Condor application in AMANDA-II Paolo Desiati UW - Physics Department

1
Neutrino Astronomy and status of IceCubePaolo
Desiatidesiati_at_icecube.wisc.eduUniversity of
Wisconsin Madisonhttp//icecube.wisc.edu
from Quark n.36, 02/01/04
Laboratori Nazionali del Sud (INFN) 19 Settembre
2006
2
Introduction
3
neutrinos and cosmic rays

• origin of the highest energy cosmic rays
• still a mistery
• transition from galactic to extra-galactic
• at the ankle change of composition
• acceleration mechanisms hadronic or
• electromagnetic ?

4
acceleration in energetic sources

• Bottom-Up hadronic scenario
• cosmic accelerator
• p (p or ?) ? ?? X ? ?e ,?? X
• ? ?o X ? ? X
• Flux ? E?-2 (fermi acceleration)

AGN
GRB
5
cosmic messengers
6
neutrino astronomy

• neutrinos are not deflected by magnetic fields
  and are not absorbed during propagation
• for the same reason they are very difficult to
  detect need large volume and long exposures
• detection of cosmic neutrinos would demonstrate
  the hadronic nature of acceleration mechanisms
• detection of cosmic neutrinos in coincidence
  with TeV gamma rays could give insight on
  internal source mechanisms
• cosmic neutrinos should exist at least for
  perspective or guaranteed sources

7
galactic ? rays and neutrinos ?
shock wave from supernova remnants
excites surrounding molecular clouds and produce
? rays indirect evidence for the acceleration of
protons at the level required to explain galactic
cosmic rays ?
8
neutrino astronomy

• detection of neutrinos from point sources
• all-sky searches
• stacking AGN classes
• in coincidence with TeV ? ray flares
  (multi-wavelength campaign)
• in coincidence with GRB events (extra-galactic
  neutrinos)
• low energy neutrinos from Supernovæ
• neutrinos from WIMP annihilation in the Sun and
  the center of Earth

• detection of neutrinos from diffuse sources and
  from cosmological times
• neutrinos from galactic plane
• perspective neutrinos associated to
  extra-galactic cosmic rays (Waxman-Bachall upper
  limit)
• probe models for acceleration and cosmological
  evolution
• GZK neutrinos

• measurement of spectrum and composition of
  cosmic rays
• huge background of muons and irreducible
  background of neutrinos
• need to understand cosmic rays

9
IceCube Collaboration
Univ. of Alabama, USA Clark-Atlanta University,
USA Univ. of Maryland, USA University of Kansas,
USA Southern Univ. and AM College, Baton Rouge,
LA, USA University of Alaska Anchorage,
USA Institute for Advanced Study, Princeton, NJ,
USA
Bartol Research Inst, Univ of Delaware,
USA Pennsylvania State University, USA University
of Wisconsin-Madison, USA University of
Wisconsin-River Falls, USA LBNL, Berkeley, USA UC
Berkeley, USA UC Irvine, USA
Chiba University, Japan
University of Canterbury, Christchurch, New
Zealand
Université Libre de Bruxelles, Belgium Vrije
Universiteit Brussel, Belgium Université de
Mons-Hainaut, Belgium Universiteit Gent,
Belgium Universität Mainz, Germany RWTH Aachen
Universität, Germany
DESY Zeuthen, Germany Universität Wuppertal,
Germany Universität Dortmund, Germany Humboldt
Universität, Germany Heidelberg Universität,
Germany
Uppsala Universitet, Sweden Stockholm
Universitet, Sweden Imperial College, London,
UK University of Oxford, UK Utrecht University,
Netherland
Amundsen-Scott Station, Antarctica
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Amundsen-Scott South Pole Station
Where are we ?
Runway
South Pole
AMANDA-II
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the construction and how it works
12
the apparatus at the South pole
IceTop 160 frozen-water tanks 2 DOMs / tank
IceCube 80 strings 60 DOMs/string 17 m vertical
spacing 125 m between strings
digital sensors (Digital Optical Modules)

instrument deployed (Jan 2006) 9 IceCube
strings (540 DOMs) 32 IceTop Tanks (64 DOMs)
AMANDA-II 19 strings 677 OMs
analog sensors
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the Enhanced Hot Water Drill (EHWD)
Supply 200 GPM _at_ 1000 psi, 190 F (88
C)Return 192 GPM _at_ 33 F (0 C) Make-Up 8
GPM _at_ 33 F
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.
Thermal Power 4.5 Megawatt
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drilling holes
Top layer of packed snow is called firn. Hot
water drill designed for ice drilling it gets
starter hole from firn drill (lower right). (Top
left and top right) EHWD drill head entering hole.
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deploying IceCube strings
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deploying IceTop stations
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Digital Optical Module (DOM)
DOM Requirements

