Transcript Document

The IceCube Neutrino Telescope
Kyler Kuehn
Center for Cosmology and AstroParticle Physics
The Ohio State University
Novel Searches for Dark Matter
CCAPP
November 17, 2008
The IceCube Collaboration
USA:
Bartol Research Institute, Delaware
Pennsylvania State University
UC Berkeley
UC Irvine
Clark-Atlanta University
University of Alabama
University of Maryland
University of Wisconsin-Madison
University of Wisconsin-River Falls
Lawrence Berkeley National Lab
University of Kansas
Georgia Institute of Technology
Southern University and A&M
College, Baton Rouge
University of Alaska, Anchorage
The Ohio State University
Sweden:
Germany:
Uppsala Universitet
Stockholm Universitet
Universität Mainz
DESY-Zeuthen
Universität Dortmund
Universität
Wuppertal
Humboldt Universität
MPI Heidelberg
RWTH Aachen
UK:
Oxford University
Netherlands:
Utrecht University
Switzerland:
EPFL
Japan:
Chiba
University
Belgium:
Université Libre de Bruxelles
Vrije Universiteit Brussel
Universiteit Gent
Université de Mons-Hainaut
>30 institutions, ~250 members
http://icecube.wisc.edu
New Zealand:
University of
Canterbury
South Pole
Counting
House
AMANDA
IceCube
3
IceCube
IceTop
5
The Enhanced Hot Water Drill (EHWD)
Hose Reel
IceTop Tanks
(w/ sun shield)
Solar heated
Drill speeds ~ 2 m/minute
Facilities
~40 hours to drill a hole
~12 hours to deploy a string
Deploy: DOMs, pressure sensors, Std. Candle, dust logger, …
Drill head
6
EHWD in Action
A New Astronomical Messenger
Cutoff determined by e+e- threshold for stellar IR photons
diffuse, GRB
Cutoff determined by μG galactic B field
AGN, TD
Neutrinos open a new window onto astrophysical
processes in ways which no other particle can
Neutrino Detection
• Neutrino interacts with a nucleon
and produces a lepton
• Lepton emits Cherenkov light as it
travels through ice (in 41° cone)
• Light is detected by Digital Optical
Module (DOM)


• 35 cm pressure vessel surrounding a 25
cm Photomultiplier
• 400 ns recording time
• 3 channels gives a 14 bit dynamic range
• 1 - 2% of DOMs fail during freeze-in
• 15 year survival probability 96%
9
Neutrino Event Identification
Cascades
Tracks
IceCube
Angular
Resolution
< 1°
Muon from IC40 Data
Track-Like
IceCube
AMANDA
Cascade-Like IceCube
AMANDA
Time
Resolution
(nsec)
2
5-7
Time
Resolution
(nsec)
2
5-7
Energy
Resolution
(log10E)
0.3 – 0.4
0.3 – 0.4
Energy
Resolution
(log10E)
0.18
0.18
2π
Field of View
4π
4π
Field of View
2π
10
A Wealth of
Science
AGNs, GRBs:
cosmic
accelerators?


Diffuse Sources

?
Point Sources
GZK/UHE 
Supernovae
DM: Solar WIMPs
(see subsequent talks)
11
CRs
AMANDA Datasets
Most published physics results
are from AMANDA
completed 2000
completed 1997
In 2006 AMANDA was
merged into IceCube.
Year
2000
2001
2002
2003
2004
2005
2006
Total*
Livetime
197 d
193 d
204 d
213 d
194 d
199 d
187d
3.8 years
* Not including AMANDA B-10 (1997-1999)
12
IceCube Datasets
#Strings
Year
Run Length
CR  Rate
 rate
IC1
2005
164 days
5 Hz
~0.01/day
IC9
2006
137 days
80 Hz
~ 1.5/day
IC22
2007
319 days
550 Hz
~ 20/day
IC40
2008
~ 1year
1400 Hz
IC80
2011
10 years
1650 Hz
+
+
+
~ 200/day
IC1
IC9
IC22
IC40
13
Cosmic Ray Flux Measurement
• IceCube can measure the “background” cosmic ray μ flux
• Allows evaluation of detector simulation as well as
– Cosmic ray flux and composition around the knee
– Prompt contribution to muon flux from charm production
Atm. 
Atm.

