1. Neutrino Astronomy at the South Pole David Boersma UW Madison “New Views of the Universe” Chicago, 10 December 2005

2. 10 December 2005David Boersma @ New Views of the Universe2 Cosmic Ray Spectrum

3. 10 December 2005David Boersma @ New Views of the Universe3 High Energy neutrinos Neglecting  absorption (uncertain)    Targets: p or ambient  Beam-dump model:  0   -astronomy  ±  -astronomy Berezinsky et al, 1985 Gaisser, Stanev, 1985

4. 10 December 2005David Boersma @ New Views of the Universe4 Neutrino Detection μ νμνμ νμνμ μ XX’ W Angle(ν μ,μ) ≈ 1° (at E=1TeV) Detected energy deposit by muon gives lower limit for energy of neutrino

5. 10 December 2005David Boersma @ New Views of the Universe5 Neutrino Detection ν e,τ XX’ W e,τ ν μ,e,τ XX’ Z μ,e,τ

6. 10 December 2005David Boersma @ New Views of the Universe6 Optical properties of ice @SP Average optical ice parameters: AMANDA/IceCube ANTARES abs ~ 110 m @ 400 nm abs ~ 60 m @ 470 nm sca ~ 20 m @ 400 nm sca ~ 300 m @ 400 nm

7. 10 December 2005David Boersma @ New Views of the Universe7 Amundsen-Scott South Pole Station Population: Austral Summer: ~240 people Austral Winter: ~60 people South Pole Dome Summer camp AMANDA road to work 1500 m 2000 m [not to scale] IceCube ANTARTICA

8. 10 December 2005David Boersma @ New Views of the Universe8 IceCube Collaboration IceCube Collaboration Universität Wuppertal, Germany Uppsala university, Sweden Stockholm university, Sweden Imperial College, London, UK Oxford university, UK Utrecht University, Netherlands Universität Wuppertal, Germany Uppsala university, Sweden Stockholm university, Sweden Imperial College, London, UK Oxford university, UK Utrecht University, Netherlands Universite Libre de Bruxelles, Belgium Vrije Universiteit Brussel, Belgium Université de Gent, Belgium Université de Mons-Hainaut, Belgium Universität Mainz, Germany DESY-Zeuthen, Germany Universität Dortmund, Germany Universite Libre de Bruxelles, Belgium Vrije Universiteit Brussel, Belgium Université de Gent, Belgium Université de Mons-Hainaut, Belgium Universität Mainz, Germany DESY-Zeuthen, Germany Universität Dortmund, Germany Bartol Research Institute, Delaware, USA Pennsylvania State University, USA UC Berkeley, USA UC Irvine, USA Clark-Atlanta University, USA University of Maryland, USA IAS, Princeton, USA University of Wisconsin, Madison, USA University of Wisconsin, River Falls, USA LBNL, Berkeley, USA University of Kansas, USA Southern University and A&M College, Baton Rouge, USA Bartol Research Institute, Delaware, USA Pennsylvania State University, USA UC Berkeley, USA UC Irvine, USA Clark-Atlanta University, USA University of Maryland, USA IAS, Princeton, USA University of Wisconsin, Madison, USA University of Wisconsin, River Falls, USA LBNL, Berkeley, USA University of Kansas, USA Southern University and A&M College, Baton Rouge, USA USA (12) Europe (13) Japan New Zealand ANTARCTICA Chiba University, Japan University of Canterbury, Christchurch, New Zealand Chiba University, Japan University of Canterbury, Christchurch, New Zealand

9. 10 December 2005David Boersma @ New Views of the Universe9AMANDA AMANDA-II (2000 – 200x) 677 OMs on 19 strings677 OMs on 19 strings 200m, 500m tallØ 200m, 500m tall Trigger rate 80 HzTrigger rate 80 Hz Since 2003: TWRSince 2003: TWR AMANDA-B10 (1997-1999) 302 OMs on 10 strings Ø 120m, 500m tall DAQ: TDC/ADC (surface) AMANDA-A (1996)