• Fast timing resolution lt 5 ns DOM-to-DOM on LE
  time.
• Pulse resolution lt 10 ns
• Optical sens. 330 nm to 500 nm
• Dynamic range - 1000 pe / 10 ns - 10,000 pe /
  1 us.
• Low noise lt 500 Hz background
• High gain O(107) PMT
• Charge resolution P/V gt 2
• Low power 3.75 W
• Ability to self-calibrate
• Field-programmable HV generated internal to unit.
• Flasher board capable of emitting optical
  pulses O(20) ns wide gt 109 ?/pulse
• 10000 psi external

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after deployment

• noise rate w/o dead time 700 Hz
• noise rate with 50 µsec dead time 300 Hz

• noise rate variations during hole re-freezing
• temperature stabilization during re-freezing

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in-ice data acquisition
DOM Mainboard
This is the core of the DAQ. It contains an
Altera Excalibur ARM CPU / 400 k-gate FPGA which
controls most aspects of the acquisition and
communications with the surface. All aspects
except bootloader program remotely
reloadable. Fast waveform capture via 1 of 2
ATWD ASICs which capture 4 ch at 200 MSPS 800
MSPS, 128 samples deep and 10-bits wide. ATWDs
operate in ping-pong mode true deadtimeless
operation possible. 3 ch are high, medium, low
gain (14-bit effective dynamic range). Slow
waveform capture from 40 MHz 10-bit FADC which
captures long slow pulses for 6.4 usec. Digital
communication to surface using electrical pairs
two DOMs per pair. Electrical penetrators more
robust. Communication bandwidth 1 Mbit.
DOM contains local free-running oscillator. DOM
DOM clock synchronization via RAPCal mechanism
which involves exchange of analog pulses from
surface to DOM and back to surface. This
coordinates local clock with global surface
clocks slaved to GPS-driven master.
DFL measurements (easy synchronous source) and
measurements in the ice (harder no synchronous
source) along real cable indicate precision of
RAPCal mechanism is better than 2.5 ns.
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surface data acquisition

• DOMs independently collect and buffer up to 8k
  waveforms.
• DOM communication handled at surface by DOR card
  hosted by standard industrial PCs called
  DOMHub.
• Beyond Linux driver DAQ software is a distributed
  set of Java applications.
• Data is time coordinated and sorted by processing
  nodes which may in future perform data reduction.
• Triggers take sorted streams request to event
  builder to grab data from string processors and
  IceTop data handlers to make events.
• Note data from deep-ice and surface arrays
  participate in triggers and are bundled together
  at event level.
• Online filter at pole selects interesting
  events for transmission north over satellite
  (limited bandwidth).
• All data taped raw data rate currently 70 GB /
  day.

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local coincidence modes
DOMs contain 2 wire pair (UP, DN) for exchanging
LC signals between adjacent DOMs on string. DOM
FPGA trigger logic can abort waveform capture on
absence of one or both signals. LC signals are
binary-coded digital DOMs can relay LC info
thru in this manner LC can span up to 4 DOMs
distant in either direction. IceCube currently
running in NN mode that is DOM trigger requires
adjacent hit (red circles) as shown in case A
to right. In this mode B and D would not
trigger, C would trigger only 1 and 2 and reject
4. This has advantage of (a) dramatically
reducing amount of data sent over 1 Mbit link to
surface (see figure) and (b) makes array
virtually noiseless. Disadvantage is that real
photon hits are lost in ice. IceCube baseline
operate in soft LC mode waveforms suppressed
/wo/ LC requirement, all hit timestamps (12
bytes) sent to surface.
A
B
C
D
(IceTop configured so that UP/DN neighbors are 2
DOMs in conjugate station).
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single photoelectron with AWTD
10 pulses are superimposed

• single photoelectron pulses (SPE) recorded in 6
  DOMs during the final acceptance test.
• All PMT gains are set to 1E7.
• Threshold at 0.3 SPE
• FWHM13.6 ns

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pulse shapes taken in situ

• Pulse shapes are recorded with three ATWD
  channels for high dynamic range coverage
• Runs of 10 flasherboard pulses at 5 different
  brightness settings are shown.
• High saturation in channel 0 (high gain), but
  good coverage of the brightest pulses in channel
  2 (low gain).

