BESS BESS-Polar BESS-Polar II
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1 BESS
2 BESS BESS-Polar BESS-Polar II
3
4 1912 V.F. (Victor Franz Hess) 1936
5 HESS 17,500 (1912)
6 1912 Dirac
7 10 14 ev ev
8 3K
9 γ 30
10 ?
11 He He n p n p
12 + + ) + e / ( e Positron fraction e Grajek et al., astro ph Hooper and Profumo, Phys. Reports 453, 29 (2007) Shaviv, Nakar and Piran, astro ph Yuksel et al., astro ph v Moskalenko and Strong, ApJ 493, 694 (1998) PAMELA TS γ: Galactic centre ~kpc AMS HEAT Energy [GeV]
13
14 Standard Leaky box model or Diffusion box model) Diffusive reacceleration inelastic scattering Tertiary Interaction)
15 Tan and Ng, Stephens 12 ~400 GeV Differential Cross Section d /de p _ (mb/gev) Tan and Ng Stephens 10 GeV 30 GeV E p =300 GeV 100 GeV p _ Kinetic Energy (GeV)
16 0.3 Leaky Box Model (SLB) Diffusion Model 0.2 λesc B/C) B/C Flux Ratio HEAO-3 Standard Leaky Box Model Garcia-Munoz et al. =700 MV =600 MV (>0.2 GeV/n) =490 MV (<0.4 GeV/n) (a) Diffusive Reaccelaration (DR) Kinetic Energy (GeV/n)
17 Tertiary Interaction Intersteller Flux
18 10 1 Force-field Fisk 22 p _ Flux (m 2 sr 1 s 1 GeV 1 ) primary+secondary primary+secondary Solar Min Secondary Solar Max Kinetic Energy (GeV) secondary
19 (PBH) 1015 g PBH
20 PBH BESS, BESS-Polar II BESS 93 R=1.7x10-2 (pc -3 y -1 ) Ωpbh< 6 x 10-9 h -2 PBH Antiproton Flux (m -2 sr -1 sec -1 GeV -1 ) BESS-Polar II Simulation for secondary only (20 days) Simulation for secondary +PBH (20 days) BESS95+97 real data BESS PBH BESS Polar Secondary Kinetic Energy (GeV)
21 γ PBH 100 MeV Diffuse γ Ωpbh< 5.1 x 10-9 h -2 γ γ R<5x108 pc -3 y -1 Hagedorn R<5x10-2 pc -3 y -1 PBH
22 1955 Aizu et al. Aizu et al Golden et al Golden et al. Bogolomov et al.
23 Buffington 1981 Buffington, Schindler and Pennypacker, ApJ 248 (1981) 1179
24 Buffington 1981 Buffington, Schindler and Pennypacker, ApJ 248 (1981) 1179
25 Buffington 1981 Buffington, Schindler and Pennypacker, ApJ 248 (1981) GeV Photino? Stecker et al. PRL
26 ~1990 Buffington 1981 Buffington, Schindler and Pennypacker, ApJ 248 (1981) GeV Photino? Stecker et al. PRL
27 ASTROMAG 1985~ ISS Spin off Isotopes SMILI MASS IMAX BESS CAPRICE ISOMAX Antimatter LEAP PBAR MASS IMAX BESS CAPRICE HEAT
28 BESS Astromag Workshop 1987 Collaboration
29 BESS
30 Low Energy Cosmic-ray Spectra Precisely Measured by BESS Rigidity Measurement BESS Precise spectra proton (0.2~500 GeV) helium (0.2~250 GeV/n) antiproton (0.2~ 4 GeV) AMS ATIC TRACER CREAM Particle Astrophysics ANITA Anchor the spectrum in the lowest energy region. EUSO? OWL? 27
31 Low Energy Cosmic-ray Spectra Precisely Measured by BESS Rigidity Measurement Precise spectra proton (0.2~500 GeV) helium (0.2~250 GeV/n) antiproton (0.2~ 4 GeV) Anchor the spectrum in the lowest energy region. 27
