enhancements to the observatory: heat and amiga

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Enhancements to the Observatory: HEAT and AMIGA Peter O. Mazur Director’s Review December 15, 2011 1

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Enhancements to the Observatory: HEAT and AMIGA. Peter O. Mazur Director’s Review December 15, 2011. The Goals. Extend the energy reach down to ~0.1 EeV Main Observatory sensitive down to ~3 EeV - PowerPoint PPT Presentation

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Page 1: Enhancements to the Observatory: HEAT and AMIGA

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Enhancements to the Observatory:HEAT and AMIGA

Peter O. MazurDirector’s Review

December 15, 2011

Page 2: Enhancements to the Observatory: HEAT and AMIGA

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The Goals• Extend the energy reach down to ~0.1 EeV

– Main Observatory sensitive down to ~3 EeV– Transition from galactic to extragalactic origin expected to occur between 0.1 EeV

and 10 EeV.– Overlap with highest energy LHC measurements for understanding of hadronic

interactions • Enhancement to FD to extend energy spectrum and composition

measurements from 0.1 EeV to overlap with main Observatory energy range.

• Enhancement to SD to measure spectrum above ~0.3 EeV to overlap with main Observatory and to measure composition (using buried muon counters) from 0.3 – 3 EeV

• Both enhancements provide source angular position measurement for large scale anisotropy determination.

Page 3: Enhancements to the Observatory: HEAT and AMIGA

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Fluorescence Detector Enhancement:HEAT: High Elevation Auger Telescopes

• Main telescopes consist of four sites with six telescopes each, with each telescope covering 30°×30°

• HEAT consists of one site (180m from Choihueco FD telescopes) with three telescopes.– Telescopes similar to main FD but they can be tilted upward

by 30°– Operation at 0°: calibration and overlap with Coihueco

telescopes.– Operation at 30°: sensitive to low energy showers which

occur higher in the atmosphere and, being fainter, must be closer to the detector.

Page 4: Enhancements to the Observatory: HEAT and AMIGA

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Page 5: Enhancements to the Observatory: HEAT and AMIGA

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HEAT and the Infill

Page 6: Enhancements to the Observatory: HEAT and AMIGA

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Surface Detector EnhancementAMIGA: Auger Muon and Infill for the Ground Array

• Main array is 1600 surface detectors (SD) with 1.5 km spacing, sensitive down to ~3 EeV.

• Infill array of identical SD embedded in main array with spacing 750 m lowers sensitivity limit to ~0.3 EeV.

• Muon counters being installed paired with infill SDs.

Page 7: Enhancements to the Observatory: HEAT and AMIGA

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Infill vs. Main Array Trigger Efficiency

Page 8: Enhancements to the Observatory: HEAT and AMIGA

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Preliminary Energy Spectrum

Page 9: Enhancements to the Observatory: HEAT and AMIGA

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Muon Counters

Page 10: Enhancements to the Observatory: HEAT and AMIGA

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Enhancements Status

• HEAT complete and operating as expected• AMIGA 750 m infill complete and operating as

expected• AMIGA Muon counters under development and in

production• Fermilab was not involved in HEAT• Fermilab has minimal involvement in AMIGA– Fermilab made the scintillator, paid for by others.– Peter Mazur advised on design and production of muon

counters.