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ATWD and FADC

• Pulse shapes are recorded with ATWD and with
  FADC.
• Shown is an average flasher pulse and a single
  shot superimposed at 125 m distance.
• The ATWD captures 400 ns of this pulse (top).
  The full waveform is recorded in the FADC
  (bottom).

Here the flasher is 21-55 and the receiver is
29-55 (neighboring string, 125m away). This is a
50 nsec pulse, maximum brightness, six
horizontal LEDs flashing.The smooth curve shows
the average of several thousand events.   One
example waveform is superimposed.
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2005, 2006, 2007 deployment
AMANDA
80
79
IceCube string and IceTop station deployed 01/05
74
73
72
67
66
65
IceCube string and IceTop station deployed 12/05
01/06
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58
57
56
50
49
48
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IceTop station only 2006
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40
39
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IceCube string and IceTop station to be deployed
12/06 01/07
30
29
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604 DOMs deployed to date Next year looking for
12 strings. IceTop will be backed off to remain
in line with hole deployment Want to achieve
steady state of 14 strings / season.
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event detection principle
O(km) long m tracks
O(10m) cascades
if energy is gt few TeV muon points to neutrino
direction neutrino astronomy is possible ice
properties very important
17 m
a neutrino telescope Qmn?0.65o?(En/TeV)-0.48 (3Te
VltEnlt100TeV)
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polar ice optical properties
Measurements ?in-situ light sources ?atmospheri
c muons
J. Geophys. Res. 111 (2006) D13203
Average optical ice parameters labs 110 m
_at_ 400 nm lsca 20 m _at_ 400 nm
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detailed ice properties measurement dust logger
ash layers
404nm CW laser
light blocking brushes
Geophys. Res. Lett., 32, L21815 (2005)
counter
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Calibrations
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apparatus calibrations

• time calibrations
• synchronization of DOM oscillator to surface
  clock (every 2 sec) - RAPCal
• phase correction of actual pulse wrt the latched
  clock value ( 1 tick)
• PMT transit time correction (measured every
  month) DMCal
• amplitude calibrations
• measured every month by DOMCal ATWD/FADC bin
  width (nsec) and amplitude (mV). Using gain we
  get p.e.
• geometry calibrations
• energy calibrations
• IceTop calibrations (VEM Vertical Muon
  Equivalent)

31
time calibration RAPCal synchronization
Time
In-ice DOMs
IceTop
IceTop
404nm CW laser
light blocking brushes
counter
32
time calibration flasher events
6 vertical LED _at_top
Photon arrival time difference between DOM45 46
6 horizontal LED _at_bottom
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absolute DOM calibration golden DOM
Quantum efficiency Collection Efficiency
Map
University of Chiba
4p scan using 380nm LED mounted orthogonal to
surface of the DOM
PMT/DOM absolute calibrated with 337nm nitrogen
laser in Rayleigh scattering experiment
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absolute calibration light sources standard
candle

• 337 nm pulsed nitrogen laser
• Reflective cone resembles Cascade
• Cascade source with absolutely
• known intensity for each pulse
• Equivalent cascade energy of 1-10PeV
• In-ice energy calibration
• Contains internal, absolutely calibrated
• PMT for measuring the laser brightness
• for each pulse

Golden DOMs Standard Candle provide absolute
in-ice calibration chain
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Neutrino Astronomy at the South Pole
404nm CW laser
light blocking brushes
counter
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backgrounds
?µ fluxes from CR ? background for ET
neutrinos conventional, prompt
intense muon flux from CR ? background for CR
neutrinos
ET neutrinos as excess of measured neutrino flux
at high energies (? E-2)
(statistical errors)
404nm CW laser
Preliminary
light blocking brushes
5.0
50.0
500.0
5,000.0
Eprim (TeV)

• uncertainties on CR spectrum composition
• uncertainties on hadronic interaction models
• atmosphere properties
• ice optical properties

counter

• µ background (106 times ?µ events) in form of
• mis-reco atmospheric bundles (103 times ?µ
  events)
• coincident events (10
  times ?µ events)

37
cosmic ray measurement in AMANDA-II
Astrop Phys 21, 565, (2004)

• mass-independent high resolution primary energy
  measurement
• probing relative change of muonic energy to
  electromagnetic energy in the shower
• method robust against systematic
• uncertainties
• data are consistent with an
• increase of cosmic ray mass
• composition at the knee, between 500 TeV and 5
  PeV.

