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1 KEK I. II. a. BESS b. c. d. III. BESS-Polar IV.
2 Introduction
3 D
4 p GeV (<1GeV )
5 D B.G. free D (Fuke et al.) D D D (<1GeV/n)
6 LSP WIMP Dark Matter χ jet fragmentation D K.Mori et al, APJ 566 (2002) 604
7 PBH PBH D
8 D BESS : σ t C
9 BESS Detector
10 BESS Spectrometer BESS 99 T ~ 0.3m 2 sr, ~8-10 g/cm 2 / wall Rigidity (=Pc/Ze), β (σ t ~70ps), de/dx
11 Trigger
12 Balloon Flights
13 BESS Balloon Flight Launch up to ~36km (~5mbar) BESS spectrometer ~200m
14 Data Taking Live Time (hr) Mean Air Depth (g/cm 2 )
15 Analysis
16 Event Selection Pre-Selection single track downward going fully contained N TOF = 1 or 2 Upper TOF de/dx Quality Cut trajectory fitting Paticle Identification de/dx vs Rigidity 1/β vs Rigidity Aerogel Chrenkov OK NG
17 Fiducial Volume
18 Quality Cuts Hits used in trajectory fitting χ 2 of trajectory fitting Dropped hits Trajectory agreement with IDC hits ( r-φ, z ) Trajectory agreement with TOF hits ( r-φ, z ) (TOF, de/dx)
19 Particle ID
20 Upper TOF de/dx dx cut Eliminate recoil deuterons ( fake events ) broad tail in upper de/dx Tighter than lower / JET de/dx
21 Particle ID
22 1/β cut
23 Silica aerogel veto cut eliminate e - /µ - backgrounds especially in high β region (1/β < 1.1) 97 n= ~ 00 n=1.02
24 Survived Events No D candidate
25 Deuteron Samples Number of D samples Rigidity (GV) < < < < 3.59 Efficiency
26 Possible Contamination D ( in R >2.3 GV where p 1/β band overlaps D band ) D p ~ 1 event / 4 flights (+3.89σ) ( c.f. ~ 0.1 event / 4 flights (+6σ) ) e - /µ - ~ 0.1 times p contamination p < 0.5 % T < 1 % e + /µ +, He << 0.1 %
27 Results D
28 Outline conservative D ( independent ) obs Φ D Ω total live 2 1 N S ε T ( E E )(1 sys. err) min ε = ε ε ε ε ε ε ε ε ε ε total trig rec pre qual d E/dx 1/ β agl acctrk acchit air
29 Normalization, Correction 3.09 for 95% C.L. upper limit (with null b.g.) obs Φ D Ω total live 2 1 N S ε T ( E E )(1 sys. err) min Monte Carlo simulation (GEANT) Measured by 1 MHz-clock
30 Normalization, Correction ε = ε ε ε ε ε ε ε ε ε ε total trig rec pre qual d E/dx 1/ β agl acctrk acchit air D sample p sample random p beam M.C.
31 Cross section Elastic/inelastic cross sections of D scale those of p by hard sphere model σ 1/3 1/3 1/3 1/3 ( Ai, At) Ai + At 0.71( Ai + At ) Inelastic interaction D is fragmented or annihilated 2
32 Efficiency of Quality Cut Quality cut efficiency basically from Deuteron data. In high-e region, quality cut is essential for p/d separation. Estimated by using both of data and MC. ε qual ε = εqdata ( p) ε qmc qmc ( D) ( p) simulated ε ε qmc qmc ( D) ( p) ε ( p) qdata estimated ε qual
33 Efficiencies
34 ( ε ) ( ) Systematic errors SΩ Tlive total SΩ T ε live trig ε ε rec = SΩ T ε SΩ T ε ε ε live total live trig rec pre ε ε ε ε ε ε ε ε ε ε ε ε ε ε qual de/dx 1/ β agl acctrk acchit air qual de/dx 1/ β agl acctrk acchit air pre dominant ~ 9 % 2nd largest ~ 6 % 3rd largest ~ 3 % Total ~ 10.4 % The above three efficiencies from MC. Uncertainty in cross sections is not considered ( fixed by the assumption )
35 Effective exposure factor
36 D x10-4 ( sum ) (m 2 s sr GeV/n) x x x x GeV/n
37 Discussions
38 Prediction of D s D s from PBHs Calculation steps Particle emission Coalescence model Source spectrum Interstellar spectrum Solar modulation
39 Particle Emission dn s 2s dt 2 π [exp( Q/ kt) ( 1) ] d 2 N = N det d = 3 c T 8π GMk M j Γ Q= E dq emission spectrum Γs d g ( Q, E) j jn α j dq 2s j 2 π [exp( Q/ kt) ( 1) ] de antinucleon emission rate g GeV T vs. M relation M t 14 u 1/ ( ) g initial mass of expring PBHs 13.7Gyr
40 Coalescence model d n 4 d n d d 3 p n 4 n D n 3 p γ = π p 3 0 γ p 3 γ 3 π 0 γ 3 dp 3 dp dp 3 dp 2 Coalescence momentum p 0 = 130MeV/c c.f. Other predictions of D spectra p 0 ~110~160MeV/c A+A accelerator (Low E) p 0 ~140~210MeV/c Theoretically p 0 ~100~400MeV/c PYTHIA/JETSET
41 Coalescence model
42 Source Spectrum dn dt T ε ρ h M GeV pc 1GeV GeV/cm g ρ ε h local density of halo dark matter ratio of the density of PBHs with M = M to i ρ h
43 Interstellar Spectrum Propagation by the Standard Leaky Box 1 λ esc I D QD =, λesc = λesc( R, β) 17g/cm 4πρ m c.f. τ esc λ ρβ c esc 7 = 3 10 yr 2 B/C ratio, C/O ratio
44 Solar Modulation Numerical calculation of the spherically symmetric model by Fisk. 1 V 2 2 r r 3 r E α ( 2 rs) = ( EU) Modulation parameter from proton spectrum 1997: φ = 500MV 1998: φ = 610MV 1999: φ = 648MV 2000: φ = 1344MV
45 Solar Activity Climax Neutron Monitor Solar Min. Solar Max.
46 PBH D
47 Local PBH R PBH T 1 dn dt d T 3.1 ε ρ M 10 pc yr GeV/cm g 95% C.L. (pc -3 yr -1 ) x10 0 sum x x x x h c.f. Upper limits on R PBH p ~10-2 TeV-GRB ~ Diffuse γ-ray ~10-1
48 PBH 95% C.L. 1 α dε ε M i =, α = dm M M dε ε Ωh Ω Ω = d PBH h dm i M 8 M i x10-6 sum 5 2 result c.f. Upper limits on Ω PBH p ~10-8 ~ -9 e + /e - ~10-9 Diffuse γ-ray ~10-8
49 Future Prospects BESS-Polar Tiger Antarctica Flight, 2001/2002
50 Future Prospects BESS-Polar AMS PAMELA GAPS
51 BESS-Polar D
52 BESS-Polar / PAMELA / AMS Sensitivity SΩεt BESS 3 yr 20 days 3 yr
53 BESS-Polar BESS-Polar
54 10 Ft. Sumner
55 BESS-TeV BESS-Polar
56
57
58 BESS-Polar
59 D 1.9 x 10-4 (m 2 s sr 2 GeV/n) -1 in GeV/n D BESS D D Local PBH PBH BESS-Polar
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