 0.3 cm
Taking into account: geometrical factor and exp. duration +
selection efficiency 80%
Experiment
Duration
Planar GF
(m2 sr)
CALET
5y
0,12
~2%
AMS02
10 y
0,5**
ATIC
30 d
0,25
FERMI
G400
e/p
rejection
factor
E > 0.5 TeV
E > 1 TeV
E > 2 TeV
E > 4 TeV
30 X0
105
3193
611
95
10
~2%
16 X0
103 **
26606
5091
794
84
~2%
18 X0
104
109
21
3
0
10 y
1,6@300
GeV *
0,6@800
GeV *
~15% 8,6 X0
104
59864
2545
0
0
10 y
8,5
~0,9% 39 X0
106
452303
86540
13502
1436
* efficiencies included
Calo Calo
s(E)/E depth
** calorimeter standalone
Counts estimation, protons and helium nuclei
Polygonato model
G400 configuration: CsI(Tl), 20x20x20 crystals
Size: 78.0x78.0x78.0 cm3 – gap 0.3 cm
Taking into account: geometrical factor and exp. duration + selection
efficiency 80%
Experiment
Duration
Planar
GF
(m2 sr)
CALET
5y
0,12
CREAM
180 d
0,43
ATIC
30 d
0,25
TRACER
30 d
5
G400
10 y
8,5
e sel
e conv
0,8
0,5
* carbon target
0,8
0,8
0,4
E > 0.5 PeV
E > 1 PeV
E > 2 PeV
E > 4 PeV
p
He
p
He
p
He
p
He
p
He
Calo
depth
~40%
30 X0
1,3 l0
146
138
9
10
2
3
1
1
0
0
~45%
20 X0
1,2 l0
41
39
3
3
1
1
0
0
0
0
~37%
18 X0
1,6 l0
5
5
0
0
0
0
0
0
0
0
-
TRD
200
189
12
13
3
4
1
1
0
0
~20%
39 X0
1,8 l0
16521
15624
979
1083
261
326
60
92
10
21
0,8
0,5 CT*
E > 0.1 PeV
Calo
s(E)/E
0,8
0,4 CT*
~ knee
Counts estimation, heavier nuclei (3 ≤ Z ≤ 24)
Polygonato model
G400 configuration: CsI(Tl), 20x20x20 crystals
Size: 78.0x78.0x78.0 cm3 – gap 0.3 cm
Taking into account: geometrical factor and exp. duration + selection
efficiency 80%
Experiment
Duration
Planar
GF
(m2
sr)
CALET
5y
0,12
e sel
e conv
E > 0.1 PeV
Calo
s(E)/E
0,8
0,46
0,25
TRACER
30 d
5
G400
10 y
8,5
*carbon target
** better than 20% using TRD
0,5 CT*
0,8
0,8
0,4
to
3Li
to
10Ne
to
3Li
to
10Ne
to
3Li
to
10Ne
E > 4 PeV
to
3Li
to
10Ne
to
9F
24Cr
9F
24Cr
9F
24Cr
9F
24Cr
9F
24Cr
70
5
5
1
2
0
1
0
0
~45% **
20 X0
1,2 l0
21
21
1
1
0
0
0
0
0
0
~37%
18 X0
1,6 l0
2
2
0
0
0
0
0
0
0
0
TRD
TRD
93
96
6
7
2
2
1
1
0
0
~17%
39 X0
1,8 l0
7698
7910
533
555
169
180
51
60
15
17
0,8
30 d
10Ne
E > 2 PeV
68
0,4 CT*
ATIC
to
E > 1 PeV
30 X0
1,3 l0
0,8
180 d
3Li
E > 0.5 PeV
~30%
0,5
CREAM
Calo
depth
~ knee
ISS-CREAM
 The idea is to put the CREAM detector, developed
as a Long Duration balloon experiment, onboard
the ISS, at the Japanese Experiment Modules
Exposed Facility (JEM-EF) KIBO.
 The 1,200 kg estimated mass of the payload is over
twice the mass of any previously launched payload
using the JAXA’s HTV. The development team will
modify the existing instruments to meet the new
requirements of the launch vehicle and ISS.
 Very good chance to reach 1015 eV.
Click to edit Master text
styles
Conclusions
With respect to the standard GCR scenario, what
have we learned by the recent direct measurements?
Click to edit Master text
styles
High energy line
 H and He spectra are different
 H and He spectra harden with energy (230 GV)
 Hi-Z spectra might show similar hardening
 Energy dependance of propagation still undecided
Composition line
 Source matter must be a composition of old ISM with
newly sinthetized matherial, in percentage 80%-20% (sites
of acceleration rich in massive stars?)
Conclusions
Antimatter line
Click to edit Master text
styles
All electron spectrum
shows enhancement at high
energy (hundreds GeV). Nearby source?
 Positrons show enhancement in the E>10 GeV region
(new e+ e- source. Correlated to previous?)
 No antiproton excess observed both at low and high
energy (several DM models and exotics ruled out)
 No heavier anti-nucleus observed (very stringent limits)
New fresh data from AMS-02 could improve the understanding of
some of the still open issues in the direct measurements sector
THANK YOU!