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  • Количество слайдов: 60

C. Spiering, Leeds, July 23, 2004 C. Spiering, Leeds, July 23, 2004

Entrance to the Promised Land after 40 Years ! Entrance to the Promised Land after 40 Years !

Moisej Markov 1960 M. Markov, : We propose to install detectors deep in a Moisej Markov 1960 M. Markov, : We propose to install detectors deep in a lake or in the sea and to determine the direction of charged particles with the help of Cherenkov radiation Bruno Pontecorvo

Pioneering DUMAND Fred Reines John Learned + Roberts, Stenger, Gorham, . . ~ 1975: Pioneering DUMAND Fred Reines John Learned + Roberts, Stenger, Gorham, . . ~ 1975: first meetings towards an underwater array close to Hawaii

DUMAND-II Proposal 1988 : - 216 PMTs at 9 strings - height 230 m DUMAND-II Proposal 1988 : - 216 PMTs at 9 strings - height 230 m Alas !. . . terminated in 1996

Later used by Amanda and Baikal 1987: DUMAND test string Later used by Amanda and Baikal 1987: DUMAND test string

Search for diffuse excess of extraterrestrial high energy neutrinos DUMAND FREJUS MACRO bound WB Search for diffuse excess of extraterrestrial high energy neutrinos DUMAND FREJUS MACRO bound WB bound log E /Ge. V

Neutrino Telescopes Underground KGF Baksan FREJUS IMB e. g. MACRO, 1356 upgoing muons Kamiokande Neutrino Telescopes Underground KGF Baksan FREJUS IMB e. g. MACRO, 1356 upgoing muons Kamiokande Superkamiokande MACRO ~ 1000 m²

Pioneering BAIKAL Bezrukov, Domogatsky Berezinsky, Zatsepin 1981 1984 1993 1994 1998 first site explorations Pioneering BAIKAL Bezrukov, Domogatsky Berezinsky, Zatsepin 1981 1984 1993 1994 1998 first site explorations first stationary string first neutrino detector NT-36 first atm. neutrino separated NT-200 finished G. Domogatsky ~ 2 x Super-K for 1 Te. V muons

Camp Ice as a natural deployment platform Camp Ice as a natural deployment platform

1366 m 3600 m NT-200 4 -string stage (1996) 1366 m 3600 m NT-200 4 -string stage (1996)

Baikal Search for H. E. Cascades NT-200 Look for upward moving light fronts. Signal: Baikal Search for H. E. Cascades NT-200 Look for upward moving light fronts. Signal: isolated cascades from neutrino interactions Background: Bremsshowers from h. e. downward muons e lar um ve vol cti e effe g

Baikal Upgrade NT 200+ 140 m cascades 36 additional PMTs 4 times better sensitivity Baikal Upgrade NT 200+ 140 m cascades 36 additional PMTs 4 times better sensitivity !

Mediterannean approaches NESTOR (since 1991) „Amanda-sized“ -- under construction ANTARES (since 1996) „Amanda sized“ Mediterannean approaches NESTOR (since 1991) „Amanda-sized“ -- under construction ANTARES (since 1996) „Amanda sized“ -- under construction NEMO: R&D for km 3 project Since 2003: joined km 3 initiative KM 3 NET

2400 m ANTARES NEMO 3400 m 4100 m NESTOR 2400 m ANTARES NEMO 3400 m 4100 m NESTOR

Beyond the DUMAND scale: AMANDA first site studies at South Pole shallow detector in Beyond the DUMAND scale: AMANDA first site studies at South Pole shallow detector in bubbly ice ~ 1990 1993/4 10 strings (Amanda-B 10) 1997 19 strings (Amanda-II) 2000 Francis Halzen + Steve Barwick, Bob Morse, . .

AMANDA depth Super-K DUMAND AMANDA-II Amanda-II: 677 PMTs at 19 strings (1996 -2000) AMANDA depth Super-K DUMAND AMANDA-II Amanda-II: 677 PMTs at 19 strings (1996 -2000)

Ocean Water Ocean Water

Hot water drilling Drilling Hot water drilling Drilling

AMANDA Event Signatures: Muons CC muon neutrino interaction track + N + X AMANDA Event Signatures: Muons CC muon neutrino interaction track + N + X

AMANDA Event Signatures: Cascades § CC electron and tau neutrino interaction: § (e, , AMANDA Event Signatures: Cascades § CC electron and tau neutrino interaction: § (e, , ) + N (e, ) + X § NC neutrino interaction: x + N x + X Cascades

