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L.L.Ma for LHAASO collaboration Beijing China

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Presentation on theme: "L.L.Ma for LHAASO collaboration Beijing China"— Presentation transcript:

1 L.L.Ma for LHAASO collaboration Beijing China
Expectation on Observation of Cosmic Ray Energy Spectrum from 10PeV to 100PeV with LHAASO Experiment L.L.Ma for LHAASO collaboration Beijing China

2 Outline Difficulties in cosmic ray detection LHAASO introduction
LHAASO science in cosmic ray measurement Performance Study of LHAASO detectors Composition separation Energy resolution Effective aperture and event rate Summary

3 Difficulties in cosmic ray detection
Energy > 100 TeV Air shower measurement EAS array Cherenkov telescope or Array Fluorescence telescope Calibration of primary energy estimate uncertain. Composition measurement diffcult Model dependent

4 Large High Altitude Air Shower Observatory
1KM2 Array (KM2A) 5195 scintillator detectors every 15 m 1171 muon detectors every 30m Wide Field View Cherenkov telescope Array (WFCTA) 18 Telescopes Energy meaurements Hillas Geometry reconstruction ， Muon content Geometry reconstruction Core information Water Cherenkov detector Array (WCDA) 78,000m2 4400m above see level DaoCheng SiChuan Large High Altitude Air Shower Observatory

5 LHAASO science in cosmic ray measurement
Measure individual cosmic ray spectra from 10TeV to EeV Multi-parameters, Multi-stages 10TeV-100TeV Energy Scale WCDA, WFCTA 100TeV-10PeV Knees for H,He,… WCDA, WFCTA, KM2A 10PeV-100PeV knee of Fe WFCTA, KM2A 100PeV-2EeV 2nd knee & composition changing Transition from galactic to extra-galactic Proceedings 206

6 KM2 Array (KM2A) 2.8m 1.2m ED MD Effective area 1m2 36m2 Spacing 15m
NO. of detectors 5195 1171 Time resolution 2ns 10ns Muon number Core reconstruction : 5m Direction reconstruction: 0.3°

7 Wide Field view Cherenkov Telescope Array (WFCTA)
Reflectors: 25 spherical mirrors Side length：300mm curvature：5800mm Cameras 32 x 32 SiPMs 16degree X 14degree Pixel diameter:25.4mm Focal length: 2870mm Hillas Parameters Xmax Energy reconstruction

8 Performance Study of LHAASO detectors
Shower generation CORSIKA V74005 Energy range: 10PeV ~100PeV Compositions: Proton, helium, CNO, MgAlSi, iron hadronic model: QGSJETII04+FLUKA Layout of detectors Pointing direction of WFCTA 45°in zenith 0~360°in azimuth Air depth with zenith 45° Air depth of LHAASO

9 Composition separation
Obtained from KM2A Log10(Ne/Nmuon) Blue: iron Red:proton Obtained from WFCTA Distance: the angular distance between image center to the arriving directions

10 KM2A Blue: iron Red: proton WFCTA Purity in selecting iron: 84% Purity in selecting iron and MgAlSi: 94%

11 Energy reconstruction
The reconstructed energy is a function total Npe recorded by WFCTA and Rp Energy resolution <20% (Rp<100m) <25%(Rp<200m) ~30%(Rp<300m) Rp<100m Rp<200m Rp<300m

12 Effective aperture and event rate
15% duty cycle 50m<Rp<250m 50m<Rp<230m 50m<Rp<200m All particle 15% duty cycle 100irons Iron

13 Summary With multiple detectors LHAASO can measure individual spectra of cosmic rays by multi- parameters KM2A and WFCTA can be used in the 10PeV to 100PeV energy range 25 % energy resolution can be achieved 100 gold iron events can be obtained with 87% purity and at 100PeV

14 Thanks for your attention

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