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利用 ARGO-YBJ 的月亮阴影数据对能标的讨论

利用 ARGO-YBJ 的月亮阴影数据对能标的讨论. 查 敏 中科院高能物理研究所. Motivation: constructing an energy “anchor”. normalization and absolute energy calibration and reference for indirect measurements. Important progress on elemental CR energy spectrum from satellite/balloon-born experiments. ISS-CREAM.

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利用 ARGO-YBJ 的月亮阴影数据对能标的讨论

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  1. 利用ARGO-YBJ的月亮阴影数据对能标的讨论 查敏 中科院高能物理研究所

  2. Motivation: constructing an energy “anchor” normalization and absolute energy calibration and reference for indirect measurements Important progress on elemental CR energy spectrum from satellite/balloon-born experiments

  3. ISS-CREAM ISS-CREAM is planned for launch in 2014

  4. Direct experiment: CREAM example Few TeV region  few 100 TeV (MC )

  5. first suggestion by Clark 1957 Deficit of CR as looking at the moon Size of the deficit --> actual angular resolution Positon of the deficit  pointing error Displacement of moon shadow  energy calibration ( size.vs. E)

  6. Selected MOON data Using moon shadow East-West displacement to calibration Erec: The relation between Erec and Nstrip 利用地磁场的磁谱仪的作用，再加上ARGO高海拔、低阈能得特点，挑选阴影数据通过对宇宙线轻成分在低能端能谱的测量，建立“能标”。

  7. Summary of notable experiments 82 MAGIC

  8. Energy calibrtion • Two systematic uncertainties may affect the Multiplicity-Energy relation: • the assumed primary CR chemical composition (7%) • the uncertainties of different hadronic models (6%) 55 s.d. The energy scale error is estimated to be smaller than 13% in the energy range 1 – 30 (TeV/Z). ARGO coll., Phys.Rev. D 84 (2011) 022003 / ARGO coll., Phys.Rev. D 85 (2012) 022002

  9. From Menjo Hiroaki ICRC2013 (LHCf coll.)

  10. Geomagnetic field International Geomagnetic Reference Field (IGRF) coefficients by IAGA

  11. ARGO-YBJ Detector Low energy with digital signal High energy with analog readout • Trigger: 20 pads • Rate ~3.5 kHz • Dead time 4% • First data in July 2006 • Stop operation in February 2013

  12. High altitude location ( 4300 m + 606g/cm2) Full coverage with RPC (92% covering factor)

  13. analysis details • Shower production • Zenith angle range: 0-40° • Moon shadow statistics. Vs. shower attenuation effect • Moon shadow statistics • Data Selection • Add more inclined showers • detailed shower information 1 month moon shadow -9 sigma; Theta< 30 deg + |xc|<31 + |yc|<31 + Ns>300

  14. --continued <R> < 22 m Non-light contamination ratio: 4-6% Proton showers  steeper and narrower lateral distribution

  15. --continued • Moon shadow analysis • Direct Integration method • 0-35 °light data • LGRFmodel • Shower production • CORSIKA package • Hadronic models: • EPOS-LHC + Fluka & QGSJETII-3 + QHEISHA; • Zenith angle range: 0-40° + uniform azimuth angle; • 5 groups composition • P /He /CNO/MgAlSi/Iron • Detector response simulation: G4ARGO package • Core sampling 1500 x 15000 m2; • Data Selection • Core: |Xc|<31 + |Yc|<31 m; • Good contained data: r + Rp70 <50 m; • Zenith < 35 deg • <R> <22 m

  16. Moon shadow result 400-800 800-1000 1000-2000 >2000

  17. Preliminary result:

  18. Summary and Outlook • ARGO-YBJ is a good candidate to construct an “energy anchor”; • Selection of light component is OK; • Moon shadow measurement offers cross check; • Preliminary result is encouraging; • To finish work and understand systematic uncertainty;

  19. backup

  20. Moon shadow: an important tool to check the detector performances and offer energy calibration  10standard deviations /month Energy calibration West displacement of the shadow caused by the geomagnetic field Bending ≈ 1.58°Z/E (TeV) ARGO coll., Phys.Rev. D 84 (2011) 022003 / ARGO coll., Phys.Rev. D 85 (2012) 022002

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