32 BESS Balloon-borne Experiment with a Superconducting Spectrometer 1000g/cm 2 37km, 1/200 28
33 Boomerang => WMAP <=>
34 BESS Buffington Golden Golden et al, 1979 First observation Gas cherenkov VETO Buffington et al, 1982 Low energy excess Annihilation topology Their results stimulated theoretical conjectures
35 BESS
36 (+) (-) m 2 = R 2 e 2 Z 2 ( β 2 1)
37 BESS (III) Comparison between CAPRICE and BESS 33
38 L ± B MDR=200 GV
39 JET/IDC Development for BESS-TeV & -Polar Spatial resolution
40
41 BESS 37
42 ~2002 9
43
44
45
46
47
48 ~ β -1 vs. Rigidity σ TOF 300 ps 100 ps 70 ps N obs ~650/year E p 0.18~0.5 GeV 0.18~1.5 GeV 0.18~4.2 GeV First mass ID New TOF Cherenkov veto
49 45
50 BESS
51 BESS
52 1~2 GeV OK 1 GeV? 1 48
53 Limit on parameter for SUSY DM BESS data has limited parameter space for SUSY. Bottino, Donato, Fornego, Salati 1998 Bergstrom, Edsjo, Ullio 1999 Bergstrom, Edjo, Ullio
54 Indirect search for Dark matter Low energy window is now filing Secondary background is larger at low energies than we expected Bergstrom, Edjo, Ullio, Gaisser et al., 1999 Room for primary component? Higher energy (>10 GeV) Bump? Ullio, 1999 Bergstrom, Edjo, Ullio 1999 Outside the heliosphere to avoid solar modulation Wells, Moiseev, Ormes 1998 Precise measurement and calculation
55 PBH (BESS95 ) R < pc -3 yr -1 (90%C.L) K. Maki, et al. PRL 76 (1996)
56 2 He/He < (1~14GV) 52
57 1 (PBH, SUSY ) 1 53
58 K.Mori et al, ApJ 566 (2002)
59 pbar/p ratio 1993~
60 56
61 p-bar/p ratio Maeno et al. AP 16 (2001) 121 Asaoka et al. PRL 88 (2002) phase - phase E k = 0.7 GeV BESS- Polar p/p ratio: Haino et al. ICRC
62 1 ( ) 1~100GeV 5% BESS/AMS 58
63 BESS-TeV (2001~2002) Super KAMIOKANDE TeV 1 ~1.4 TV 100% 59
64 500GeV BESS-98, AMS-I 100 GeV ATIC 100GeV 60
65 5 p π K p (93~02) (01) 5 g/cm 2 ~1 d/yr 5~30 ~10 hr 740 ν 1000 µ p ν µ p e (99) (95~02) (99~02) 740 ~ 3 days 1000 ~ 3 days 5~1000 ~3 hr/yr (g/cm 2 ) 61
66 µ (5~26 g/cm 2 ) BESS-2001 Hadronic interaction model hr
67 KEK µ 63
68 (~1990) 64
69 (1998: Bess-98, AMS-I, Caprice) Error: < +/ GeV Sanuki et al. ApJ. 545 (2000)
70 (BESS-TeV) Error: < +/ GeV Haino et al. PLB 594 (2004) 35 66
71 BESS-TeV F = φ E k -γ Proton (E k > 30 GeV) φ = (1.37 ± 0.12)x10 4 γ = ± Helium (E k > 20 GeV) φ = (7.06 ± 1.15)x
72 68
73 BESS ( ) (M Events) (GeV) 0.18~ ~ ~ ~4.2 He/He
74 70
75 10 - Pbar flux [m -2 sr -1 sec -1 GeV -1 ] 10 - BESS(95+97) BESS(93) IMA CAPRICE Kinetic Energy 71
76 BESS-Polar 72
77 BESS Polar 2006~2007 Assume PBH evapolation rate R = pc -3 yr -1 10~20 73
78 BESS-Polar BESS-2000 BESS-Polar TOF Upper 18g/cm 2 Coil 5g/cm 2 JET/IDC 10g/cm 2 MTOF ACC Incident Particles TOF Lower (Middle TOF) 0.1 GeV 74
79 BESS Polar (III) 75
80 (I) ( Coil: 1 g/cm 2, Total: 2 g/cm 2 ) 0.85 Tesla 5 G 76
81 Micro alloying Al+Ni 0.5% Cold-work hardening 15% Structure Conductor BESS BESS Polar
82 (II)
