Neutrino Astronomy at the South Pole

1. Neutrino Astronomy at the South Pole David Boersma UW Madison Lake Louise Winter Institute Chicago, 23 February 2006

2. IceCube Collaboration • Alabama University, USA • University of Alaska, Anchorage, 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 (14) Europe (15) Japan New Zealand ANTARCTICA • Universite Libre de Bruxelles, Belgium • Vrije Universiteit Brussel, Belgium • Université de Gent, Belgium • Université de Mons-Hainaut, Belgium • Universität Mainz, Germany • Humboldt Universität, Germany • DESY-Zeuthen, Germany • Universität Dortmund, Germany • Universität Wuppertal, Germany • MPI Heidelberg • Uppsala university, Sweden • Stockholm university, Sweden • Imperial College, London, UK • Oxford university, UK • Utrecht University, Netherlands • Chiba University, Japan • University of Canterbury, Christchurch, New Zealand David Boersma @ Lake Louise Winter Institute 2006

3. ANTARTICA Amundsen-Scott South Pole Station IceCube South Pole Dome road to work AMANDA Summer camp 1500 m Population: Austral Summer: ~240 people Austral Winter: ~60 people David Boersma @ Lake Louise Winter Institute 2006 2000 m [not to scale]

4. Cosmic Ray Spectrum ? David Boersma @ Lake Louise Winter Institute 2006

5. Berezinsky et al, 1985 Gaisser, Stanev, 1985 High Energy neutrinos Beam-dump model: p0g-astronomy p±n-astronomy Neglecting g absorption (uncertain) ng Targets: p or ambient g David Boersma @ Lake Louise Winter Institute 2006

6. Neutrino Detection μ νμ W X X’ μ νμ Angle(νμ,μ) ≈ 1° (at E=1TeV) Detected energy deposit by muon gives lower limit for energy of neutrino David Boersma @ Lake Louise Winter Institute 2006

7. νe,τ e,τ W N X Neutrino Detection νμ,e,τ νμ,e,τ Z N X David Boersma @ Lake Louise Winter Institute 2006

8. AMANDA AMANDA-A (1996) AMANDA-B10 (1997-1999) • 302 OMs on 10 strings • Ø 120m, 500m tall • DAQ: TDC/ADC (surface) AMANDA-II (2000 – 200x) • 677 OMs on 19 strings • Ø 200m, 500m tall • Trigger rate 80 Hz • Since 2003: TWR David Boersma @ Lake Louise Winter Institute 2006

9. AMANDA research topics • Steady sources of neutrinos • Point sources (e.g. AGNs) • Diffuse flux (with muons) • Diffuse flux (with cascades) • Atmosphere (cosmic rays) • Gravitationally trapped WIMPs • Exotics: e.g. magnetic monopoles • Search for sources with time variability • GRBs • Supernova explosions • Flarers from e.g. AGNs, magnetars David Boersma @ Lake Louise Winter Institute 2006

10. 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, <Nbg>=5.4 (chance probability with 33 source candidates: 64%) David Boersma @ Lake Louise Winter Institute 2006

11. Atmospheric Muons & Neutrinos E deposited Nch Get Eν and Eμ through unfolding David Boersma @ Lake Louise Winter Institute 2006

12. WIMPs from the Sun c χ + χ → ν + ν (+…) ν David Boersma @ Lake Louise Winter Institute 2006 l

13. WIMP search in AMANDA Published in Astrpart. Phys. Submitted for publication Limits on muon flux from Sun Limits on muon flux from Earth center Disfavored by direct search (CDMS II) David Boersma @ Lake Louise Winter Institute 2006

14. Let’s build a bigger one: IceCube Construction: 2004-2010 (status February 2006) In-Ice Array: Number of strings: 80 (9) Optical Sensors: 4800 (540) Depth: 1450-2450m Instr. Volume: 0.9 km3 Angular Resolution: 0.6° Surface Array (IceTop): 160 (32) tanks (2 per in-ice string) 2 DOMs per tank Total 320 DOMs (64) David Boersma @ Lake Louise Winter Institute 2006

15. LED flasher board main board PMT base 25 cm PMT 33 cm Benthosphere David Boersma @ Lake Louise Winter Institute 2006

16. High Energy muons Eμ= 6 PeV David Boersma @ Lake Louise Winter Institute 2006

17. ContainedHigh Energy Shower E = 375 TeV David Boersma @ Lake Louise Winter Institute 2006

18. High Energy Tau(double bang) E ≈ 10 PeV David Boersma @ Lake Louise Winter Institute 2006

19. Ice is a quiet detection medium (compare: expected ~60kHz per OM in ANTARES) David Boersma @ Lake Louise Winter Institute 2006

20. First IceTop-IceCube coincidence event David Boersma @ Lake Louise Winter Institute 2006

21. Conclusions & Outlook • AMANDA showed the feasibility of High Energy Neutrino astronomy with ice as the detection medium. • IceCube will be the coolest neutrino telescope on Earth. • Maybe extended with acoustic detectors (extension to EHE) David Boersma @ Lake Louise Winter Institute 2006

22. Extra Material • Specs AMANDA (resolution etc.) • IceTop • GRB • Deployment • Flasher David Boersma @ Lake Louise Winter Institute 2006

23. AMANDA-II μ tracks pointing error : 1.5º - 2.5º σ[log10(Eμ/TeV)]: 0.3 - 0.4 coverage: 2π Cascades (particle showers) pointing error: 30º - 40º σ[log10(Ec/TeV)]: 0.1 - 0.2 coverage: 4π cosmic rays (+SPASE) combined pointing err : < 0.5ºσ[log10(Ep/TeV)]: 0.06 - 0.1 Nucl. Inst. Meth. A 524, 169 (2004) energy deposited in OM time recorded on OM David Boersma @ Lake Louise Winter Institute 2006

24. David Boersma @ Lake Louise Winter Institute 2006

25. IceTop David Boersma @ Lake Louise Winter Institute 2006

26. IceCube’s First String: January 28, 2005 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 David Boersma @ Lake Louise Winter Institute 2006

27. All 60 DOMs David Boersma @ Lake Louise Winter Institute 2006