14
Astrophysical 
Cosmic Ray
IC9 Diffuse Analysis
E-3.7
E-2
• Search for excess of unresolved neutrinos
from astrophysical sources
• Use energy based variables (NCh) to separate
astrophysical  from atmospheric 
• Preliminary sensitivity: E2 dN/dE < 1.4 x 10-7
GeV/cm2/s/sr
• Roughly comparable to limit
from AMANDA combined
4-year limit
Most stringent AMANDA limits:
≤ 106 GeV - E-2 dN/dE < 9 x 10-8 [Ap.J 675, 1014, (2008)]
> 106 GeV - E-2 dN/dE < 7.4 x 10-8 [Phys. Rev. D 76, 042008 (2007)]
15
Point Source Search
Detector
(Years)
Energy
(TeV)
Live
Time
(days)
AMANDA B-10
(1997-1999)
1 - 1000
623
AMANDA-II
(2000-2004)
1.6 - 2600
1001
AMANDA-II
(2000-2006)
1.6 -2600
1387
IceCube 22
(2007)
5 - 5000
270
IceCube 22 +
AMANDA
0.1 - 10
1657*
* Livetime varies for specific scenarios
Atm. 
Atm. 
• Search for
excess of
astrophysical
neutrinos from
a common
direction over
the background
of atmospheric
neutrinos from
the Northern
hemisphere
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IceCube Point Source Searches
IC9
• 26 a priori source
locations
• 60% of random
datasets had a sigma
higher than 3.35 no excess seen
C. Finley et al. arXiv:0711.0353 [astro-ph] p.107-110
• Unbinned likelihood
+ energy information
• Hottest spot at
r.a.153º, dec.11º
• p‐value (pre-trials):
7×10‐7 (4.8σ)
• p‐value (post-trials)
1.34% (2.2σ)
• Consistent with
background fluctuation
IC22
17
AMANDA
ν
IceCube
CGRO
γ, ν
A Distant GRB
IPN Satellites
(Fermi, Swift, HETE, ...)
GRB timing/localization information
from correlations among satellites
GRBs in AMANDA & IceCube
• AMANDA
Cascade
(Rolling)
Cascade
(Trig & Roll)
R03b
 search
R03a
R03b: Supranova model
WB03: Waxman-Bahcall model
R03a: Choked Burst model
MN06: Murase Nagataki model
  search
• Over 400 GRBs in
Northern Hemisphere
– Cascade search
• Triggered search for 73
GRBs in both hemispheres
• Rolling search for 20012003
• IceCube
– 93 SWIFT bursts during IC22
– GRB080319B: brightest
(optical) burst ever
• ~0.1  events predicted in
IC22 using fireball model
• ~1  event predicted for
equivalent burst in IC80
19
Future Plans
• Deep Core (see subsequent talks)
– Greatly enhances IceCube
sensitivity to lower energy ’s
Dust concentration
• Lower mass solar WIMPs
• Atmospheric neutrinos
– Six new strings
• 60 high QE DOMs in clear ice
• First string deployed 08/09,
• Remaining strings deployed 09/10
• Multi-messenger astronomy
– Correlations with ROTSE, AGILE,
MAGIC, and LIGO
• New Technologies
Very
clear
ice
– 3 Prototype digital radio strings
deployed with IceCube strings
– 4 Hydrophones deployed above IceCube
D. Cowen, Neutrino 2008
20
Optional Slides
Solar Physics
• IceTop is sensitive to ~GeV
particles emitted by the Sun
during outburst
• Monitor IceTop tanks rates
– Can extract energy spectrum in
1 - 10 GeV region
• Paper in preparation
IceTop Counting Rate (Hz)
Dec. 13, 2006 Solar
outburst seen by
international monitoring
network
22
CR Moon Shadow
• Select well reconstructed tracks and
look in angular bins
Real Moon
Obs. Exp.
Dummy Moons
(°)
(°)
(°)
• See a 4  deficit in the direction of the
moon in 3 mos. of IC40 data
• Independent method of calibrating
IceCube’s angular resolution
23
Flux Limits for Point Sources