First spectrum > 3 Te. V: - up to 100 Te. V - matches First spectrum > 3 Te. V: - up to 100 Te. V - matches lower-energy Frejus data PRELIMINARY

Skyplot Amanda-II, 2000 697 events below horizon above horizon: mostly fake events Skyplot Amanda-II, 2000 697 events below horizon above horizon: mostly fake events

Intrinsic source spectrum (corrected for IR absorption) Measured spectrum AMANDA average flux limit for Intrinsic source spectrum (corrected for IR absorption) Measured spectrum AMANDA average flux limit for two assumed spectral indices , compared to the average gamma flux of Markarian 501 as observed in 1997 by HEGRA. AMANDA-II has reached the sensitivity needed to search from neutrino fluxes from Te. V gamma sources of similar strength to the instrinsic gamma flux.

90% C. L. upper limits (in units of 10 -8 cm-2 s-1) for selected 90% C. L. upper limits (in units of 10 -8 cm-2 s-1) for selected sources for an E-2 spectral shape integrated above Eν=10 Ge. V 1997 2000+2001 Nobs / Nbgr Source Declination SS 433 5. 0 o - 0. 7 0 / 2. 38 2. 3 1 / 1. 69 M 87 12. 4 o 17. 0 1. 0 0 / 0. 95 3. 8 2 / 1. 10 Crab 22. 0 o 4. 2 2. 4 2 / 1. 76 4. 2 3 / 1. 10 Mkn 421 38. 2 o 11. 2 3. 5 3 / 1. 50 1. 5 0 / 0. 65 Mkn 501 39. 8 o 9. 5 1. 8 1 / 1. 57 1. 4 0 / 0. 69 Cyg. X-3 41. 0 o 4. 9 3. 5 3 / 1. 69 1. 5 0 / 0. 67 Cas. A 58. 8 o 9. 8 1. 2 0 / 1. 01 4. 7 2 / 1. 03 PRELIMINARY

AMANDA skyplot 2000 -2003 optimized for best sensitivity to E-3 – E-2 sources reli AMANDA skyplot 2000 -2003 optimized for best sensitivity to E-3 – E-2 sources reli P y nar mi 3369 events

elim Pr ary in elim Pr ary in

ary in elim Pr Cas A Mk 421 Mk 501 Cyg Crab M 87 ary in elim Pr Cas A Mk 421 Mk 501 Cyg Crab M 87 SS 433

Selected Source Analysis Stacking Source Analysis Galactic Plane Transient Sources Burst Search Correlation Analysis Selected Source Analysis Stacking Source Analysis Galactic Plane Transient Sources Burst Search Correlation Analysis Multi-Pole Analysis Lower energy threshold (optimize to steeper spectra)

cm-2 s-1 southern sky 10 -14 and er-Kamiok up 4 years S e cm-2 s-1 southern sky 10 -14 and er-Kamiok up 4 years S e northern sky 170 days AMANDA-B 10 230 days AMANDA-II 8 years MACRO SS-433 10 -15 Mk-501 / ~ 1 Expected sensitivity for AMANDA 97 -03 Measured sensitivity 00 -03 -90 -45 0 45 declination (degrees) 90

Experimental Limits DUMAND FREJUS MACRO Baikal (98, 99, 00) bound Amanda-B 10 (1997), UHE Experimental Limits DUMAND FREJUS MACRO Baikal (98, 99, 00) bound Amanda-B 10 (1997), UHE Amanda-B 10 (1997) Amanda-II (2000) cascades Amanda-II (2000) Expectation Amanda-II, 3 years WB bound Expectation Ice. Cube, 3 years In red: only muons In blue: all flavors

e: : = 1: 2: 0 1: 1: 1 bound WB bound e: : = 1: 2: 0 1: 1: 1 bound WB bound

bound WB bound bound WB bound

Experimental all-flavor limits FREJUS DUMAND MACRO Amanda-B 10 (1997) Baikal (98, 99, 00) bound Experimental all-flavor limits FREJUS DUMAND MACRO Amanda-B 10 (1997) Baikal (98, 99, 00) bound Amanda-B 10 (1997), UHE Amanda-II (2000) cascades Expectation Amanda-II, 3 years WB bound Expectation Ice. Cube, 3 years

