tyce deyoung penn state university for the icecube collaboration june 22, 2007 icecube recent...

June 22, 2007

Tyce DeYoung Penn State University

for the IceCube Collaboration

IceCubeRecent Results and Prospects

Rome International Conference on Astroparticle Physics

The IceCube CollaborationThe IceCube CollaborationUniversity of Alaska, AnchorageUniversity of California, BerkeleyUniversity of California, IrvineClark-Atlanta UniversityUniversity of Delaware / Bartol

Research InstituteUniversity of KansasLawrence Berkeley Natl. LaboratoryUniversity of MarylandPennsylvania State UniversitySouthern University and A&M

CollegeUniversity of Wisconsin, MadisonUniversity of Wisconsin, River Falls

RWTH AachenDESY, ZeuthenUniversität DortmundMPIfK HeidelbergHumboldt Universität, BerlinUniversität MainzBUGH Wuppertal

Stockholms UniversitetUppsala Universitet

Vrije Universiteit BrusselUniversité Libre de

BruxellesUniversiteit GentUniversité de Mons-

Hainaut

Chiba University

University of Canterbury, Christchurch

Universiteit Utrecht

Oxford University

June 22, 2007RICAP 2007 Tyce DeYoung

OutlineOutline

• The IceCube Detector– Design– Construction Status

• Recent Results– AMANDA– IceCube

• Scientific Prospects

AMANDA

Eiffel Tower

Svenska DagbladetDigital Optical Module

(DOM)

currently instrumentedIceCubeIceCube

4800 DOMs on 80 strings

160 Ice-Cherenkov tank surface array (IceTop)

Surrounds existing AMANDA detector (677 OMs)

22 strings deployed in 3 construction seasons

IceTop


The Digital Optical Module (DOM)The Digital Optical Module (DOM)

• Onboard capture of PMT waveforms– 300 MHz for ~400 ns with custom chip– 40 MHz for 6.4 µsec with comm. fast ADC

• Absolute timing resolution < 2 ns (RMS)• Dynamic range ~1000 p.e./10 ns• Deadtime < 1%• Noise rate ~700 Hz (260 Hz w/ artif. deadtime)• Failure rate < 1%

• Onboard capture of PMT waveforms– 300 MHz for ~400 ns with custom chip– 40 MHz for 6.4 µsec with comm. fast ADC

• Absolute timing resolution < 2 ns (RMS)• Dynamic range ~1000 p.e./10 ns• Deadtime < 1%• Noise rate ~700 Hz (260 Hz w/ artif. deadtime)• Failure rate < 1%

Digitized Waveform

20

IceTopIceTop

See talk by Tilo WaldenmaierSee talk by Tilo Waldenmaier


IceCube + AMANDAIceCube + AMANDA• Densely

instrumented “Inner Core”

• Lower energy threshold

• 7 IceCube + 18 AMANDA strings

• 225 DOMs + 540 OMs

• Outer IceCube strings form veto volume

InnerCore

veto

IceCube Construction StatusIceCube Construction Status

AMANDA 01/ 2000

IceCube string and IceTop station 01/06

IceTop station only 2006

21

3029

40

50

3938

4748

49

595857

6667

74

65

73

78

46

56

72



2004/05: 12005/06: 82006/07: 13 (12 planned)2007/08: 142008/09: 142009/10: 142010/11: 11+

Drilling Performance 2007Drilling Performance 2007

Drill dow

n

Ream

hole

40 hours!


Integrated ExposureIntegrated Exposure

• 1 km3∙yr by early 2009

• Close to 4 km3∙yr after one year of operations with full detector

0

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

2005 2006 2007 2008 2009 2010 2011 2012

Date

0

10

20

30

40

50

60

70

80

km3·yr Strings

0

0.5

1

1.5

2

2.5

3

3.5

4

4.5

5

2005 2006 2007 2008 2009 2010 2011 2012

Date

0

10

20

30

40

50

60

70

80

km3·yr Strings


OutlineOutline


• Recent Results– AMANDA (See talk by Kirsten Münich)– IceCube



AMANDA Atmospheric NeutrinosAMANDA Atmospheric Neutrinos

preliminary

K. Münich

Limit based on only 2000 data:

