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1 Akira Yamamoto (KEK) and John W. Mitchell (NASA-GSFC) for the BESS Collaboration To be presented at SpacePart12, held at CERN, November 5-7, 2012 Search.

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Presentation on theme: "1 Akira Yamamoto (KEK) and John W. Mitchell (NASA-GSFC) for the BESS Collaboration To be presented at SpacePart12, held at CERN, November 5-7, 2012 Search."— Presentation transcript:

1 1 Akira Yamamoto (KEK) and John W. Mitchell (NASA-GSFC) for the BESS Collaboration To be presented at SpacePart12, held at CERN, November 5-7, 2012 Search for Primary Antiparticles and Cosmological Antimatter with BESS

2 2 BESS Collaboration The University of Tokyo High Energy Accelerator Research Organization(KEK) University of Maryland Kobe University Institute of Space and Astronautical Science/JAXA National Aeronautical and Space Administration Goddard Space Flight Center University of Denver BESS Collaboration Balloon-borne Experiment with a Superconducting Spectrometer A. Yamamoto, 6 November 2012 BESS Experiment

3 3 BESS Collaboration The University of Tokyo High Energy Accelerator Research Organization(KEK) University of Maryland Kobe University Institute of Space and Astronautical Science/JAXA National Aeronautical and Space Administration Goddard Space Flight Center University of Denver BESS Collaboration Balloon-borne Experiment with a Superconducting Spectrometer A. Yamamoto, 6 November 2012 BESS Experiment

4 4 Balloon-borne Experiment with a Superconducting Spectrometer BESS Objectives Balloon-borne Experiment with a Superconducting Spectrometer Search for Antiparticle/Antimatter Search for Antiparticle/Antimatter p, D Novel 、 primary cosmic origins p, D Novel 、 primary cosmic origins Evaporation of Primordial Black Holes (PBHs) Evaporation of Primordial Black Holes (PBHs) Annihilation of super-symmetric particles Annihilation of super-symmetric particles He Baryon asymmetry in Universe He Baryon asymmetry in Universe Provide Fundamental Cosmic-ray Data Provide Fundamental Cosmic-ray Data Precise p, He,  spectra Precise p, He,  spectra Propagation, solar modulation, Propagation, solar modulation, Atmospheric secondaries, Atmospheric secondaries, Atmospheric neutrinos Atmospheric neutrinos Light isotopes Light isotopes AntiGalaxy Galax y p p A. Yamamoto, 6 November 2012 BESS Experiment

5 Outline Introduction Introduction Cosmic-ray antiparticles BESS history and progress New results from BESS-Polar New results from BESS-Polar Low-energy Antiproton Measurement Antihelium Search Antidueteron Search in progress Proton flux and annual/daily variation during flight (not covered, in this talk) Summary Summary A. Yamamoto, 6 November 2012 5BESS Experiment

6 Cosmic-ray Antiparticles Provide Unique Information Provide Unique Information Elementary particle phenomena in the early universe Elementary particle phenomena in the early universe Matter/Antimatter asymmetry, Matter/Antimatter asymmetry, SUSY dark matter, SUSY dark matter, Primordial black hole (PBH), etc. Primordial black hole (PBH), etc. Fundamental Cosmic-ray data Fundamental Cosmic-ray data Production, propagation Production, propagation Solar modulation Solar modulation Interaction in the atmosphere Interaction in the atmosphere A. Yamamoto, 6 November 2012 6BESS Experiment

7 7 Possible Origin of Antiprotons Collision Origin (Secondary) Collision Origin (Secondary) Kinematically suppressed in low energy Kinematically suppressed in low energy Primary Origin Primary Origin Evaporation of primordial black holes (PBH) Evaporation of primordial black holes (PBH) Annihilation of SUSY DM Annihilation of SUSY DM Could be probed by spectral shape Could be probed by spectral shape 6 A. Yamamoto, 6 November 2012 BESS Experiment