83 20 900W ( ) < 300 kg ( ) 79
84 NASA/GSFC 2003 Oct Aug Upper TOF JET/IDC & MTOF Aerogel Cherenkov Counter Integration complete!
85 with NSBF 2004 Aug NSBF
86 BESS-Polar Campaign 2004 Oct Williams Fields Dec 3 with NASA/NSBF Dec 13! McMurdo Station & Williams Fields 2005 Jan 4 BESS-Polar 2004
87 USA McMurdo Station Crary Lab. Airport Church
88 Williams Field BESS-Polar Weatherport SIP Pig Barn Weatherport
89
90
91 10 ( Wind map of flight day
92 ( )
93 Williams Field, McMurdo, in Antarctica, (S77-51, E ), 5:56(UTC), Dec. 13, 2004
94 1 RS-232C(19.2 kbps) 2 RS-232C(1200 bps) 28 Digital O.C. output 1 Timed-gate O.C. output 32 Analog input 16 Digital input LOS Payload TDRSS TDRSS TDRSS Internet Event data ROCC (McMurdo) POCC (Palestine) White Sands (New Mexico) Link TDRSS Iridium LOS Uplink Scheduled Backup Downlink 6 kbps 255 bytes / 15 min kbps
95 Float Termination Flight 8.5days
96 170km Siple Dome 8 0km Williams Field Impacted the ground at (S-83-06, W ), at 22:56(UTC), Dec. 21
97 (1)
98 (2),,
99 Limit by MTOF Trigger Antiproton event RGT -0.4GV 1/β 2.47 Limit by BTOF Trigger Kinetic Energy 0.11GeV TOA) 95
100 BESS-Polar I BESS (95+97) (550 MV.) BESS-Polar I (851 MV
101 PAMELA PAMELA 1~5 GeV BESS-Polar I
102 / BESS
103 BESS-Polar II 2007~
104 BESS-Polar II - Cross section - BESS-Polar II BESS-Polar I 100
105 BESS-Polar II (BESS-Polar I) (BESS-Polar II) ~ 11 days > 22 days ~ 10 days > 20 days TOF-PMT Rejection ~ 630 >> stage 900 W 3 stage 675 W 0.2 m2sr 0.3 m2sr 8.5 days > 20 days 4 x BESS97 2 of 3.6 TB (recorded) 20 x BESS97 12 ~ 16 TB 101
106 Detector Improvement BESS-Polar I BESS-Polar II Longer life (10 days >20 days) New magnet with new cryostat Larger tank, third radiation shield Increase gas bottle for chamber gas Detector improvement TOF PMT HV leak ACC rejection MTOF will be read from both end Fast DAQ system Maintain weight balance Solar panel will be compactified fit in the new staging area optimize mechanical structure
107 BESS-Polar II - Launch Dec 23, 2007-
108 BESS-Polar II Flight Positive Event Launch 12/22/07 17:30 UTC Science Termination 1/16/08 2:00 UTC Negative Event Magnet-on at float - 24 days 10 hours Average altitude ~36 km (118,000 ft) Latitude South
109 End of BESS-Polar II Flight Flight termination January 20, 2008 ~30 days Location S, W On West Antarctic ice sheet nm from Patriot Hills Camp, 185 nm from AGO-2, 357 nm from South Pole Data successfully recovered February 3, 2008!
110 End of BESS-Polar II Flight Flight termination January 20, 2008 ~30 days Location S, W On West Antarctic ice sheet nm from Patriot Hills Camp, 185 nm from AGO-2, 357 nm from South Pole Data successfully recovered February 3, 2008!