-1 hour +1 hour 10 min Blinded Window Background determined on-source/off-time - Low background -1 hour +1 hour 10 min Blinded Window Background determined on-source/off-time - Low background (due narrow time and space coincidence) - Large effective areas (50 000 m² @ 1 Pe. V) Year # of GRB Bkgd seen events 1997 78 0. 06 0 1998 99 0. 20 0 1999 96 0. 20 0 2000 44 0. 40 0 Total Upper limit: 218 0. 86 0 16 · Waxman/Bahcall flux t=0+1 h Waxman/Bahcall 99

Indirect Search for WIMPs Neutrinos from the Sun Amanda At South Pole the Sun Indirect Search for WIMPs Neutrinos from the Sun Amanda At South Pole the Sun sinks maximally 23° below horizon. Therefore only Amanda-II with its dramatically improved reconstruction capabilities for horizontial tracks (compared to Amanda-B 10) can be used for solar WIMP search.

Present upper limits and expected Ice. Cube sensitivity on muon flux from neutralino annihilations Present upper limits and expected Ice. Cube sensitivity on muon flux from neutralino annihilations in center of Sun d ore rch v isfa t sea D rec i yd b

upper limit (cm-2 s-1 sr-1) 10 -14 Soudan KGF 10 -15 Baikal-98, 99, 00 upper limit (cm-2 s-1 sr-1) 10 -14 Soudan KGF 10 -15 Baikal-98, 99, 00 MACRO Orito 10 -16 10 -17 Cherenkov-Light Amanda-97 n 2·(g/e)2 el ectr ons n = 1. 33 (g/e) = 137/ 2 Ice. Cube 10 -18 0. 50 0. 75 = v/c Search for relativistic magnetic monopoles 1. 00 8300

Supernova-Monitor Amanda-II B 10: 60% of Galaxy A-II: 95% of Galaxy Amanda-B 10 Count Supernova-Monitor Amanda-II B 10: 60% of Galaxy A-II: 95% of Galaxy Amanda-B 10 Count rates 0 5 Ice. Cube: Up to LMC 10 sec Ice. Cube

The km 3 scale at South Pole Ice. Cube - 80 Strings - 4800 The km 3 scale at South Pole Ice. Cube - 80 Strings - 4800 PMTs - Instrumented Volume: 1 km 3 - Installation: 2005 -2010

6 Amanda modules Ice. Cube Super. Kamiokande (Japan) AMANDA-II 6 Amanda modules Ice. Cube Super. Kamiokande (Japan) AMANDA-II

Aeff / km 2 Ice. Cube Effective Area Ice. Cube Eff Area cos Aeff / km 2 Ice. Cube Effective Area Ice. Cube Eff Area cos

Ice. Top + Ice. Cube: 1/3 km 2 sr …. . for coincident tracks Ice. Top + Ice. Cube: 1/3 km 2 sr …. . for coincident tracks VETO against all downward events E > 300 Te. V with trajectories inside Ice. Top CALIBRATION of angular response and geometry with tagged muons CHEMICAL COMPOSITION in energy range 1015 e. V – 1018 e. V

Cosmic rays Amanda/Spase Ice. Cube/Ice. Top. . . investigates transition to extra-galactic CR Cosmic rays Amanda/Spase Ice. Cube/Ice. Top. . . investigates transition to extra-galactic CR

cm-2 Achieved and expected sensitivities to steady point sources s-1 10 -14 AMANDA cm-2 Achieved and expected sensitivities to steady point sources s-1 10 -14 AMANDA Super-K, MACRO 2001 SS-433 10 -15 Antares Nestor ? 2003 Mk-501 / ~ 1 GX 339 -4 2007 10 -16 Ice. Cube KM 3 in Mediterr. 10 -17 2012 -90 -45 0 45 90

Achieved and expected sensitivities to diffuse fluxes RICE Amanda, Baikal 2002 AGASA RICE AGASA Achieved and expected sensitivities to diffuse fluxes RICE Amanda, Baikal 2002 AGASA RICE AGASA AUGER t 2004 Anita AABN 2007 EUSO 2012 km 3 Auger Salsa

„Nothing is guaranteed, but history is on our side. “ Francis Halzen „Nothing is guaranteed, but history is on our side. “ Francis Halzen

Moses HAD a guarantee for final success. . . but saw the promised land Moses HAD a guarantee for final success. . . but saw the promised land only from far and never entered it by himself. With nearly 3 orders of magnitude improvement over 10 years we have a good chance for success before OUR retirement !