8 Search for Antiparticle/Antimatter Novel Cosmic Origin A. Yamamoto, 6 November 2012 8 1979: p-bar first observation (Golden et al,, Bogomolov et al.) 1981: Anomalous excess (Buffington et al) 1985: ASTROMAG proposed 1987: LEAP, PBAR 1988: Astromag frozen 1991: MASS 1992: IMAX 1993: BESS, TS93 1994: CAPRICE, HEAT 1996: Solar minimum 1998: CAPRICE, AMS-01 2000/2:Heat-pbar 2004: BESS-Polar I 2006-present PAMELA (Polar-orbit) 2007: BESS-Polar II - Solar minimum 2011-present: AMS-02 (ISS) BESS Experiment

9 Search for Antiparticle/Antimatter Novel Cosmic Origin A. Yamamoto, 6 November 2012 9 1979: p-bar first observation (Golden et al,, Bogomolov et al.) 1981: Anomalous excess (Buffington et al) 1985: ASTROMAG proposed 1987: LEAP, PBAR 1988: Astromag frozen 1991: MASS 1992: IMAX 1993: BESS, TS93 1994: CAPRICE, HEAT 1996: Solar minimum 1998: CAPRICE, AMS-01 2000/2:Heat-pbar 2004: BESS-Polar I 2006-present PAMELA (Polar-orbit) 2007: BESS-Polar II - Solar minimum 2011-present: AMS-02 (ISS) BESS Experiment

10 Search for Antiparticle/Antimatter Novel Cosmic Origin A. Yamamoto, 6 November 2012 10 1979: p-bar first observation (Golden et al,, Bogomolov et al.) 1981: Anomalous excess (Buffington et al) 1985: ASTROMAG studied 1987: LEAP, PBAR 1988: Astromag frozen 1991: MASS 1992: IMAX 1993: TS93,BESS first flight 1994: CAPRICE, HEAT 1996: Solar minimum 1998: CAPRICE, AMS-01 2000/2: Heat-pbar 2004: BESS-Polar I 2006-present: PAMELA (Polar-orbit) 2007: BESS-Polar II Solar minimum 2011-present: AMS-02 (ISS) BESS: 1985Thin Solenoid conf. proposed U.Tokyo started preparation 1987:Collaboration formed 1993:First flight, p-bar mass identified 1995: Distinctive peak observed at 2 GeV 1998: Spectrum up to 4.2 GeV Precise p spectrum: ~ 120 GeV 2000: Charge dependence, p-bar/p 2001: Atmospheric p and p-bar, mu 2002: BESS-TeV: p spectrum: ~ 500 GeV 2004: BESS-Polar I 2007/8BESS-Polar II Consistent 11 flights successful BESS Experiment

11 Search for Antiparticle/Antimatter Novel Cosmic Origin A. Yamamoto, 6 November 2012 11 1979: p-bar first observation (Golden et al,, Bogomolov et al.) 1981: Anomalous excess (Buffington et al) 1985: ASTROMAG studied 1987: LEAP, PBAR 1988: Astromag frozen 1991: MASS 1992: IMAX 1993: BESS first flight 1994: CAPRICE, HEAT 1996: Solar minimum 1998: CARPRICE, AMS-01 2000/2: Heat-pbar 2004: BESS-Polar I 2006-present: PAMELA (Polar) 2007: BESS-Polar II Solar minimum 2011-present: AMS-02 (ISS) BESS: 1985Thin Solenoid conf. proposed U.Tokyo started preparation 1987:Collaboration formed 1993:First flight, p-bar mass identified 1995: Distinctive peak observed at 2 GeV 1998: Spectrum up to 4.2 GeV Precise p spectrum: ~ 120 GeV 2000: Charge dependence, p-bar/p 2001: Atmospheric p and p-bar, mu 2002: BESS-TeV: p spectrum: ~ 500 GeV 2004: BESS-Polar I 2007/8BESS-Polar II 11 flights successful BESS Experiment Courtesy: M. Casolino Consistent

12 BESS Ballooning 1993~2000, BESS, North Canada 2002, BESS-TeV 2001, BESS-TeV, Fort Sumner 2004, 2007 /08: BESS-Polar, Antarctica 1999, 2001, BESS-Ground, Japan 11 scientific balloon flights2004 A. Yamamoto, 6 November 2012 BESS Experiment 12