404nm CW laser
light blocking brushes
SPASE2-AMANDA-B10 3.310-5 km2 sr 0.01 of
IceTop/IceCube
Direct measurements
counter
38
IceTop
404nm CW laser
light blocking brushes
counter
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IceTop sim vs exp
Data events located within 50m from the
geometric center of the 16-station
array Simulation dN/dEE-2.76, 60TeV-20PeV
proton showers
A
B
404nm CW laser
C
light blocking brushes
counter
40
IceTop/IceCube coincidence events
_at_ surface _at_ sea level
_at_ depth _at_ high altitude
by Ralph Engel
41
IceTop/IceCube coincidence events
by Ralph Engel
IceTop-IceCube
SPASE-AMANDA-II
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atmospheric ?µ measurement

• energy-dependent uncertainties on primary cosmic
  ray spectrum and composition
• uncertainties on hadronic interaction models

43
all-sky search for point sources
2000-2004 data set
1001 effective days
1997 ApJ 583, 1040  (2003) 2000 PRL 92,
071102 (2004) 2000-02 PRD 71 077102
(2005) 2000-04 in preparation.............
IceCube Astrop Phys 20, 507 (2004)
Final neutrino sample Final neutrino sample 4282 events
Atm-?µ simulation 3627 4912 events 3627 4912 events

• background estimated from exp data with random a
  (i.e. time) blindness
• signal obtained from full simulation
• obtain best sensitivity (average upper limit
  with FC prescription)

44
all-sky search for point sources
Largest fluctuation 3.7s at 12.6 h, 4.5
69 chance probability for gt3.7s
90 confidence level flux upper limits for the
northern hemisphere in 0.5 deg bins (15 sys)
45
point sources sensitivity

• sensitivity for an E-2 neutrino spectrum

• no signal detected
• upper limits determined for
• different modeled spectra

2000-04 preliminary
2000-04 preliminary
2000-04 preliminary
angular resolution 2.25 - 3.75
46
candidates of point sources
Source Events observed/ background (2000-2004) Excess parameter -log10 P Flux upper limit (15 sys, 7 stat) F0 _at_ 90 CL 10-7 GeV cm-2s-1 for F F0 E-2 Flux upper limit (15 sys, 7 stat) F0 _at_ 90 CL 10-7 GeV cm-2s-1 for F F0 E-2
F0 (?µ ) F0 (?µ ?t ) (11)
Markarian 421 6 / 7.37 0.13 0.42 0.74
Markarian 501 8 / 6.39 0.51 0.85 1.47
1ES1959650 5 / 4.77 0.29 0.78 1.35
M87 6 / 6.08 0.25 0.49 0.87
3C273 8 / 4.72 0.98 1.00 1.80
SS433 4 / 6.14 0.06 0.27 0.48
LSI 61 303 5 / 4.81 0.28 0.74 1.26
Cygnus X-1 8 / 7.01 0.39 0.77 1.32
Cygnus X-3 7 / 6.48 0.50 0.68 1.18
Cassiopeia A 5 / 6.00 0.15 0.51 0.89
Crab Nebula 10 / 6.74 0.84 1.02 1.78
AGN
Microquasar
SNR

• 32 sources in candidate list
• No significant excess, no indication for a
  neutrino source
• Systematic error of 15 on signal prediction
  included in limits

47
if point sources are too weak ?

