Transcript Neutrino Physics with IceCube

Neutrino Physics with IceCube
Overview
•Design of IceCube
•Construction Status
•Current Physics Results
Erik Blaufuss
University of Maryland
for the IceCube Collaboration
THE ICECUBE COLLABORATION
Sweden:
USA:
Bartol Research Institute, Delaware
Pennsylvania State University
UC Berkeley
UC Irvine
Clark-Atlanta University
University of Maryland
University of Wisconsin-Madison
University of Wisconsin-River Falls
Lawrence Berkeley National Lab.
University of Kansas
Southern University and A&M
College, Baton Rouge
University of Alaska, Anchorage
Uppsala Universitet
Stockholm Universitet
UK:
Oxford University
Netherlands:
Utrecht University
Germany:
Universität Mainz
DESY-Zeuthen
Universität Dortmund
Universität Wuppertal
Universität Berlin
MPI Heidelberg
RWTH Aachen
Belgium:
Université Libre de
Bruxelles
Vrije Universiteit Brussel
Universiteit Gent
Université de Mons-Hainaut
30 institutions, ~250 members
http://icecube.wisc.edu
E. Blaufuss - Neutrino Physics with IceCube
Japan:
Chiba university
New Zealand:
University of
Canterbury
IceCube
• 4800 Digital Optical
modules on 80 strings
• 160 Ice-Cherenkov
tank surface array
(IceTop)
• Instrumenting 1 km3 of
Antarctic Ice
• Surrounding exisiting
AMANDA detector
– 677 Optical Modules
• Just completed 3rd
construction season
E. Blaufuss - Neutrino Physics with IceCube
IceCube at the South Pole
IceCube
South Pole Station
AMANDA
Geographic
South Pole
Skiway
E. Blaufuss - Neutrino Physics with IceCube
Dark sector
Life at the South Pole
E. Blaufuss - Neutrino Physics with IceCube
The Digital Optical Module (DOM)
•Waveforms captured on Main Board
•Each DOM self-triggering
•Custom waveform digitization at 300 MHz (~425ns)
•Commercial fADC chip at 40 MHZ (~6 usec)
•Timing calibrations with surface GPS clock to ~2ns
•Low intrinsic dark noise ~ 500 Hz (260 Hz w/ 200 sec)
•Low Power consumption: <5 W per DOM
•Large dynamic range (~1000pe/10ns)
•Main board software is reprogrammable
•Self calibrating
•Very robust design: Failure rate <1%
Noise characteristics of modules
very low PMT random noise due to low temperature
correlated noise due to radioactivity driven fluorescence in glass
AMANDA
correlated
noise
suppress correlated noise
by artificial deadtime O(200μs)
IceCube noise rate distribution:
9 IceCube strings
mean ~ 260 Hz
width ~ 30 Hz
Poissonian
expectation
E. Blaufuss - Neutrino Physics with IceCube
rate [kHz]
IceCube calibrations
LED Flashers
Standard Candle
E. Blaufuss - Neutrino Physics with IceCube
Drilling and Deployment
E. Blaufuss - Neutrino Physics with IceCube
E. Blaufuss - Neutrino Physics with IceCube
Deployments
2005: 1
2006: 8
2007: 13 (12 planned)
2008: 14
2009: 14
2010: 14
2011: 11+
AMANDA 01/ 2000
78
74
73
72
67
66
65
59
58
57
56
47
50
49
48
IceCube string and
IceTop station 01/05
46
40
39
38
30
29
21
IceCube string and
IceTop station 01/06
IceTop station
only 2006
IceCube string and
IceTop station 02/07
E. Blaufuss - Neutrino Physics with IceCube
IceCube Integrated Volume (Projected)
5
80
km3·yr
Strings
4.5
70
4
60
• Graph shows cumulative
km3·yr of exposure × volume
50
• 1 km3·yr reached 2 years
before detector is completed
km3·yr
3
2.5
40
2
# Deployed Strings
3.5
• Close to 4 km3·yr at the
beginning of 2nd year of full
array operation.