E2 <2.6·10-7 GeV/cm2s

sr

Unfolded neutrino energy spectrum

based on observed muon

energies

(807 days)

AMANDA Sky Map

Random events

2000-2004 data

Significance /

Significance /

69 out of 100 sky maps with randomized events

show an excess higher than3.7

4282 neutrino candidates selected

purity 95%

Achterberg et al. 2007, astro-ph/0611063

event selection optimized for both dN/dE ~E-2 and E-3 spectra

source

nr. of events

(5 years)

expectedbackground

(5 years)

E-2 flux upper limit (90% c.l.)

[10-11 TeV-1 cm-2 s-1]

Markarian 421 6 7.4 7.4

M87 6 6.1 8.7

1ES 1959+650 5 4.8 13.5

SS433 4 6.1 4.8

Cygnus X-3 7 6.5 11.8

Cygnus X-1 8 7.0 13.2

Crab Nebula 10 6.7 17.8

3C 273 8 4.72 18.0

No significant excess observed

Search for neutrinos from 32 candidate sourcesSearch for neutrinos from 32 candidate sources

crab

Mk421Mk501

M87

Cyg-X3

1ES1959

Cyg-X1

SS433

3C273

€

μ +τ

1.2equiv.

(randommaps) Achterberg

et al. 2007,astro-ph/ 0611063

IceCube Neutrino ObservationsIceCube Neutrino Observations

• 9-string data (2006)

• Cosmic ray background seen with weak cuts

• Atmospheric neutrinos seen with strong cuts

• Agreement in event rate over 6 decades

Final Cuts

cosmic ray m

uonsatmos. neutrinos

Achterberg et al. astro-ph/0705.1781


IceCube-9 NeutrinosIceCube-9 Neutrinos• Residual background near

horizon (~10% of total set)• Peaks in azimuth along

detector long axis

Zenith Angle

Azimuth

Achterberg et al. astro-ph/0705.1781


OutlineOutline


• Recent Results– AMANDA– IceCube


W-B

IceCube 1 yr

AMANDA 2000-03

Achterberg et al., astro-ph/0705.1315

Diffuse Neutrino FluxesDiffuse Neutrino Fluxes

AMANDA UHE 2000-02 (prelim)


Point Source SensitivityPoint Source Sensitivity

QuickTime™ and aTIFF (Uncompressed) decompressor

are needed to see this picture.



T. Montaruli

IceCube 1 yr

AMANDA 2000-4

ANTARES 1 yr

MACRO:astro-ph/ 0002492

AMANDA: astro-ph/ 0611063

ANTARES (binned):E. Carmona, Ph.D. thesis

IceCube:astro-ph/ 0305196


IceCube Muon ResponseIceCube Muon Response

• Simulations and analysis techniques based on AMANDA

• Big improvements possible – waveforms, more hits, better noise reduction, reconstruction techniques

cos

Aef

f / k

m2

cos

Muon Energy ResolutionMuon Energy Resolution





0.3 in log10(E)

low stochastic loss rate – use muon range?

saturation – can

be correctednew method

Zornoza, Chirkin et al. ICRC 2007

total charge

Nchannels


Extremely High EnergiesExtremely High Energies

5 year search for muon events depositing more than 10 PeV in the detector

Detector response not yet included!

S. Yoshida et al. astro-ph/0312078

GZK (hard, strong evol.) Kalashev et al. 2002GZK (standard) Yoshida & Teshima ’93TD - Sigl et al. 1999Z-burst – Yoshida et al. 1998

A Distant GRB

HAWC

IceCube

γ, ν

ν

Swift, GLAST, HETE, etc.)

Timing/localization from satellites & ground-based detectors for neutrino

searches

Neutrinos from GRBs, AGN, and supernovae

ROTSE

IceCube alerts to TeV ACTs, robotic optical telescopes?