13 BESS Spectrometer: Concept Rigidity measurement SC Solenoid (L=~1m, B=~1T) SC Solenoid (L=~1m, B=~1T) Transparent Transparent Min. material (5 g/cm 2 ) Uniform field Uniform field Large acceptance Large acceptance Central tracker Central tracker Drift chamber Drift chamber Minimize scattering  ~150  m Z, m measurement Z, m measurement R,  --> m = ZeR 1/  2 -1 dE/dx --> Z JET/IDC Rigidity TOF , dE/dx √ 13

14 Transparent Superconducting Magnet BESS: Diameter: 1 m Coil thickness: 8 mm B: 1.0 T Al, NbTi/Cu 1.2 x 1.8 mm 2 r B ・ Strong magnetic field with thin coil ・ Persistent current A. Yamamoto, 6 November 2012 BESS Experiment14

15 Evolution of BESS Nine northern latitude flights (1+ days) 1993-2002 and two Antarctic flights in 2004 (8.5 days) and 2007 (24.5 days) Including BESS-Polar I and II: 11,643 antiprotons reported 0.2 - 4.2 GeV 2001, 2002 2004, 2007 p6, 243415, 398668, 5581471,512, 7,886 Maximizing advantages with balloon experiments

16 16 Antiproton Spectrum Measured at Solar Minimum in 1995 - 1997 Peak for Secondary Flatter in low energy? Primary Origin? More statistics necessary at solar minimum S. Orito et al. PRL, Vol. 84, No, 6, 2000 A. Yamamoto, 6 November 2012 BESS Experiment

17 17 Antiproton Spectrum Measured at Solar Minimum in 1995 - 1997 Peak for Secondary Flatter in low energy? Primary Origin? More statistics necessary at solar minimum S. Orito et al. PRL, Vol. 84, No, 6, 2000 A. Yamamoto, 6 November 2012 BESS Experiment

18 BESS-Polar Experiment - Very precise measurement at solar minimum at solar minimum - Antarctica Long duration flight at high latitude, at high latitude, low rigidity cut-off, low rigidity cut-off, - Large A  and transparent with a new high-resolution with a new high-resolution spectrometer A. Yamamoto, 6 November 2012 18 BESS Experiment

19 19 BESS-Polar Feature AMS02PAMELA (10+20 days) (3 years) BESS-Polar provides the best sensitivity in low energy 36 320-390 690 Altitude (km) 2007> 7525 days0.3 BESS-Polar II 2006<70.4>6 years0.0021 PAMELA 2011< 51.7TBD0.5 AMS LaunchLatitud e Flight TimeAcceptance (m 2 sr) A. Yamamoto, 6 November 2012BESS Experiment

20 20 BESS-Polar Spectrometer Minimizing Material in particle path Minimize material in spectrometer New detector (Middle TOF) Energy range extended down to 0.1 GeV Low power electronics Solar Power System, Longer life of LHe cryogen Long duration flight BESS-2000 BESS-Polar TOF Upper Coil JET/IDC ACC MTOF TOF Lower 18 g/cm 2 5 g/cm 2 10 g/cm2 A. Yamamoto, 6 November 2012 BESS Experiment

21 21 BESS-Polar ： Superconducting Magnet: much thinner and more transparent Support Cyl. A. Yamamoto, 6 November 2012 BESS Experiment

22 A Key: High-Strength Al stabilized Superconductor A Key: High-Strength Al stabilized Superconductor Micro alloying Al+Ni 0.5% Micro alloying Al+Ni 0.5% Cold-work hardening 15~20% Cold-work hardening 15~20% 22 BESSBESS–Polar 1.2 1.8 0.8  1.1 Structure Conductor A. Yamamoto, 6 November 2012 BESS Experiment

