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Particle Astronomy from Antarctica Per Olof Hulth Stockholm University

Particle Astronomy from Antarctica Per Olof Hulth Stockholm University. Why Particle Astronomy from Antarctica?. Difficult logistics No continues access during the year Cold and expensive Long time to build up large experiment. Antarctic platform.

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Particle Astronomy from Antarctica Per Olof Hulth Stockholm University

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  1. Particle Astronomy from Antarctica Per Olof Hulth Stockholm University Per Olof Hulth

  2. Why Particle Astronomy from Antarctica? • Difficult logistics • No continues access during the year • Cold and expensive • Long time to build up large experiment Per Olof Hulth

  3. Antarctic platform • 24 hours coverage of astronomical objects • Largest ice sheet with very transparent ice • Unique wind conditions at high altitudes • Low magnetic field cut off for cosmic charged particles • Possibility to combine large surface detectors with neutrino telescopes in the ice • South Pole special with the sources at constant zenith angles Per Olof Hulth

  4. One large common question to answer for Particle Astronomy from Antarctica From where are the cosmic rays coming? Medium energy Supernovas? Super High energy GRB? AGN? ?? LHC Galactic? Extra galactic? Per Olof Hulth

  5. What are the sources of the Cosmic rays? ? Some new physics? Galactic? Galactic? Extra galactic? Extra galactic? Per Olof Hulth

  6. Cosmic ray investigations • Determine the chemical composition and energy dependence of CR • Detect the incoming CR before interacting in the atmosphere (Balloon flights and space flights) • Only one particle at 1015 eV/m2 and year! Direct detection possible up to 1015 eV. Above 1015 eV using large air shower detectors at surface. But identification of primary particle depending on simulations of the shower development. • Detect CR sources by neutrino production at the source. Per Olof Hulth

  7. c Earth nm m Detector Dark matter detection by neutrinos Sun Per Olof Hulth

  8. Balloon Cosmic ray detectors CREAM Tiger ATIC TRACER Polar Patrol Balloon (PPB) Surface Cosmic ray detectors SPASE IceTop Neutrino Cherenkov telescopes AMANDA IceCube Neutrino radio telescopes Rice Anita Different projects in Antarctica Per Olof Hulth

  9. Balloons • NASA is using McMurdo as a base for launching Balloons for altitudes up to 37km • Long duration flights (LDF) up to three weeks • Ultra Long duration flights (ULDF) up to 100 days. • Only 5-10 grams/cm2 of the atmosphere remains. Per Olof Hulth

  10. Balloon Cosmic ray detectors • ATIC 1010 - 1014 eV H - Fe • CREAM 1012 - 5 1015 eV H - Fe • TIGER 108 - 1010 eV Fe - Zr • TRACER - 1014 eV O - Fe • Polar Patrol Balloon (PPB) 1010 - 1012 eV electrons Per Olof Hulth

  11. CREAM CREAM Per Olof Hulth

  12. ATIC 19 days of scientific mission Dec 02 - Jan.03 Per Olof Hulth

  13. Per Olof Hulth

  14. Tiger Per Olof Hulth

  15. Polar Patrol Ballon (PPB) Detector launched from Syowa station See poster 2013 IAU00287 by Toii Shoji Per Olof Hulth

  16. Messengers of Astronomy Only neutrinos cover the whole energy range Per Olof Hulth

  17. Neutrino fluxes from Cosmic ray sources log(E2 Flux) pp core AGN p blazar jet Top-Bottom model Various recent models for transient sources GRB (W&B) 3 6 9 log(E/GeV) TeV PeV EeV Per Olof Hulth

  18. Estimation of diffuse neutrino flux MPR W&B Atmospheric neutrinos Demands km3 size detectors!! Per Olof Hulth

  19. Neutrino telescopes • Needs large volumes of optical transparent material => ice sheet! Per Olof Hulth

  20. Detection of e , , O(km) long muon tracks Electromagnetic and hadronic cascades  15 m ~ 5 m direction determination by cherenkov light timing Per Olof Hulth

  21. Measured Ice properties at South Pole Per Olof Hulth

  22. AMANDA The worlds largest running neutrino telescope situated at the South Pole Per Olof Hulth

  23. South Pole Dark sector Skiway AMANDA Dome IceCube Per Olof Hulth

  24. AMANDA-II event 2000 • AMANDA observes about 3-4 atmospheric neutrinos/day in a atmospheric muon background 106 times larger. Per Olof Hulth