MAGIC


MeV Supernova NeutrinosMeV Supernova Neutrinos

DOM counts integrated over 10s

Significance of observation vs distance

IceCube

AMANDA

Visibility out to Large Magellanic Cloud (~5 signal)

Signal at LMC:52 kpc

L. Köpke

AMANDA

Eiffel Tower

Svenska Dagbladet

New CapabilitiesNew Capabilities IceTop

• IceCube will be a factor of ~60 larger than AMANDA (instr. volume)

• Better events, not just more events– Fully contained,

well away from edge of detector

– More of event observed

AMANDA


Low Energy PhysicsLow Energy Physics

5400IceCube

only

8200 incl.

AMANDA

Preliminary

Atmos. μ per 200 days(trigger level,

IC22+AMANDA)

Gross et al. ICRC 2007

30 GeV!

Akhmedov, Maltoni & Smirnov, hep-ph/0612285

102

Indirect WIMP detectionIndirect WIMP detection

Sun

Krauss, Srednicki & Wilczek, ’86 Gaisser, Steigman & Tilav, ’86

Silk, Olive and Srednicki, ’85Gaisser, Steigman & Tilav, ’86Freese, ’86

μ

Detector

μ

velocitydistribution

scatt

capture

annihilation

interactions

int. μ int.

→ cc ,bb ,tt ,τ+τ−,W±,Z0,H±H0

annihilation channels


Solar WIMP SensitivitySolar WIMP Sensitivity

AMANDAlimits (144

days, 2001):

astro-ph/0508518

current AMANDA

limits

soft decay spectrum

hard spectrum

Expected sensitivity with IC22 + AMANDA

Expected sensitivity

for 1/2 year: Lic. thesis,

G. Wikström

Preliminary

Prompt Neutrino FluxPrompt Neutrino Flux

Muon neutrinosElectron neutrinos

“prompt” neutrinosfrom charm decay

“prompt” neutrinosfrom charm decay

T. Montaruli


Tau Neutrino DetectionTau Neutrino Detection

• Negligible intrinsic tau neutrino flux from accelerated hadrons

• Oscillations over astrophysical distances lead to flavor equality (we think)

• Essentially zero physics background to astrophysical tau neutrinos at relevant energies

« 1 yr-1 above 1 PeV (TDY, Razzaque & Cowen 2007)

– Only background is misidentified events


Tau Neutrino SignaturesTau Neutrino Signatures

τ

τ

ττ decay

N“Double Bang”

Learned & Pakvasahep-ph/9405296

τ

τ“Lollipop”

Beacom et al.hep-ph/0307025

τ

μ “Sugar Daddy”TDY, Razzaque

& Cowenastro-ph/0608486

τ decay


Energy Windows by FlavorEnergy Windows by Flavor

(supernovæ)showers vs. tracks

full flavor ID

Neutrino flavor

μ

τ

e

Log10(Energy/eV)12 18156 219

e

Expect 1:1:1 from oscillations – if not…?


Beyond IceCube?Beyond IceCube?


are needed to see this picture.QuickTime™ and aTIFF (Uncompressed) decompressor


Besson et al., astro-ph/0512604

Effective volumes and number of GZK neutrinos detected per year

(ESS flux)

Very low attenuation of radio, acoustic waves in ice


I Didn’t Have Time to Talk About…I Didn’t Have Time to Talk About…• Cosmic ray composition • Diffuse extraterrestrial neutrino fluxes• Sources of ultrahigh energy cosmic rays• Neutrino point sources (AGN, microquasars, magnetars,

SNRs,…)• Neutrinos from GRBs (afterglow, precursors, choked

GRBs, neutrons)• Ultrahigh energy cosmogenic neutrinos (GZK

interactions)• Non-neutralino dark matter (Kaluza-Klein, sleptons,…)• Neutrino oscillations (13)• Tests of Lorentz invariance, weak equivalence principle• Exotic massive particles (topological defects, relic

particles)• TeV-scale extra dimensions, electroweak instantons,…• Magnetic monopoles, nuclearites, Q-balls,…• Fundamental physics with flavor ratios


ConclusionsConclusions

• IceCube construction is going well– On target for completion in 2011

• 22 IceCube strings now deployed, working well and taking data

• AMANDA analysis is continuing– Now integrated into IceCube

• First IceCube physics papers are starting to appear

• Stay tuned!

tyce deyoung penn state university for the icecube collaboration june 22, 2007 icecube recent...

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