10. 10 December 2005David Boersma @ New Views of the Universe10 time recorded on OM AMANDA-II μ tracks pointing error :1.5º - 2.5º σ[log 10 (E μ /TeV)]:0.3 - 0.4 coverage:2π Cascades (particle showers) pointing error:30º - 40º σ[log 10 (E c /TeV)]:0.1 - 0.2 coverage:4π cosmic rays (+SPASE) combined pointing err : < 0.5º σ[log 10 (E p /TeV)]:0.06 - 0.1 Nucl. Inst. Meth. A 524, 169 (2004) energy deposited in OM

11. 10 December 2005David Boersma @ New Views of the Universe11 AMANDA research topics Steady sources of neutrinos Steady sources of neutrinos Point sources (AGNi) Point sources (AGNi) Diffuse flux (with muons) Diffuse flux (with muons) Diffuse flux (with cascades) Diffuse flux (with cascades) Atmosphere (cosmic rays) Atmosphere (cosmic rays) Gravitationally trapped WIMPs Gravitationally trapped WIMPs Magnetic monopoles Magnetic monopoles Search for sources with time variability Search for sources with time variability GRBs GRBs Supernovae Supernovae Flaring AGNi Flaring AGNi

12. 10 December 2005David Boersma @ New Views of the Universe12 Point source search Combined data from 2000-2003 (livetime 807 days) 3329 (upward going) neutrino events Highest excess: 3.4 sigma (chance probability: 92%) Crab nebula: 10 events, =5.4 (chance probability with 33 source candidates: 64%)

13. 10 December 2005David Boersma @ New Views of the Universe13 Atmospheric Muons & Neutrinos E deposited ≈ N ch Get E ν and E μ through unfolding

14. 10 December 2005David Boersma @ New Views of the Universe14 Diffuse flux

15. 10 December 2005David Boersma @ New Views of the Universe15 The first km 3 detector: IceCube 60/OM string 17 m vertical distance Strings in vertices of 125 m-side triangles

16. 10 December 2005David Boersma @ New Views of the Universe16 main board LED flasher board PMT base 25 cm PMT 33 cm Benthosphere

17. 10 December 2005David Boersma @ New Views of the Universe17 IceCube construction Jan 2005: 1 string (60 DOMs) + 4/8 tanks/ stations deployed 2005/6 Plan (starting now!) 10-12 strings 24/12 tanks/stations Full detector: 2010

18. 10 December 2005David Boersma @ New Views of the Universe18 High Energy muons E μ = 6 PeV

19. 10 December 2005David Boersma @ New Views of the Universe19 Contained High Energy Shower E = 375 TeV

20. 10 December 2005David Boersma @ New Views of the Universe20 High Energy Tau (double bang) E ≈ 10 PeV

21. 10 December 2005David Boersma @ New Views of the Universe21 Ice is a quiet detection medium (compare: expected ~60kHz per OM in ANTARES)

22. 10 December 2005David Boersma @ New Views of the Universe22 First IceTop-IceCube coincidence event

23. 10 December 2005David Boersma @ New Views of the Universe23 Conclusions & Outlook AMANDA showed the feasibility of High Energy Neutrino astronomy with ice as the detection medium. AMANDA showed the feasibility of High Energy Neutrino astronomy with ice as the detection medium. IceCube will be the coolest neutrino telescope on Earth. IceCube will be the coolest neutrino telescope on Earth. Maybe extended with acoustic detectors (extension to EHE) Maybe extended with acoustic detectors (extension to EHE)

24. 10 December 2005David Boersma @ New Views of the Universe24 Extra Material WIMPs WIMPs IceTop IceTop GRB GRB Deployment Deployment Flasher Flasher

25. 10 December 2005David Boersma @ New Views of the Universe25 WIMPs from the Sun  χ + χ  W + + W -  ν + ν ν l

26. 10 December 2005David Boersma @ New Views of the Universe26 WIMP limits

27. 10 December 2005David Boersma @ New Views of the Universe27

28. 10 December 2005David Boersma @ New Views of the Universe28 IceTop

29. 10 December 2005David Boersma @ New Views of the Universe29 27.1, 10:08: Reached maximum depth of 2517 m 28.1, 7:00: preparations for string installation start 9:15: Started installation of the first DOM 22:36: last DOM installed 12 min/DOM 22:48: Start drop 29.1, 1:31: String secured at depth of 2450.80 20:40: First communication to DOM IceCube’s First String: January 28, 2005

30. 10 December 2005David Boersma @ New Views of the Universe30 All 60 DOMs