Simulation Studies for Cosmic Neutrino Detection with IceCube++ at the South Pole - PowerPoint PPT Presentation

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Simulation Studies for Cosmic Neutrino Detection with IceCube++ at the South Pole

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  1. Simulation Studies for Cosmic Neutrino Detectionwith IceCube++ at the South Pole Rolf Nahnhauer DESY SFB 676 C8-2

  2. ~ km sound disk p t radio lobe The Vision Build ~100 km3 hybrid detector to: Confirm GZK cutoff ! Do physics with extremelyhigh energy cosmic neutrinos*) - astrophysics - E > 1016eV : study origin of cosmic rays - (AGN’s, black holes, GZK cutoff, …) - particle physics - E > 1018eV : study neutrino cross section (sphalerons, mini BH, strong,…) - cosmology - E > 1021eV : study relic neutrino background radiation (UHE absorption at CBR ) nm optical light cone m *) see e.g. A. Ringwald ,ARENA 2005 SFB 676 C8-2

  3. Milestone One nearly finished Check capabilities of technologies at South Pole R. Bay, UCB, unpublished Optical detection: excellent  AMANDA, IceCube transp. / arb. units 92000 year old ash layer Radio detection: probably good RICE, more to come (AURA, IceRay) ice depth / m bottom echo visible through 2x 2.8 km! Acoustic detection: no measurements until recently Expectations: att ~ 1-10 km low noise favourable refraction  confirm by in-situ test “SPATS” SFB 676 C8-2

  4. SPATS The South Pole Acoustic Test Setup 3 strings deployed Jan/07+1 string deployed Dec/07 instrumented depth:80m - 500m per string:7 sensors, 7 transmitters string-PC: digitization, time-stamp, monitoring (p, T) master-PC: process steering, GPS data storage data transfer via satellite Measure: 1) speed of sound + refraction 2) sound attenuation length3) absolute noise level 4) transient signal rate + source SFB 676 C8-2

  5. SPATS Status Summary Mission accomplished to ~80% : -1) Speed of Sound + Refraction speed of sound constant below 200 m no refraction - 2) Sound Attenuation Length 300 m < λ <  , needs to be improved new measurements at longer baseline transient signals - 3) Absolute Noise Level gaussian and stable < 10 mPa ( with reasonable assumptions) think about in-situ calibration - 4) Transient Signal Rate small (~100 events/day) easy to separate from neutrino signal +++ + ++ +++ SFB 676 C8-2

  6. Near Term Future IceCube Meeting Utrecht September 2008 1 Day Common Meeting of Radio and Acoustic groups about future strategy SFB 676 C8-2

  7. Milestone Two to be started Detailed simulations forGZK hybrid detector at South Pole D. Besson et al.,astroph/0512604 Very first approach: instrumented volume ~(110 +3) km3 Calculations done up to now : - for only one neutrino flux model- without detailed input for detector - without measured target material properties GZK neutrino flux:R. Engel, D. Seckel and T. Stanev Phys. Rev. D 64, 093010 (2001) SFB 676 C8-2

  8. Necessary Next Steps • Working group and collaboration building • Write Letter of Intent to demonstrate: scientific importance in comparison to other topics  expected improvement to previous experiments time scenario and milestones • Finish basic exploration of ice properties • Start extensive MC studies of different detector options • Track down number of different detector options • Write Proposal •  expand letter of intent to give detailed information based on extensive MC and hardware studies still go with flexible design plan and 2 phase structure include realistic budget plan SFB 676 C8-2

  9. Resources at DESY Available for SFB C8-2: Working hours /week scientific ass. R. Nahnhauer 10scientific ass. C.Spiering Cpostdoc J. Berdermann 5PhD Student D. Tosi (later NN) 20 Required for SFB C8-2: postdoc NN 40 + some travel money SFB 676 C8-2