• single steady point sources may not be strong
  enough
• bigger detector and longer exposure
• correlation with steady TeV gamma sources
• stacking of classes of possible point sources
• paper in preparation (2000-04)

1997 ApJ 583, 1040  (2003) 2000 PRL 92,
071102 (2004) 2000-02 PRD 71 077102
(2005) stacking Astrop.Phys. in press

• time correlation with known transient phenomena
• known active flary periods of TeV gamma sources
• coincidence with observed GRB/SGR events
• multi-wavelength campaign under development

• time correlation with any transient phenomena
• time-rolling search of excess over background
• chopped GRB
• paper in preparation

SGR 1806-20 astro-ph/0607233 (PRL) GRB 030329
astro-ph/0602481--------- astro-ph/0510336--------
-

• space correlation of events in the sky
• clustering searches
• anisotropy of neutrino events

• diffused flux of neutrinos with no space-time
  correlation
• neutrinos emitted throughout the evolution of
  Universe
• neutrinos from galactic plane
• GZK neutrinos
• paper in preparation

48
search for diffused sources
HE ?µ - tracks 2p coverage

• muon neutrino search with up-going µ
• extra-terrestrial neutrinos as E-2
• expected to dominate at high energy

49
search for diffused sources
HE ?e?µ?t - cascades 4p coverage
Astroparticle Physics 22 (2004) 127

• cascade events
• semi-contained events allows energy recolution
  of 0.1-0.2 in LogEcasc

50
search for UHE diffused sources

• Earth opaque to PeV neutrinos ? look up and
  close to horizon
• Look for very bright events (large number of
  multiple hits / sensor)
• Train neural network to distinguish E-2 signal
  from background

UHE ?e?µ?t4p coverage
simulated UHE event in AMANDA-B10
Astroparticle Physics 22 (2005) 339
51
neutrino telescope effective area
?µ from point sources
?µ from diffuse sources
AMANDA-II (2000-2004)
AMANDA-II (2000-2003)
angular resolution 2.25 - 3.75
IceCube PRELIMINARY
52
neutrino telescope effective area
GRB030329 at d21.5
point source search 2000-04
IceCube PRELIMINARY
from VERITAS astro-ph/0507445
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neutrino flavor identification
Tau Neutrinos Regeneration earth
quasi-transparent to nt Enhanced m cascade
flux due to secondary nm, ne
54
to conclude

• AMANDA has seen no signal but produced good
  limits
• IceCube will improve statistics, resolutions and
  will increase energy coverage
• new simulation on-line and extended sensitivity
  studies on the way
• data coming from 9 strings and array increasing
  every year
• IceTop will measure spectrum and composition of
  cormis rays
• detector study and data analyses under way
• data coming from 16 tanks
• neutrino-gamma ray physics need collaboration
  and theoretical development
• 21-23 strings/stations to be deployed this
  season
• detector is very stable (only 3 DOMs are not
  comunicating now)

55
Extra Slides
56
Event detection in the iceperformance of
AMANDA-II
a neutrino telescope Qmn?0.65o?(En/TeV)-0.48 (3Te
VltEnlt100TeV)
event reconstruction by Cherenkov light timing
Events pointing resolution Energy resolution slog10(Eµ/TeV) coverage
m tracks 1.5º - 2.5º 0.3 0.4 2p
cascades 30º - 40º 0.1 0.2 4p
cosmic rays SPASE combined lt 0.5º 0.06 0.1 -
Nucl. Inst. Meth. A 524, 169 (2004)
57
simulation agreement
IceCube 9 strings exp vs sim
CORSIKA
Experiment
simulation reproduces well the detector
response studying observable performance at high
selection levels
? reconstructed (rad)
CORSIKA
Experiment
CORSIKA
Experiment
number of hit DOMs
f reconstructed (rad)
58
stacking of point sources

• GeV blazars (EGRET) GeV
• Unidentified EGRET sources unidGeV
• Infrared sources IR
• HAEO-A-detected keV sources keV(H)
• ROSAT-detected keV sources keV(R)
• TeV blazars - TeV
• Compact Steep Spectrum and Giga-
• Hertz peaked sources CSS/GpS
• FR-I galaxies including M87 FR-I(M)
• FR-I galaxies without M87 FR-I