30
1.5
20
1
10
0.5
0
2005
0
2006
2007
2008
2009
2010
2011
2012
Date
E. Blaufuss - Neutrino Physics with IceCube
IceCube as a Neutrino Telescope
Angular resolution
Effective Area for Muons
Galactic
center
Muon neutrino
Electron neutrino
Tau neutrino
*Studies based on simpler reconstructions
waveform information will improve
E. Blaufuss - Neutrino Physics with IceCube
AMANDA Skymap
Significance / s
2000-2004
Largest fluctuation:
3.7s
at 12.6 h, +4.5 deg
AMANDA II data from 2000-2004 (1001 live days)
Random events
4282  from northern hemisphere
69 out of 100 sky maps
with randomized events
show an excess higher than
No significant
“hot spot”
3.7s
E. Blaufuss - Neutrino Physics with IceCube
Search for neutrinos from interesting spots
1ES1959
Cyg-X3
Mk421
Mk501
Cyg-X1
crab
M87
SS433
3C273
event selection optimized for both dN/dE ~ E-2 and E-3 spectra
expected
background
(5 years)
(5 years)
flux upper limit
F90%(E>10 GeV)
[10-8cm-2s-1]
Markarian 421
6
7.37
0.43
M87
6
6.08
0.50
1ES1959+650
5
4.77
0.78
SS433
4
6.14
0.27
Cygnus X-3
7
6.48
0.67
Cygnus X-1
8
7.01
0.76
Crab Nebula
10
6.74
1.01
source
3C273
8(1yr)
4.72(1yr)
0.99
E. Blaufuss - Neutrino Physics with IceCube
No significant excess observed
nr. of 
events
IceCube as MeV SN  detector
…first proposed by Halzen, Jacobsen & Zas, astro-ph/9512080
IceCube at 10kpc
• Takes advantage of low noise DOMs
• Ice uniformly illuminated
• Detect correlated rate increase
on top of PMT noise
• Participation in SNEWS
• Also search for High Energy …
E. Blaufuss - Neutrino Physics with IceCube
Looking for core collapse SN
Significance of observation vs distance:
signal expected at LMC:
52 kpc
Integrated over 10s
IceCube
AMANDA
Visibility up to Large Magellanic Cloud (~ 5 s signal)
E. Blaufuss - Neutrino Physics with IceCube
Atmospheric neutrinos
• Dominant background
– Point source searches
– Diffuse neutrinos
• Important calibration
“beam”
– Standard candle to
measure sensitivity to
neutrinos
– Establishes IceCube as
a neutrino detector!
E. Blaufuss - Neutrino Physics with IceCube
Atmospheric neutrinos in 2006
Data selection done online at S. Pole
and transferred by satellite North
At selected cut strength of 10:
234 up-going muon events found
MC Expectation: 225 +81/-77
(211 neutrino + 14 background)
Clean sample of neutrinos!
John Pretz, Ph.D. thesis DRUM 1903-4163
E. Blaufuss - Neutrino Physics with IceCube
Diffuse neutrinos with AMANDA
Limit on diffuse E-2 νμ flux
(15.8 TeV - 2.51 PeV):
E2Fμ(E) < 8.8 ·10–8
GeV cm-2 s-1 sr-1
E. Blaufuss - Neutrino Physics with IceCube
Other physics topics…
• Science potential with IceCube is vast…
–
–
–
–
–
Point source searches
Diffuse neutrinos
GRB neutrinos
Cosmic ray physics
Search for exotic particles and new physics
• Monopoles, WIMPs…
– Supernova neutrinos
• Very active working groups…
E. Blaufuss - Neutrino Physics with IceCube
Summary
• IceCube construction is well underway!
– More than 25% complete.
– Completed detector in 2011.
– 1 km^3*yr exposure in ~2 years
• Physics analysis already underway.
– IceCube atmospheric neutrino results
– AMANDA analysis results
– More to come…
E. Blaufuss - Neutrino Physics with IceCube
Backup material
E. Blaufuss - Neutrino Physics with IceCube
The Enhanced Hot Water Drill
EHWD designed to drill a 2450 m × 60 cm
hole in ~30 hr. Fuel budget is 7200 gal per
hole. Shown above is drill camp and tower
site (inset), both mobile field arrays.
Everything must fit into LC-130 for transport
to Pole.
Supply: 200 GPM @ 1000 psi, 190 °F
Return: 192 GPM @ 33 °F Make-Up:
8 GPM @ 33 °F
Thermal Power: 4.5 Megawatt
E. Blaufuss - Neutrino Physics with IceCube