23 23 LHC: ATLAS Central Solenoid using the same technology Solenoid

24 Large acceptance Large acceptance Uniform B field ~0.8Tesla Uniform B field ~0.8Tesla Cylindrical coaxial layout Cylindrical coaxial layout 0.3 m 2 sr 0.3 m 2 sr Transparency for low E particles Transparency for low E particles Thin solenoid 0.1 X 0 /wall Thin solenoid 0.1 X 0 /wall Precise momentum measurement Precise momentum measurement Central Tracker σ=100 ~150um 52 points Central Tracker σ=100 ~150um 52 points MDR ~ 270 GV MDR ~ 270 GV Redundant Particle ID Redundant Particle ID dE/dX (JET, TOF, MTOF) dE/dX (JET, TOF, MTOF) TOF, ACC TOF, ACC BESS Polar II Spectrometer TOF MTOF ACC 24 A. Yamamoto, 6 November 2012 BESS Experiment

25 BESS-Polar II - Launch - A. Yamamoto, 6 November 2012 25BESS Experiment

26 Launch dateDec. 23, 2007 Observation time24.5 days Cosmic-ray observed4.7 G events Data size13.5 Tb Flight altitude ~36 km (6~5g/cm 2 ) Data recovery Detector recovery Feb. 3, 2008 Jan. 16, 2010 BESS-Polar II Flight summary 26 BESS-Polar II flight realized at solar minimum A. Yamamoto, 12-06-14 BESS Experiment

27 BESS Recovered from Antarctica in 2010 27 Ski-way building team Payload recovery team 33 Magnet performance fully resumed. Magnet performance fully resumed. It may fly again, and ready for a new science proposal, with next generation, … It may fly again, and ready for a new science proposal, with next generation, … BESS Experiment A. Yamamoto, 6 November 2012

28 Particle Identification in BESS-Polar II w/o ACC Veto A. Yamamoto, 6 November 2012 28BESS Experiment

29 Particle Identification in BESS-Polar II A. Yamamoto, 12-11-06 29BESS Experiment

30 30 BESS-Polar II Antiproton Spectrum Compared with BESS’95+’97: x 14 statistics at < 1 GeV x 14 statistics at < 1 GeV Flux peak consistent at 2 GeV, Flux peak consistent at 2 GeV, Spectral shape different at low energies. Spectral shape different at low energies. Result published: Result published: Ref. for BESS’95+’97: S. Orito et al. PRL, Vol. 84, No, 6, 2000 A. Yamamoto, 6 November 2012 BESS Experiment

31 31 Comparison with secondary models Secondary p-bar flux calculated using: Propagation model × Solar modulation BESS-Polar II results - generally consistent with secondary p-bar calculations under solar minimum conditions. A. Yamamoto, 6 November 2012 BESS Experiment Phys. Rev. Lett., 108, 051102 (2012)

32 Comparison of Spectral Shapes Favored Models no low energy enhancement no low energy enhancement A. Yamamoto, 6 November 2012 32 IDModelC 2 (<1.0GeV) 1Mitsui (600MV) 0.57 2Bieber0.56 3Bergstrom1.24 4Donato1.59 5Galprop (PD) 0.63 The shaded band indicates the small variation that results from uncertainty in the modulation parameter. BESS Experiment Calculations normalized near peak Phys. Rev. Lett., 108, 051102 (2012)

33 Evaluation of PBH Antiproton PBH antiproton evaluated by: {p-bar flux observed} - {Secondary flux*} *calculated by using Mitsui: SLB+Fisk model, PBH evaporation rate, R : BESS’95+’97: 4.2 x 10 -3 /pc 3 /yr BESS-Polar II: 5.2 x 10 -4 /pc 3 /yr Upper limit (90% C.L.): 1.2 x 10 -3 /pc 3 /yr No evidence of primary p from PBH evaporation A. Yamamoto, 6 November 2012 33 Phys. Rev. Lett., 108, 051102 (2012). BESS Experiment

34 32nd International Cosmic Ray Conference, Beijing 2011 Anti-He Search Particle Identification using the TOF information No antihelium candidate was found between -14 and -1 GV after all selection among 4 x 10 7 Helium events. The figure below shows remaining events after all selections applied. TOF-β selection |Z| = 2 selection Upper TOF |Z| = 2 selection Lower TOF After all selection No He candidate -14GV A. Yamamoto, 12-06-14 34BESS Experiment