2000-04 preliminary
59
neutrinos from GRB
Observations 2000 data
1997-2000 flux limit at Earth for 312 BATSE
triggered bursts E?2F? lt 4x10-8 GeV cm-2 s-1
sr-1 for Waxman-Bahcall-type spectrum with
Ebreak100 TeV, G 300
Year NBursts NBG, Exp NObs Event U.L.
2000 44 (BT) 0.41 0 2.05
2000 26 (BNT) 0.24 0 2.19
2000 44 (IPN) 0.60 0 2.01
2000 88 (BTIPN) 1.02 0 1.61
2000 114 (All) 1.25 0 1.47
404nm CW laser
light blocking brushes
BT BATSE Triggered BNT BATSE Non-Triggered
IPN InterPlanetary Network
counter
60
neutrinos from GRB
Preliminary Results of 2001-03 Analysis
Year Nbursts (BTIPN) NBG, Exp NObs Event U.L. MRF MRF (Sensitivity)
2001 Precursor 15 15 0.06 0.05 0 0 2.38 2.39 64 66
2002 Precursor 17 17 0.08 0.06 0 0 2.36 2.38 54 54
2003 Precursor 19 18 0.10 0.06 0 0 2.34 2.38 52 54
01-03 Precursor 51 50 0.24 0.16 0 0 2.19 2.28 16 20
00-03 139 1.25 0 1.47 5 10
404nm CW laser
light blocking brushes
Relative to W-B model, modified for ? oscillation
counter
61
GRB 030329
404nm CW laser
light blocking brushes
counter
62
404nm CW laser
light blocking brushes
counter
63
search for diffused sources
Results of ?µ Diffuse Analysis in the TeV PeV
Range
NChannel Cut Number of Bgd. Expected Number of Signal Expected Median upper limit Sensitivity Data Observed Event Upper Limit Model Limit
E-2 100 6.09 66.7 5.84Fmodel .088 6 5.84 .088Fmodel
SDSS 139 1.16 1.74 3.24Fmodel 1.9 1 3.24 1.9 Fmodel
MPR AGN 139 1.16 1.42 3.24Fmodel 2.3 1 3.24 2.3 Fmodel
Charm D 71 27.52 26.15 8.66Fmodel 0.33 37 24.13 0.92Fmodel
Charm C 71 27.52 16.05 8.66Fmodel 0.54 37 24.13 1.5 Fmodel
Naumov 71 27.52 4.74 8.66Fmodel 1.8 37 24.13 5.09Fmodel
Martin 71 27.52 0.41 8.66Fmodel 21.1 37 24.13 58.9Fmodel
Starburst 71 27.39 1.05 8.75Fmodel 8.3 37 24.72 23.5Fmodel
Ahlers et al. 71 27.39 1097.5 8.75Fmodel 0.01 37 24.72 .023Fmodel
64
n telescope all-flavor summary

• limits on E-2
• would need to model
• other spectra
• oscillations accounted
• _at_ Earth
• all-flavor limits / 3

?e (cascades B10 1yr)
all-flavor limits
?µ (B10 1yr)
?e?µ?t (UHE B10 1yr)
?µ (A-II 1yr)
?e?µ?t (cascades A-II 1yr)
?µ (A-II 4yr)
?e?µ?t (UHE A-II 1yr)
sensitivity
limit
65
IceCube sensitivities
Diffuse nm sensitivity
Point source nm sensitivity
Astropart.Phys. 20 (2004) 507-532
66
search for diffused sources galactic plane
summed over galactic longitude 33 to 213
systematic uncertainty of 30 on atm. ?
flux Energy range 0.2 to 40 TeV

• muon neutrino from galactic plane
• simple model based on density profile

(GeV-1 cm-2 s-1 rad-1)
On-source region On-source events Expected background 90 event upper limit Line source limit Diffuse limit Gaussian limit
?2.0º 128 129.4 19.8 6.3 ? 10-5 6.6 ? 10-4
?4.4º 272 283.3 20.0 4.8 ? 10-4
67
search for diffused sources summary
AMANDA-II (Units GeV s-1 sr-1 cm-2)
Fully reconstructed, (mostly) throughgoing, upward muons. Aµeff (10 TeV) 40000 m2 E2 F(?µ, 1 yr) lt 2.6 x 10-7 100 lt E lt 300 TeV (unfolded) 4 yr. Sensitivity. E2 F(?µ) lt 8.8 x 10-8 16 TeV lt E lt 2 PeV (90)
Contained cascade events, good energy reconstruction. Veff 0.001 km3 _at_ 10 TeV 50 TeV lt E lt 5 PeV E2 F(?all,174 d) lt 8.6 x 10 -7
Contained Non contained events all flavors, focus on energy reconstruction (systematics!) A ?eff (100 PeV) o(100m2) Egt 10 PeV E2 F(?all) lt10-6 (2000)