Recent results and and perspectives perspectives on on Recent - - PowerPoint PPT Presentation
Aspen Winter 2009 Workshop on Physics at the LHC era Recent results and and perspectives perspectives on on Recent results cosmic ray matter and cosmic ray matter and antimatter from antimatter from Pamela experiment experiment
Bari Florence Frascati
Trieste Naples Rome CNR, Florence Moscow
Siegen
KTH, Stockholm
89 1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 2003 2004 2005 2006 ...
Past, present and future experiment Past, present and future experiment
C 94 C 97 C 98 TS 93 89 M 91
MASS-89, 91, TS-93, CAPRICE 94-97-98 PAMELA
PAMELA
NINA-2 NINA-1
NINA-1 NINA-2
SILEYE-2 SILEYE-1
SILEYE-3/ ALTEINO: SILEYE- 4/ALTEA SILEYE-1 SILEYE-2 SILEYE-3 ALTEA LAZIO-SIRAD LAZIO-SIRAD SIRAD
Neutron Stars
White Dwarfs . 1020 eV protons
1 012 e V p r
s
109 eV protons
Cosmic ray acceleration
p, p- He
B/C Search for Dark Matter p-
Neutron Stars
White Dwarfs . 1020 eV protons
1 012 e V p r
s
109 eV protons
Propagation on the local part of the galaxy
e+/e- Search for Dark Matter (e+)
Neutron Stars
White Dwarfs . 1020 eV protons
1 012 e V p r
s
109 eV protons
Heliospheric phenomena, charge dependent solar modulation e+/e- p-/p+ Anomalous cosmic rays P, He, C
Neutron Stars
White Dwarfs . 1020 eV protons
1 012 e V p r
s
109 eV protons
Solar particle events Acceleration, shock, stochastic, CME P, He, CNO e-
Neutron Stars
White Dwarfs . 1020 eV protons
1 012 e V p r
s
109 eV protons
Magnetosphere: Earth Van Allen belt p, e- Jupiter e- interpl.
Adapted from Si mpson 1983 in PDG by M. Casolino
GF GF ~ 20.5 cm ~ 20.5 cm2sr sr Mass: 470 kg Mass: 470 kg Dim Dim: 120x40x45 cm : 120x40x45 cm3 Power: 360 W Power: 360 W
Calorim eter SI-W: 44 planes 96 strip 16 X0 0.6 int 22 W 0.26cm
Tracker (B= .43T)
MDR from test beam 1 TV ND: 36 tubes 3He Discrimin p/ e > 10 E> 10 GeV/ c
TOF (6 planes, 3 pairs, 48 PMT) : (paddle) 110 ps (ToF) 330 ps (MIPs)
3 double-layer scintillator paddles
350 mm2 7 mm 180 x 50 mm2 3 S32 420 mm2 7 mm 150 x 60 mm2 3 S31 450 mm2 5 mm 150 x 90 mm2 2 S22 375 mm2 5 mm 180 x 75 mm2 2 S21 385 mm2 7 mm 408 x 55 mm2 6 S12 357 mm2 7 mm 330 x 51 mm2 8 S11
Adapted from W. Menn
assembled in an aluminum mechanics
mm
magnetic cavity : 0.43 T Geometric Factor: 20.5 cm2sr
Adapted from E.Vannuccini ............................................................ ICRC2005 – Pune (India)
6 detector planes composed by 3 “ladders”
(1 plane = 0.3% X0)
to the ladders
compromise:
channels
E.Vannuccini ....................................................................................... ICRC2005 – Pune (India)
sx = (2.77 ± 0.04) m sy = (13.1 ± 0.2) m
40-100 GeV pions (CERN-SPS 2000) beam-test of a small tracking-system prototype
(> 300 GeV; GF~600 cm2 sr)
GeV
Adapted from V. Bonvicini
Lebedev Physical Institute Academy of Science, Russia
3He tube
Flight data: 14.4 GV non-interacting proton
From E. Mocchiutti
Flight data: 36 GV interacting proton
Flight data 84 GeV/c interacting antiproton
Flight data: 2.8 GV electron
Flight data: 92 GeV/c positron
14.7 GV Interacting nucleus (Z = 8)
Galactic cosmic ray Matter / Antimatter / Dark Matter
Rcutoff=14.9GV/L2
albedo particles antiparticles albedo particles antiparticles
4He+d
albedo particles antiparticles albedo particles antiparticles
Energy loss from tracker
BESS
Caprice / Mass /TS93
AMS-01 Pamela
1.5 2.0 2.5 3.0 3.5 1955 1965 1975 1985 1995 2005 Y e ar Nm, сm
Rc= 2.4 CV Rc = 0.03 и 0.6 GV
)) ( , ( )) ( ( ) , , (
2 2 2 2 2
t E J E t E E E t E r J Balloon: low frequency modulation Pamela: low and high frequency modulation Long solar minimum Variation in Galactic flux Short Term (months) Long term (years) Charge dependence
(e.g. Asaoka Y. et al. 2002, Phys.