35 Search for Antihelium: in Previous Flights BESS-Polar I results: He-bar/He Upper limit: 4.4 x 10 -7 X 1/100 Survival probability in the residual air for He (He) Single track efficiency for He (He) Selection efficiency for He (He) x 1/10 x 1/ 20 A. Yamamoto, 12-06-14 35BESS Experiment

36 Search for Anti-He: BESS & BESS-Polar BESS-Polar I: Upper limit: 4.4 x 10 -7. BESS-Polar II Upper limit: 9.4 x 10 -8 All-BESS results combined: Upper limit: 6.9x 10 -8 (1x10 -7 w/o spectrum assumption) This limit is improved by three orders of magnitude over first reported limits X 1/100 x 1/10 A. Yamamoto, 12-06-14 36 PRL 108, 131301 (2012)

37 37 BESS has accomplished many of the Scientific Objectives expected from ASTROMAG in 1980s Balloon Experiments are a very useful approach for Astroparticle physics

38 38 BESS has accomplished many of the Scientific Objectives expected from ASTROMAG in 1980s and they are extended to AMS Balloon Experiments are a very useful approach for Astro-particle physics AMS

39 Search for Antideuteron Large Exposure and Superior PID Essential: Capable detectors: - BESS-Polar - GAPS - AMS Secondary antideuteron: Secondary antideuteron: strongly suppressed due to strict kinematical constraint. strongly suppressed due to strict kinematical constraint. Separation from antiproton: Separation from antiproton: essentially important, and essentially important, and antiprotons would be a background. antiprotons would be a background. Model calculations for decay of supersymmetric particles

40 Further Data Analysis in progress Further Data Analysis in progress BESS-Polar I BESS-Polar II Improvement of JET (Central Tracker) dE/dx BESS-Polar II p, p-bar / p ratio, and d-bar analysis, in progress p He d t Further calibration achieved!

41 Summary BESS-Polar II at Solar Minimum: BESS-Polar II at Solar Minimum: Gathered cosmic-ray data with >the previous solar minimum (’95 + ’97). Gathered cosmic-ray data with >10 times statistics to the previous solar minimum (’95 + ’97). Antiproton spectrum observed is Antiproton spectrum observed is consistent with secondary antiproton calculations. Result shows, Result shows no evidence of primary antiprotons, An evaporation rate, upper limit set: An evaporation rate, upper limit set: 1.2 x 10 -3 /pc 3 /yr (90% C.L.). All BESS (1993 ~ 2007/8): All BESS (1993 ~ 2007/8): Indicates no antihelium candidate, and Indicates no antihelium candidate, and S6.9x 10 -8, and Sets He-bar/He upper limit 6.9x 10 -8, and 1x10 -7 (with no spectrum assumption). BESS Polar I and II (in analysis): BESS Polar I and II (in analysis): Proton flux and the annual/daily time-variation. Proton flux and the annual/daily time-variation. Anti-deuteron search and Light-isotopes. Anti-deuteron search and Light-isotopes. 41

42 42 Acknowledgements Our sincere thanks to: NASA-Headquarters, NASA-Headquarters, NASA-Balloon Project Office and Columbia Scientific Balloon Facility, NASA-Balloon Project Office and Columbia Scientific Balloon Facility, National Science Foundation and Raytheon Polar Services Company, National Science Foundation and Raytheon Polar Services Company, NASA-GSFC, ISAS-JAXA, KEK, U- TOKYO/RESCEU, NASA-GSFC, ISAS-JAXA, KEK, U- TOKYO/RESCEU, All BESS collaborators All BESS collaborators Special thanks to all PhD students (24 PhDs since 1993) for their hardest effort to bring BESS to science frontier. Special thanks to all PhD students (24 PhDs since 1993) for their hardest effort to bring BESS to science frontier. A. Yamamoto, 12-11-06 BESS Experiment

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