Performance of the AMANDA-II Detector AMANDA-II Detector First Analysis Conclusions Largest High Energy Neutrino- Detector ever built:An open Under-Ice Cerenkov Detector for high energy muons and showers. 19 vertical strings with 677 Optical Modules (OM): 8 inch PMTs with analog pulse transmission to surface. Construction started in fall 1995, full detector commssioned in early 2000. Different technologies applied: strings 1-10: analog electrical pulse transmission strings 11-19: analog fiber pulse transmission 1 test string with Digital OM technology (IceCube prototype) Results obtained with the10 string detector AMANDA-B10 (1997 data) Isolation of 325 atmospheric v μ achieved - proof of performance (Nature,2001) - HE2.03 Limits on flux of HE diffuse v μ /v e -flux (AGN) - HE2.03 Limits on v-flux from point sources and GRB and UHE-v - HE232/236 Limit on WIMPs, on relativistic magnetic Monopoles and galactic Supernova v‘s - HE231 Reconstructed zenith angle cos(Θ reco ) (left) and azimuth angle Φ reco (right, in degress) at trtigger level Signal Expectation R.Wischnewski for the AMANDA Collaboration; DESY-Zeuthen, Germany AMANDA-II is in stable operation and delivers high quality muon and neutrino data. Neutrino-event selection is much improved over AMANDA-B10 by better geometry and better OM timing. Neutrino event-rates will be at least 3 times larger compared to B10. Angular acceptance is much improved for horizontal tracks, Trigger: majority trigger (>23 OMs in 2.5 μs) and local cluster trigger external: EAS-array SPASE Data sample: 1.3 TB raw data in ca. 250 run days in 2000 MC-data comparison at trigger and higher v-cut levels number of hit PMTs (n OM ), angular-distributions, pass.-rates fit well absolute rates & vertical hit structure under study (ice, noise) Data-analysis for AMANDA-II/2000 has started. Preliminary v -cuts developed. Number of hit optical modules per event, n OM (dots- exper., histogram -MC). Astrophysical sources: AGN, GRB, SN-shells, topological defects,... with spectra much harder than v‘s generated in the atmosphere Assume a diffuse AGN E -2 spectrum: 10 -6 E -2 GeV sr -1 s -1 cm -2 Trigger level acceptance of v μ and v e Charged Current (CC) and Neutral Current (NC) interactions: Neutrino energy spectrum for events, triggering AMANDA-II: CC v μ -events (thick lines) and CC v e -events (thin lines) for atmospheric neutrinos (full lines) and AGN like neutrinos (dashed-dotted lines). Zenith angle distribution for atmospherci nmu MC events in AMANDA-II (full line), compared to AMANDA-B10 detector (dashed). Preliminary cuts, normalized for vertical bin. AGN Atm The various analog OMs used in AMANDA-II: electrical and ﬁber readout modules, and the digitally controlled module (from left to right). For Digital OM see H.E.2.05 An AMANDA-II v-candidate close to the horizon, May 2000. v μ v e AMANDA-II AMANDA-B10 Triggered events / year Atmospheric AGN v μ 11000 (CC) 130 (NC) 853 (CC) v e 162 (CC) 9 (NC) 103 (CC)

Performance of the AMANDA-II Detector

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Performance of the AMANDA-II Detector. R.Wischnewski for the AMANDA Collaboration; DESY-Zeuthen, Germany. AMANDA-II Detector.  Largest High Energy Neutrino-Detector ever built:An open Under-Ice Cerenkov Detector for high energy muons and showers. - PowerPoint PPT Presentation

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Performance of the AMANDA-II Detector

AMANDA-II Detector

First Analysis

Conclusions

Largest High Energy Neutrino-Detector ever built:An open Under-Ice Cerenkov Detector for high energy muons and showers. 19 vertical strings with 677 Optical Modules (OM): 8 inch PMTs with analog pulse transmission to surface. Construction started in fall 1995, full detector commssioned in early 2000. Different technologies applied: strings 1-10: analog electrical pulse transmission strings 11-19: analog fiber pulse transmission 1 test string with Digital OM technology (IceCube prototype)

Results obtained with the10 string detector AMANDA-B10 (1997 data) Isolation of 325 atmospheric vμ achieved - proof of performance (Nature,2001) - HE2.03

Limits on flux of HE diffuse vμ/ve-flux (AGN) - HE2.03 Limits on v-flux from point sources and GRB and UHE-v - HE232/236 Limit on WIMPs, on relativistic magnetic Monopoles and galactic Supernova v‘s - HE231

Reconstructed zenith angle cos(Θreco) (left) and azimuth angle Φreco (right, in degress) at trtigger level

Signal Expectation

R.Wischnewski for the AMANDA Collaboration; DESY-Zeuthen, Germany

AMANDA-II is in stable operation and delivers high quality muon and neutrino data. Neutrino-event selection is much improved over AMANDA-B10 by better geometry and better OM timing. Neutrino event-rates will be at least 3 times larger compared to B10. Angular acceptance is much improved for horizontal tracks, opening full lower hemisphere for HE-neutrino astronomy. DAQ-Upgrade planned for 2001/02 for improved HE/UHE sensitivity.

Trigger: majority trigger (>23 OMs in 2.5 μs) and local cluster trigger external: EAS-array SPASEData sample: 1.3 TB raw data in ca. 250 run days in 2000

MC-data comparison at trigger and higher v-cut levels number of hit PMTs (nOM), angular-distributions, pass.-rates fit well absolute rates & vertical hit structure under study (ice, noise)

Data-analysis for AMANDA-II/2000 has started.Preliminary v -cuts developed.

Number of hit optical modules per event, nOM(dots- exper., histogram -MC).

Astrophysical sources: AGN, GRB, SN-shells, topological defects,... with spectra much harder than v‘s generated in the atmosphere

Assume a diffuse AGN E-2 spectrum: 10-6 E-2 GeV sr-1 s-1 cm-2

Trigger level acceptance of vμ and v e Charged Current (CC) and Neutral Current (NC) interactions:

Neutrino energy spectrum for events, triggering

AMANDA-II: CC vμ-events (thick lines) and CC ve-

events (thin lines) for atmospheric neutrinos (full lines) and AGN like neutrinos (dashed-dotted lines).

Zenith angle distribution for atmospherci nmu MC events in AMANDA-II (full line), compared to AMANDA-B10 detector (dashed). Preliminary cuts, normalized for vertical bin.

AGN

Atm

The various analog OMs used in AMANDA-II: electrical and fiber readout modules, and the digitally controlled module (from left to right). For Digital OM see H.E.2.05

An AMANDA-II v-candidate close to the horizon,May 2000.

vμ

AMANDA-IIAMANDA-II

AMANDA-B10AMANDA-B10

Triggered events / year Atmospheric AGNvμ 11000 (CC) 130 (NC) 853 (CC)

ve 162 (CC) 9 (NC) 103 (CC)