306 [7] GeV TeV PAMELA 100 GeV PAMELA AMS GeV [8] TeV [9] PAMELA[10] AMS BESS-Polar 95 [11]AMS 1.3 AMS AMS rigidity TOFTime Of Flight TRDE
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- ひろき うるしはた
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1 305 Alpha Magnetic Spectrometer (AMS) AMS 1.1 AMS AMS LEP L3 LEP GeV TeV AMS ISS ISS BESS [2] HEAT[3] AMS PAMELA [4] Fermi [5] 10 GeV 100 GeV AMS 10 8 ev ev AMS GeV TeV Golden [1]1990 PAMELAFermi [5] [6]
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2 306 [7] GeV TeV PAMELA 100 GeV PAMELA AMS GeV [8] TeV [9] PAMELA[10] AMS BESS-Polar 95 [11]AMS 1.3 AMS AMS rigidity TOFTime Of Flight TRDEcal RICH AMS Rigidity
3 307 AMS 1 m 1.1 m 64 Nd-Fe-B 1.4 ISS 100 GeV/c 90% 3, TOF TOF [14] PMT 160 4% 50 1% Rigidity AMS LEP L3 2, cm [12] TRD TRD [13] 0.06 g/cm 3 /Xe:CO280%:20% 6 mm 2 m 5,248 X Xe 49 kgco2 5 kg TRD RICH RICH [15] 1.33 NaF cm 10,880 PMT RICH Ecal Ecal PMT PMT 0.1% Ecal Ecal [16] mm mm 11 1 mm 10 90% 10, AMS Ecal veto ISS AMS
4 308 Ecal GeV 1 TeV Fermi Magic/HESS AMS-01 AMS 1994 [17] AMS AMS AMS-02 2 TOF STS /B/C [18] 2.2 AMS AMS 6.3 Gr.m.s. 1/2 1 krad/ ISS EM QM QM QM1 QM2 QM1QM2 FMFS FM FS QM GSI XeAuU AMS CERN AMS AMS CERN Ecal
5 ISS NASA AMS ESTEC ISS AMS ISS ISS ISS B AMS % 1/5 8 [19] AMS CERN TRD Ecal RICH L=1 m L=3 m L 2 rigidity rigidity ISS AMS 900 AMS 3 2 CERN 400 GeV/c rigidity
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6 310 CERN 400 GeV/c % rigiditymaximum Detectable Rigidity, MDR 2TV [20] AMS CERN AMS C-5 C-5 AMS 4 1 AMS 2.7 AMS ISS 2010 ISS AMS ISS AMS 4 C-5 AMS C-5AMS SSPF ISS AMS MDR 2TV AMS STS ,000 1, AMS 7.5 ISS 3 AMS
7 311 5 ISS AMS AMS 1 ADC TOFISS 2 7 ISS TDRS TDRS ISS AMS 2 1/3,500 DSPDigital Signal Processor CERN POCCPayload Operation Control Center ISS DSP 300 DSP 6 AMS DSP 3.3 ISS ISS AMS ISS 0 ISS ISS AMS ISS ISS AMS ISS AMS HTV ISS AMS
8 ISS 30 Rigidity TOF PMT TRD RICH Ecal PMT GeV 2 TRDEcal TRD Ecal BDTBoosted Decision Trees 100 GeV 90% TRD 1/3,000Ecal 1/10,000 MDR rigidity Ecal 100 GeV 1 % GeV 350 GeV GeV 350 GeV 1,100 % [21] 3.6 /B/C 5 2 AMS 4 AMS GeV 20 TeV AMS [1] R. L. Golden et al, Phys. Rev. Lett. 43, 1196 (1979). [2] K. Yoshimura et al., Phys. Rev. Lett. 75, 3792 (1995); S. Orito et al., Phys. Rev. Lett. 84, 1078 (2000); K. Abe et al., Phys. Rev. Lett. 108, (2012) [3] J. J. Beatty et al., Phys. Rev. Lett. 93, (2004). [4] O. Adriani et al., Nature 458, 607 (2009); O. Adriani et al., Astropart. Phys. 34, 1 (2010). [5] M. Ackermann et al., Phys. Rev. Lett. 108, (2012). [6] K. Norita et al., Astrophys. J. 710, 958 (2010) [7] J. Hisano et al., Phys. Rev. D 79, (2009) [8] T. Sanuki et al., Astrophys. J. 545, 1135 (2000); S. Haino et al. Phys. Lett. B 594, 35 (2004) [9] K. Asakimori et al., Astrophys. J. 502, 278 (1998); M. Hareyama et al., J. Phys. Conf. Ser. 31, 159 (2006)
9 313 [10] O. Adriani et al., Science 332, 69 (2011). [11] K. Abe et al., Phys. Rev. Lett. 108, (2012). [12] B. Alpat et al., Nucl. Instr. and Meth. A 613, 207 (2010). [13] Ph. Doetinchem et al., Nucl. Instr. and Meth. A 558, 526 (2006). [14] V. Bindi et al., Nucl. Instr. and Meth. A 623, 968 (2010). [15] J. Casaus et al., Nucl. Phys. B (Proc. Suppl.) 113, 147 (2002). [16] F. Cadoux et al., Nucl. Phys. B (Proc. Suppl.) 113, 159 (2002). [17] S. Ahlen et al., Nucl. Instr. and Meth. A 350, 351 (1994). [18] M. Aguilar et al., Phys. Rep. 366/6, 331 (2002); M. Aguilar et al., Astrophys. J. 746, 105 (2011). [19] K. Lubelsmeyer et al., Nucl. Instr. and Meth. A 654, 639 (2011). [20] S. Haino et al., Nucl. Instr. and Meth. A 699, 221 (2013). [21] AMS collaboration, M. Aguilar et al., to be submitted (2013).
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