111 BESS-Polar II Flight summary BESS-Polar I BESS-Polar II Total Float Time 8.5 days 29.5 days Observation TIme 8.5 days 24.5 days Recorded Event 900 M 4700 M Recorded Data Size 2.1 TB 13.5 TB Trigger Rate 1.4 khz 2.4 ~ 2.6 khz Live Time Fraction Altitude 37 ~ 39 km 34 ~ 38 km Air Pressure 4 ~ 5 g/cm2 4.5 ~ 8 g/cm2
112 BESS-Polar II Performance BESS-Polar II Preliminary BESS Polar-I 2004 BESS Polar-II 2007 Spectrometer - <130 µm resolution, MDR GV Outer TOF ps Middle TOF ps Aerogel Cherenkov pe, 6800 background rejection factor Data Acquisition khz event rate, no onboard event selection, 82% live
113 BESS-Polar II BESS-Polar I BESS Polar II Preliminary > 8000 Antiproton candidates
114 BESS-Polar II BESS-Polar II Simulation BESS-Polar I Antiproton Flux (m -2 sr -1 sec -1 GeV -1 ) Simulation for secondary only (20 days) Simulation for secondary +PBH (20 days) BESS95+97 real data BESS PBH BESS Polar Secondary Kinetic Energy (GeV)
115 WMAP 23 % CDM SUSY Kaluza-Klein
116 γ Diffuse γ Fermi /
117 EGRET Diffuse γ
118 PAMELA 1TeV WIMP Boost factor TeV WIMP (" "! W HEAT - W Background ) AMS 98 Background + Signal ) PAMELA 08 + / ( e e + + e B = Energy [GeV] 2 10 FIG. 3: Donato et al. The fiducial case of a 1 TeV LSP annihilating into a W + W pair is featured. In the left panel, the positron signal
119 BESS-Polar II Tertiary
120 BESS-Polar II Tertiary Donato et al. Phys.Rev.D78:043506,2008
121 - Antinucleus flux [GeV m s sr ] GAPS LDB GAPS ULDB AMS-02 BESS BESS BESS 95 IMAX 92 CAPRICE 94 CAPRICE 98 Antinucleus flux [GeV -1 m -2 s -1 sr -1 ] GAPS LDB GAPS ULDB AMS-02 BESS BESS BESS 95 IMAX 92 CAPRICE 94 CAPRICE ! F = 500 MV T [GeV/n] 10-10! F = 500 MV T [GeV/n] 10 0 Ibarra et al. arxiv: r -1 ] BESS BESS 95 IMAX 92 CAPRICE 94 CAPRICE 98
122 HEAT, PAMELA AMS II BESS-Polar II AMS II GAPS
123 BESS-Polar AMS, PAMELA AMS-02 PAMELA BESS-Polar II is the most sensitive balloon-borne magnetic rigidity spectrometer to ~4 GeV Higher sensitivity than PAMELA (3 yrs shown) Exceeds AMS-02 at low energy due to orbit Acceptance (m 2 sr) Flight Time Latitude Altitude (km) Launch AMS years < ~500 ~2010 PAMELA years < BESS-Polar II days >
124 PAMELA, BESS-Polar I BESS-Polar II AMS II BESS-Polar II
125 Backup
126 Comment of e+/e- detection possibility BESS-Polar AMS-01 BESS-Polar and AMS-01 have no detector for e/m separation except Aerogel Cherenkov Counter (up to only a few GeV).
127 e+/e- detection of AMS-01 AMS-01 has demonstrated positron detection with 3-track events by blemsstrahlung+ conversion pair up to 50 GeV. [PLB 646(2007) 145] In priciple BESS-Polar can separate e+/e- from m/p backgrounds with the same method.
128 3 track event in Polar-I data Low energy region : e/m separation with Aerogel Cherenkov Counter(ACC) High energy region : e+- pair creation from brems " Pre-selection UL Number of long track N longtk >= 1 Expected hits in JET N expect >= 32 X hit position in TOF Z hit position in TOF X TKU,L < 75mm Z TKU,L < 450mm Hits in UTOF N UTOF = 1 Hits in LTOF N LTOF >= 1 Zenith angle cos! zenith > 0.9 Event with 3-track by S.Haino Estimation of atmospheric secondaries is very Important. To select the event observed in same residual atmosphere, zenith angle cut is performed.
