neutrino astronomy at the south pole david boersma uw madison “new views of the universe”...

Neutrino Astronomy Neutrino Astronomy at the South Poleat the South Pole

David BoersmaDavid BoersmaUW MadisonUW Madison

““New Views of the Universe”New Views of the Universe”Chicago, 10 December 2005Chicago, 10 December 2005

10 December 200510 December 2005 David Boersma @ New Views of the UniverseDavid Boersma @ New Views of the Universe 22

Cosmic Ray SpectrumCosmic Ray Spectrum


High Energy neutrinosHigh Energy neutrinos

Neglecting absorption (uncertain) Targets: p or ambient

Beam-dump model:0 -astronomy ± -astronomy

00

pp

ee ee

e e

Berezinsky et al, 1985Gaisser, Stanev, 1985


Neutrino Neutrino DetectionDetection

μ

νμ

νμμ

X X’

W

Angle(νμ,μ) ≈ 1° (at E=1TeV)

Detected energy deposit by muon gives lower limit for energy of neutrino


Neutrino Neutrino DetectionDetection

νe,τ

X X’

W

e,τ

νμ,e,τ

X X’

Z

μ,e,τ


Optical properties of ice Optical properties of ice @SP@SP

Absorption vs and depth

dust

ice

Absorption vs and depth

dust

ice

Scattering vs and depth

bubbles

dust

Scattering vs and depth

bubbles

dust

Average optical ice parameters:AMANDA/IceCube ANTARESabs ~ 110 m @ 400 nm abs ~ 60 m @ 470 nmsca ~ 20 m @ 400 nm sca ~ 300 m @ 400 nm


Amundsen-Amundsen-Scott South Scott South Pole StationPole Station

Population:Austral Summer: ~240 peopleAustral Winter: ~60 people

South PoleDome

Summer camp

AMANDA

road to work

1500 m

2000 m

[not to scale]

IceCube

ANTARTICAANTARTICA


IceCube CollaborationIceCube Collaboration

• Universität Wuppertal, Germany• Uppsala university, Sweden• Stockholm university, Sweden• Imperial College, London, UK• Oxford university, UK• Utrecht University, Netherlands

• Universität Wuppertal, Germany• Uppsala university, Sweden• Stockholm university, Sweden• Imperial College, London, UK• Oxford university, UK• Utrecht University, Netherlands

• Universite Libre de Bruxelles, Belgium• Vrije Universiteit Brussel, Belgium• Université de Gent, Belgium • Université de Mons-Hainaut, Belgium• Universität Mainz, Germany• DESY-Zeuthen, Germany• Universität Dortmund, Germany

• Universite Libre de Bruxelles, Belgium• Vrije Universiteit Brussel, Belgium• Université de Gent, Belgium • Université de Mons-Hainaut, Belgium• Universität Mainz, Germany• DESY-Zeuthen, Germany• Universität Dortmund, Germany

• 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

• 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 (12)USA (12)Europe (13)Europe (13) JapanJapan

New ZealandNew ZealandANTARCTICA

• Chiba University, Japan• University of Canterbury, Christchurch, New Zealand

• Chiba University, Japan• University of Canterbury, Christchurch, New Zealand


AMANDAAMANDA

AMANDA-II (2000 – 200x)AMANDA-II (2000 – 200x)• 677 OMs on 19 strings677 OMs on 19 strings• Ø 200m, 500m tall200m, 500m tall• Trigger rate 80 HzTrigger rate 80 Hz• Since 2003: TWR Since 2003: TWR

AMANDA-B10 (1997-1999)• 302 OMs on 10 strings• Ø 120m, 500m tall• DAQ: TDC/ADC (surface)

AMANDA-A (1996)


time recorded on OM

AMANDA-II

μ trackspointing error : 1.5º -

2.5º σ[log10(Eμ/TeV)]: 0.3 - 0.4

coverage: 2πCascades (particle showers)

pointing error: 30º - 40º σ[log10(Ec/TeV)]: 0.1 - 0.2

coverage: 4πcosmic rays (+SPASE)

combined pointing err :< 0.5º

σ[log10(Ep/TeV)]: 0.06 - 0.1Nucl. Inst. Meth. A 524, 169

(2004)energy deposited in OM


AMANDA research topicsAMANDA research topics Steady sources of neutrinosSteady sources of neutrinos

Point sources (AGNi)Point sources (AGNi) Diffuse flux (with muons)Diffuse flux (with muons) Diffuse flux (with cascades)Diffuse flux (with cascades) Atmosphere (cosmic rays)Atmosphere (cosmic rays) Gravitationally trapped WIMPsGravitationally trapped WIMPs Magnetic monopolesMagnetic monopoles

Search for sources with time variabilitySearch for sources with time variability GRBsGRBs SupernovaeSupernovae Flaring AGNiFlaring AGNi


Point source searchPoint source searchCombined 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%)


Atmospheric Muons & Atmospheric Muons & NeutrinosNeutrinos

E deposited ≈ Nch

Get Eν and Eμ through unfolding


Diffuse fluxDiffuse flux


The first kmThe first km33 detector: IceCube detector: IceCube

60/OM string 17 m vertical distanceStrings in vertices of 125 m-side triangles


main board

LED flasher board

PMT base

25 cm PMT33 cm Benthosphere


IceCube IceCube construction construction

Jan 2005:1 string (60 DOMs)+ 4/8 tanks/ stationsdeployed2005/6 Plan(starting now!)10-12 strings24/12 tanks/stations

Full detector: 2010Full detector: 2010


High Energy muonsHigh Energy muons

Eμ = 6 PeV


ContainedContainedHigh Energy High Energy

ShowerShower

E = 375 TeV


High Energy TauHigh Energy Tau(double bang)(double bang)

E ≈ 10 PeV


Ice is a quiet detection Ice is a quiet detection mediummedium

September 2005 InIce Noise Rates

0

100

200

300

400

500

600

700

800

900

1000

0 4 8 12 16 20 24 28 32 36 40 44 48 52 56 60

String 21 DOM Position

Rate

(H

z)

Phenol

Bat

Bucatini

ConchiglieSchneider

Weisse

ErikSegersaell Gnu

OxygenDubbel

Porter

Avocado

(compare: expected ~60kHz per OM in ANTARES)


First First IceTop-IceCube IceTop-IceCube

coincidence coincidence eventevent


Conclusions & OutlookConclusions & Outlook

AMANDA showed the feasibility of AMANDA showed the feasibility of High Energy Neutrino astronomy High Energy Neutrino astronomy with ice as the detection medium.with ice as the detection medium.

IceCube will be the coolest neutrino IceCube will be the coolest neutrino telescope on Earth.telescope on Earth.

Maybe extended with acoustic Maybe extended with acoustic detectors (extension to EHE)detectors (extension to EHE)


Extra MaterialExtra Material

WIMPsWIMPs IceTopIceTopGRBGRBDeploymentDeploymentFlasherFlasher


WIMPs from the SunWIMPs from the Sun

χ + χ W+ + W- ν + ν

ν

l


WIMP limitsWIMP limits


IceTop


27.1, 10:08: Reached maximum depth of 2517 m28.1, 7:00: preparations for string

installation start9:15: Started installation of the first DOM

22:36: last DOM installed 12 min/DOM22:48: Start drop

29.1, 1:31: String secured at depth of 2450.80 20:40: First communication to DOM

IceCube’s First String: January 28, 2005


All 60 DOMs

neutrino astronomy at the south pole david boersma uw madison “new views of the universe”...

Documents