  25. AMANDA - deployment Per Olof Hulth

  26. Atmospheric muons in AMANDA-II Atmospheric muons and neutrinos: AMANDA‘s test beams much improved simulation ...but data 30% higher than MC ...  normalize to most vertical bin Systematic errors: 10% scattering (20m @ 400nm) absorption (110m @ 400nm) 20% optical module sensitivity 10% refreezing of ice in hole PRELIMINARY threshold energy ~ 40 GeV (zenith averaged) Per Olof Hulth

  27. Atmospheric n's in AMANDA-II neural network energy reconstruction regularized unfolding measured atmospheric neutrino spectrum  spectrum up to 100 TeV  compatible with Frejus data presently no sensitivity to LSND/Nunokawa prediction of dip structures between 0.4-3 TeV 1 sigma energy error In future, spectrum will be used to study excess due to cosmic ‘s Per Olof Hulth

  28. Point source search in AMANDA II Search for excess events in sky bins for up-going tracks 697 events observed above horizon 3% non-neutrino background for  > 5°  cuts optimized in each declination band PRELIMINARY above horizon:mostly fake events  sky subdivided into 300 bins (~7°x7°) no clustering observed Per Olof Hulth

  29. IceTop AMANDA South Pole Skiway 1400 m 2400 m IceCube • 80 Strings • 4800 PMT • Instrumented volume: 1 km3 (1 Gt) • IceCube is designed to detect neutrinos of all flavors at energies from 107 eV (SN) to 1020 eV Per Olof Hulth

  30. Status of IceCube • 15 $M approved for Fy02 • 25 $M for FY03 • 295 $M in presidents budget for FY04 (should cover the full detector plus 4 years of running) • New hot water drill to be sent to South Pole 03/04 • Up to 6 IceCube strings to be deployed 04/05 (and then up to 16 strings per year) Per Olof Hulth

  31. Grid North 100 m AMANDA South Pole SPASE-2 Dome Skiway IceCube:Top View Counting House Per Olof Hulth

  32. Finished DOM Ready to Pack and Test Per Olof Hulth

  33. Simulated nm-events in IceCube Eµ=10 TeV Eµ=6 PeV Measure muon energy at the detector by counting the number of fired PMTs. Per Olof Hulth

  34. Complementarity (point sources): E < 100 TeV Mediterranean (ocean) Antares, Nestor, 1 km3 ... South Pole (ice) AMANDA, ICECUBE galactic center in middle dots: distribution of gamma ray bursts (GRBs) Per Olof Hulth

  35. SPASE SPASE is an air shower detector at the South Pole for showers above 5 *1013 eV. SPASE measure the electromagnetic component of the shower AMANDA the muon component! Unique combination!! Per Olof Hulth

  36. AMANDA-SPASE • Plot muons vs. electrons • Transformed axes correspond to mass and energy Iron Protons Per Olof Hulth

  37. IceTop - IceCube • Particle astrophysics • using surface/under-ice coincidences as a novel probe of primary cosmic-ray spectrum to 1018 eV • Calibration • with tagged muons • Veto • of certain backgrounds for n signals Per Olof Hulth

  38. Incident cosmic-ray nucleus n Penetrating muon bundle in shower core EeV nm Detection in IceCube with shower veto m Threshold ~ 1017 eV to veto this background This background for EeV events can be vetoed by detecting the fringe of the coincident horizontal air shower in an array of water Cherenkov detectors (cf. Ave et al., PRL 85 (2000) 2244, analysis of Haverah Park) Per Olof Hulth

  39. Radio detectors Very high energy cascades emits Cherenkov radiation in radio wave length Larger attenuation length than optical -> larger volumes But higher energy threshold (> 10 PeV) Per Olof Hulth

  40. RICE South Pole Antennas deployed down to a few hundred meters in the AMANDA holes. Testing since 1996 Preparing an application for a larger RICE together with IceCube Per Olof Hulth

  41. n ANITA (Antarctic Impulsive Transient Array) Flight in 2006 Per Olof Hulth

  42. Summary • Antarctica as a very successful platform for particle astronomy! Per Olof Hulth

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