129 Expected Positron events with Polar-2 Acceptance estimated by Polar1 MC PAMELA positron fraction (as Reference) BESS : Electron BESS : Positron PAMELA : design value Expected positron events with Polar-2 (1.6x10 6 sec live time) 28-42GeV : ~60 events GeV (Flux ~ 3x10-3 [m 2 sr sec GeV] -1 ) : ~160 events GeV (Flux ~ 2x10-4 [m 2 sr sec GeV] -1 ) : ~40 events
130 AMS-01 Flew on Shuttle-91 in June 1998 Antihelium/helium limit in rigidity range GV/c: 1.1 x 10-6 Aguilar et al., Phys. Reports. 366 (2002) 331
131 AMS-02
132 STS 134? 125
133 Anticoncidence system Multiple particles rejection PAMELA DETECTOR TOF ANTI Time-of-flight Level 1 trigger particle identification (up to 1GeV/c) de/dx Plastic scintillator + PMT Anticoincidence system Defines tracker acceptance Plastic scintillator + PMT ANTI TRK Time Resolution ~ 70 ps Si Tracker + magnet Permanent magnet B=0.4T 6 planes double sided Si strips 300 µm thick Si-W Calorimeter Spatial risolution ~3µm Imaging Calorimeter : reconstructs shower profile discriminating e + /p and p/e - at level of 10-4 ~ 10-5 Energy Resolution for e ± ΔE/E = 15% / E 1/2. Si-X / W / Si-Y structure 22 W planes CALO S4 ND MDR = 740 GV/c S4 and Neutron detectors Extend the energy range for primary protons and electrons up to 10 TeV Plastic Scintillator 36 3 He counters in a polyetilen moderator 16.3 X 0 / 0.6 l 0
134 Past, present and future experiment MASS-89, 91, TS-93, CAPRICE NINA-2 PAMELA SIRAD NINA-1 9 M 91 TS 93 C 94 C 97 C 98 PAMELA LAZIO-SIRAD NINA-1 NINA-2 SILEYE-1 SILEYE-2 SILEYE-3 ALTEA SILEYE-1 SILEYE-2 SILEYE-3/ ALTEINO: LAZIO-SIRAD SILEYE-4/ ALTEA
135 PAMELA flight model before delivery to Samara, March 2005 PAMELA launched into orbit June 15, 2006 from Baikonur, rides on a Russian Resurs satellite. 71 degree near-polar elliptic orbit, 300 to 600 km. Expected minimum 3 years lifetime. Normal Operation, taking data.
136 Flight data: 92 GeV/c positron
137 Flight data 84 GeV/c interacting antiproton
138 Current status of Antiproton-Proton Ratio Donato 2001 (D, φ=500mv) Simon 1998 (LBM, φ=500mv) Ptuskin 2006 (PD, φ=550mv) PAMELA IMAX 1992 BESS 2000 HEAT-pbar 2000 CAPRICE 1998 CAPRICE 1994 BESS-polar 2004 MASS 1991 BESS BESS 1999 PAMELA p/p 0.2 p/p kinetic energy (GeV) kinetic energy (GeV) 2 10
139 Pamela Positrons Till August 30 th about positrons from 200 MeV up to 200 GeV have been analyzed More than positrons over 1 GeV Other eight months data to be analyzed )) - )+ φ(e + ) / (φ(e Positron fraction φ(e Muller & Tang 1987 MASS 1989 TS93 HEAT94+95 CAPRICE94 AMS98 HEAT00 Clem & Evenson 2007 PAMELA Energy (GeV)
140 Supersymmetric neutralino cannot explain the data. (Majorana particle) no hard positrons directly (helicity suppression of light fermions in the annihilation process) Better a Dirac particle, or a spin-1 particle like Kaluza-Klein dark matter Photons radiated from charged virtual particles ( virtual internal bremsstrahlung (IB), or direct emission) can have a significant impact on the resulting gamma-ray spectrum, leading not only to an even more pronounced cutoff, but also to clearly observable bump-like features at slightly lower energies very large boost factors are needed. a strong enhancement can also be expected in the gamma-ray flux at photon energies close to m_neutral arxiv: v1
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