Baikal-Amanda-IceCube Neutrino-Astronmie in DESY Zeuthen Christian Spiering, Technisches Seminar, Mai2004

Entdeckung der Kosmischen Strahlen 1912 Viktor Hess (Nobelpreis 1936)

Kosmische Strahlen 1 TeV (HERA)

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Neutrino-Teleskope in Wasser und Eis  

Amanda Baikal Super-K Antares Nestor Km3: IceCube

Das Baikal Experiment

3600 m 1366 m NT-200 Lake Baikal: The Site

Camp

- 8 strings 192 optische Module Zeuthen: 2 N2-Laser DAQ in Uferstation Div. Elektronik Ersatzteil-Käufe Finanz-Unterstützung

BED Wasserdicht: ~ 900 Stecker ohne Leck !!!

Eines der ersten Neutrino-Ereignisse, die mit dem Baikal-Teleskop registiert wurden. (1996)

Upgrade: NT-200+ NT-200 36 zusätzliche PMTs  4x besser Sensitivität ! cascades Upgrade: NT-200+ NT-200 140 m 36 zusätzliche PMTs  4x besser Sensitivität !

A lesson on electro-corrosion + -  40m  unexpected electro-corrosion after > 6 years

points of problems + - Two out of four cables have broken during installation works in Spring 2003. Detector runs only with 5 strings in 2003. Two new cables in March 2004.

Projekte im Mittelmeer Die Konkurrenz: 2400m ANTARES 4100m 3400m NEMO NESTOR

Neutrinoteleskope im Meer 91 92 93 94 95 96 97 98 99 00 01 02 03 04 Dumand Nestor Antares Nemo

Neumayer Amundsen-Scott Mirny Vostok Concordia Mc Murdo Dumont D‘Urville Concordia Antarktis

Südpol Dark sector Landebahn AMANDA Dome

AMANDA-II 677 optische Module an 19 Trossen Installation 1996-2000

Drilling Hot water drilling 2 MW power 3-4 days / 2 km 60 cm hole

The Counting House Counting House

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

Himmelskarte Amanda-II, 2000 697 Spuren von unten Von oben: größtenteils nicht durch Neutrinos hervorgerufen

SS-433

Close by objects Sun SS-433 Crab - Nebula Cyg-X1 LMC SMC 30 kpc = 90 000 ly

the sensitivity needed to search from neutrino fluxes 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 TeV gamma sources of similar strength to the instrinsic gamma flux.

Expected sensitivity for AMANDA 97-03 m  cm-2 s-1 southern sky northern sky 4 years Super-Kamiokande 170 days AMANDA-B10 10-14 230 days AMANDA-II 8 years MACRO SS-433 Mk-501 / ~ 1 10-15 Expected sensitivity for AMANDA 97-03 -90 -45 90 45 declination (degrees)

Search for diffuse excess of extra- terrestrial high energy neutrinos  bound WB bound DUMAND FREJUS MACRO Muons in Amanda-B10 (1997) Expectation Amanda-II, 3 years Expectation IceCube, 3 years log E /GeV

Suche nach dunkler Materie (  )   Amanda Suche nach einem Überschuss von Neutrinos aus der gegenseitigen Vernichtung von Teilchen der dunklen Materie, die vom Schwerefeld der Sonne eingefangen wurden.

Upper limits on muon flux from neutralino annihilations in center of Sun ANTARES und ICECUBE: Erwartung aus Monte-Carlo Simulationen

Relativistische Magnetische Monopole 10-16 10-15 10-14 10-18 10-17  = v/c 1.00 0.75 0.50 Soudan KGF Baikal MACRO Orito upper limit (cm-2 s-1 sr-1) Cherenkov-Licht  n2·(g/e)2 Amanda  electrons n = 1.33 (g/e) = 137/ 2 IceCube  8300

Amanda/IceCube als Supernova Monitor Amanda-II B10: 60% der Galaxis A-II: 95% der Galaxis IceCube: bis zu LMC Amanda-B10 0 5 10 sec Count rates IceCube

IceCube - 80 Strings - 4800 PMT Instrumentiertes Volumen: 1 km3 AMANDA South Pole IceTop IceCube - 80 Strings - 4800 PMT Instrumentiertes Volumen: 1 km3 Installation: 2004-2010 ~ 80.000 atm. per year

Die IceCube-Kollaboration Bartol Research Institute UC Berkeley UC Iivine Pennsylvania State UW Madison UW River Falls LBL Berkeley U. Simón Bolivar, Caracas VUB, Brussel ULB-IHEE, Bruxelles U. de Mons-Hainaut Imperial College, London DESY, Zeuthen Mainz Universität Wuppertal Universität Stockholm Universitet Uppsala Universitet Kalmar Universitet South Pole Station Antarctica New Zealand Venezuela USA (10) Europa (11) Japan

Bohren: von Amanda zu IceCube Amanda IceCube Heat (surface) 2 MW 5 MW Time to 2400 m 120-140 hours 35-40 hours Fuel (gal/hole) 10,000 - 12,000 7,000 - 8,000 Set-up Time 5-6 weeks 18-25 days

ICECUBE Drilling

winch

Digital Optical Module - (DOM)  Captures waveforms with - 250 MHz first 500 ns - 40 MHz over 5000 ns  Time-stamps each pulse - r.m.s. < 5 nsec  Dynamic range - 200 PE over 15 ns - 2000 PE over 5000 ns  Dead time < 1 %  Noise rate < 500 Hz DOM 33 cm

HV Base Flasher Board DOM Mainboard Delay Board

DOR: DOM Readout card 96V DOM Power Quad Cable Con. Power Switch Comm. DAC Clock & Time String port Comm. ADC PLD Comm. Rec. FPGA FLASH SRAM JTAG I would like to present you two examples of fast link interfaces, designed in our lab. For both cards block schemes, test results and conclusions will be presented. DOR: DOM Readout card

DOR DOM Traffic over 2 km twisted pair cable: supply voltage slow control FADC output synchro-signals ( require 5 nsec accuracy) DOM

Produktion optischer Module in Zeuthen

Room 1: preparation of components cleaning pouring

Room 2: assembly integration functionality test

1st Produktion 1.3.2004 : First DOM produced at DESY End of February: First 2 kits of electronic boards arrived at Zeuthen 1.3.2004 : First DOM produced at DESY

Dark Freezer Lab - 45 °C

Simulierte IceCube  Events Eµ=10 TeV, 90 hits Eµ=6 PeV, 1000 hits

Effektive Fläche von IceCube Aeff / km2 cos 

Expected sensitivities to steady point sources m  cm-2 s-1 Expected sensitivities to steady point sources 10-14 2001 10-15 SS-433 2003 GX 339-4 Mk-501 / ~ 1 2007 10-16 „typical“ predictions for AGN, SNR, ... 10-17 2012 -90 -45 90 45

Neutrinos hören ?

Maximum of emission at ~ 20 kHz neutrino P t 50s Schallwelle Attenuation length of cold ice at 15-30 kHz: ~ 2 km (light: ~ 100 meters)

• • • • amplitude Einfluss auf: Absorptionslänge Streulänge Schallgeschwindigkeit • • • •

180 MeV Protonen Uppsala Test-Beam

RICE AGASA Amanda, Baikal 2002 2004 RICE AGASA AUGER nt Anita AABN 2007 2012 km3 EUSO Auger Akustik?

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