Dati meteor 0.03 GV 0.6 GV, Stozkov 2008
July 2006 August 2007
February 2008
Spectral index 2.76
)) ( , ( )) ( ( ) , , (
2 2 2 2 2
t E J E t E E E t E r J
0.7 R is
p/(cm2 s sr GV)
Solar modulation parameters (GV) error
JUL06 5.01-01 2e-03 JAN07 4.16-01 2-03 AUG07 4.02-01 3-03
Turquoise 0.3 G < B Yellow 0.22 G < B < 0.23 G Blue 0.21 G < B < 0.22 G Green 0.20 G < B < 0.21 G Red 0.19 G < B < 0.20 G Black B<0.19 G
P/(cm^2 sr GeV s)
Integral Pamela flux (E>35 MeV) (PSB97 plot by SPENVIS project, model by BIRA-IASB)
10. 4.7±1.8 8.1±1.8 (5±3) 10-4 verde 6.8 2.6±0.6 5.9±0.5 (2.3±0.3) 10-2 rosso 7.1 3.1±0.5 6.0±0.4 0.11±0.01 nero χ2/ndf γ1 γ0 A
) (
1
E
Arxiv 0810.4980v1
Atmospheric neutrino contribution Astronaut dose on board International Space Station Indirect measurement of cross section in the atmosphere Agile e Glast background estimation
Arxiv 0810.4980v1
Athay, R. G. and Moreton, G. E.: 1961, Astrophys. J. 133, 935.
OSPAN H-alpha (656.3 nm) - AR 10930
Quiet time spectrum
Impulsive increase Decrease of high energy component Increase of low energy component
Magnetic Field Neutron Monitor X-ray P,e-
Discrimination between acceleration processes
E-a exp(E/Eo)
accel. Impulsive events Exp in Rigid/Kinene Bessel function,
in magnetic reconnection
Arxiv 0810.4980v1
p d
3He 4He
Li Be B,C track average e±
Boron is a secondary particle. Its abundance is relevant for propagation in the Galaxy
4% 23%
73%
Adapted from M. Boezio, P. Picozza
LSP – can not decay But can annhilate
Bosonic Dark Matter: fermionic final states no longer helicity suppressed. e+e- final states directly produced. As in the neutralino case there are 1-loop processes that produces monoenergetic γ γ in the final state.
From P. Picozza
Detection, not identification
Supersymmetry, not necessarily DM
DAMA
Local structure and nature Galactic centre Antiprotons: Galactic average positrons: Local galactic 1kpc
Various galactic scales
Depends on propagation in the galaxy
Background – free channel to study rare phenomena such as Dark matter decay
ISM CR
‘Electron’ ‘Hadron’ From M. Boezio
From E. Vannuccini, P. Papini
MDR > 850 GV Minimal track requirements Strong track requirements:
clusters along the trajectory
Protons (& spillover)
From O. Adriani
Antiprotons
p-bar p
10 GV 50 GV
From O. Adriani
R < MDR/ 10
p-bar p
10 GV 50 GV
From O. Adriani
Why Ratios? Reduce systematic error All (most) efficiencies cancel out Subsequently absolute fluxes
Uncertainties in Galactic propagation Uncertainties in heliospheric propagation Released data 1-100 GeV Currently roughly 10 TB
As of March ’08 Out of 8.8 TB
arXiv:0810.4994v1 [astro-ph] 28 Oct 2008 Accepted - PRL
ApJ 457, L 103 1996 ApJ 532, 653, 2000
arXiv:0810.4994v1 [astro-ph] 28 Oct 2008 Accepted - PRL
energy up to now
secondary production
Propagation
Moskalenko 2002 (except highest energy)
– Montecarlo – Test Beam – In flight data – Cross-checked with Neutron Detector
Recipe: M. Boezio, E. Mocchiutti
Take interacting protons in BigBottom (known sample of hadronic shower. No leptons)
Using “BigTop” for e.m. showers (electrons) “BigBottom” for hadronic showers (protons)
P hadronic shower e+/- e.m. shower
p (non-int)
p (non-int)
Fraction of charge released along the calorimeter track (left, hit, right)
p (int)
p (int)
Rigidity: 20-30 GV
From P. Picozza, M. Boezio, E. Vannuccini
Fraction of charge released along the calorimeter track (left, hit, right)
Energy-momentum match
Rigidity: 20-30 GV
From P. Picozza, M. Boezio, E. Vannuccini
Fraction of charge released along the calorimeter track (left, hit, right)
Rigidity: 20-30 GV
From P. Picozza, M. Boezio, E. Vannuccini
e e- p p
Neutrons detected by ND
Rigidity: 20-30 GV
Fraction of charge released along the calorimeter track (left, hit, right)
e e+
Secondary production ‘Leaky box model’ (Protheroe 1982) Secondary production ‘Moskalenko + Strong model’ (1998) without reacceleration
Primary production from annihilation (m() = 336 GeV)
arXiv:0810.4995v1 [astro-ph] 28 Oct 2008 Accepted on Nature
20000 positrons from 200 MeV up to 200 GeV have been analyzed
positrons over 1 GeV
data to be analyzed
arXiv:0810.4995v1 [astro-ph] 28 Oct 2008 Accepted on Nature
modulation
solar cycles
channel by BESS
equation – drift term depends
BESS
Caprice / Mass /TS93
AMS-01 Pamela
Pamela
Pamela e+ Pamela p-
Clem et al. 30th ICRC 2007
According to BBE2008
directly (helicity suppression of light fermions in the annihilation process)
like Kaluza-Klein dark matter
(“virtual” internal bremsstrahlung (IB), or direct emission) can have a significant impact
not only to an even more pronounced cutoff, but also to clearly observable bump-like features at slightly lower energies
the gamma-ray flux at photon energies close to m_neutral
Potgieter at al. arXiv:0804.0220v1
Nature, 456, 362 20 November 2008 doi:10.1038/nature07477