IAU Sydney Per Olof Hulth Particle Astronomy from Antarctica Per Olof Hulth Stockholm University

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

IAU Sydney Per Olof Hulth 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

IAU Sydney Per Olof Hulth 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?

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

IAU Sydney Per Olof Hulth 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 eV/m 2 and year! Direct detection possible up to eV. Above 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.

IAU Sydney Per Olof Hulth Dark matter detection by neutrinos Sun  Earth Detector  

IAU Sydney Per Olof Hulth Different projects in Antarctica 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

IAU Sydney Per Olof Hulth 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/cm 2 of the atmosphere remains.

IAU Sydney Per Olof Hulth Balloon Cosmic ray detectors ATIC eVH - Fe CREAM eV H - Fe TIGER eVFe - Zr TRACER eVO - Fe Polar Patrol Balloon (PPB) eVelectrons

IAU Sydney Per Olof Hulth CREAM

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

IAU Sydney Per Olof Hulth

IAU Sydney Per Olof Hulth Tiger

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

IAU Sydney Per Olof Hulth Messengers of Astronomy Only neutrinos cover the whole energy range

IAU Sydney Per Olof Hulth log(E 2  Flux) log(E/GeV) TeV PeV EeV pp core AGN p  blazar jet Top-Bottom model GRB (W&B) Various recent models for transient sources Neutrino fluxes from Cosmic ray sources

IAU Sydney Per Olof Hulth Estimation of diffuse neutrino flux Atmospheric neutrinos W&B MPR Demands km 3 size detectors!!

IAU Sydney Per Olof Hulth Neutrino telescopes Needs large volumes of optical transparent material => ice sheet!

IAU Sydney Per Olof Hulth ~ 5 m Detection of e, ,  Electromagnetic and hadronic cascadesO(km) long muon tracks direction determination by cherenkov light timing  15 m

IAU Sydney Per Olof Hulth Measured Ice properties at South Pole

IAU Sydney Per Olof Hulth AMANDA The worlds largest running neutrino telescope situated at the South Pole

IAU Sydney Per Olof Hulth South Pole Dark sector AMANDA IceCube Dome Skiway

IAU Sydney Per Olof Hulth AMANDA-II event 2000 AMANDA observes about 3-4 atmospheric neutrinos/day in a atmospheric muon background 10 6 times larger.

IAU Sydney Per Olof Hulth AMANDA - deployment

IAU Sydney Per Olof Hulth Atmospheric muons in AMANDA-II PRELIMINARY threshold energy ~ 40 GeV (zenith averaged) 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 400nm) absorption 400nm)  20% optical module sensitivity  10% refreezing of ice in hole

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

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

IAU Sydney Per Olof Hulth IceCube 1400 m 2400 m AMANDA South Pole IceTop Skiway 80 Strings 4800 PMT Instrumented volume: 1 km3 (1 Gt) IceCube is designed to detect neutrinos of all flavors at energies from 10 7 eV (SN) to eV

IAU Sydney Per Olof Hulth Status of IceCube 15 $M approved for Fy02 25 $M for FY $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)

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

IAU Sydney Per Olof Hulth Finished DOM Ready to Pack and Test

IAU Sydney Per Olof Hulth E µ =10 TeVE µ =6 PeV Simulated  -events in IceCube Measure muon energy at the detector by counting the number of fired PMTs.

IAU Sydney Per Olof Hulth Mediterranean (ocean) Antares, Nestor, 1 km 3... South Pole (ice) AMANDA, ICECUBE dots: distribution of gamma ray bursts (GRBs) galactic center in middle E  < 100 TeV Complementarity (point sources):

IAU Sydney Per Olof Hulth SPASE SPASE is an air shower detector at the South Pole for showers above 5 *10 13 eV. SPASE measure the electromagnetic component of the shower AMANDA the muon component! Unique combination!!

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

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

IAU Sydney Per Olof Hulth EeV  Detection in IceCube with shower veto  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) Penetrating muon bundle in shower core Incident cosmic-ray nucleus Threshold ~ eV to veto this background

IAU Sydney Per Olof Hulth 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)

IAU Sydney Per Olof Hulth 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 RICE South Pole

IAU Sydney Per Olof Hulth Flight in 2006 ANITA (Antarctic Impulsive Transient Array)

IAU Sydney Per Olof Hulth Summary Antarctica as a very successful platform for particle astronomy!