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Science Potential/Opportunities of AMANDA-II
S. BarwickICRC, Aug 2001
•Diffuse Science •Point Sources•Flavor physics•Transient Sources
Outline
• Diffuse science opportunties– Sub-PeV search– Trans-PeV search
• Search for point sources
• Effective volume and flavor physics
• Transient sources (GRBs, AGN bursts, etc)
• AMANDA-II/IceCube cooperation
• Conclusions
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AMANDA-II
AtmosphericMuon Event
1.2 km !
Am-II Performance
• Improved Aeff, especially near horizon
• Trigger – Majority trigger optimized for HE phenomena– String trigger optimized for <100 GeV ’s
• Angular resolution ~ 2 degrees
Am-II: Angular Sensitivity - atmospheric MC
TriggerLevel
After BGrejection
up horizon
Nearly uniform angular sensitivity to horizon
~200 atm per angular bin,precision calibration tool
Effective Area of Am-II
0
50
100
150
200
-1 -0.8 -0.6 -0.4 -0.2 0
Aeff
[ x10
3 m2]
Cos(theta)
E = 10 TeV
- Am II Trigger
- Am II Point Cuts
- 10 Am B Point Cuts
- Am II GRB Cuts
Aeff depends sensitively on the physics objective!
Point source sensitivity is uniform to near horizon
Diffuse Flux
10-10
10-8
10-6
10-4
10-2
103 104 105 106 107
E2
(dN/dE ) [GeVcm
-2s
-1sr
-1]
E( )GeV
- (3 )AMANDA II yr
- 10 ( 97)AMANDA B '
IceCube
3 273C
AGN Core
Absorption by Earth
. Atm
AGN Core
Convolved energy resolution
New techniques
Anticipated sensitivity
Diffuse Flux
10-10
10-8
10-6
10-4
10-2
103 104 105 106 107
E2
(dN/dE ) [GeVcm
-2s
-1sr
-1]
E( )GeV
- (3 )AMANDA II yr
- 10 ( 97)AMANDA B '
IceCube
3 273C
AGN Core
Absorption by Earth
. Atm
AGN Core
AMANDA window ofopportunity
KM3 window
New techniques
FrejusFly‘s Eye RICE
Ice3
AMANDA ()
(Baikal e)
Auger
OWL
AMANDA
Adopted from Learned and Mannheim(2000) Dotted curves are anticipated sensitivity
Auger
Am-II (up)Am-II (down, E-2)
Features for EHE search
• Am-II/B Aperture: Veff ~ 20 km3sr
• 2 years of livetime on tape
• Calibration possible using in-situ N2 laser
– Equivalent to 200 TeV cascade in energy
• Background rejection “straightforward”– Total energy and “energy flow” variables
– SPASE vetoes large at relevant ECR
Extreme High Energy Science
• Earth becomes opaque to E > 0.5 PeV
– More efficient to search in “downgoing” direction
– Most signal arrives from near the horizon
New search strategy and techniques are required
Downgoing Neutrino-induced Muon Flux
10-16
10-14
10-12
10-10
10-8
107 108 109 1010 1011 1012 1013 1014
Downgoing Muon Flux in AMANDA-B
with Eth
=106GeV
F,10^14F,GelF,ProthF,SteckF,p-gammaF,ZBurstF,pi-KF,pQCDF,SM
E ( )GeV
TD MX=1014 , =1p
& (00)Gelmini Kusenko ( 97)AGN Protheroe ( 96)AGN Stecker et al
pγ2.7
ZBurst
π, -K muons ( )Charm pQCD ( )Charm SM
Attenuation( , )Area E theta
120Filt
10 AMANDA B Sensitivity
Note: this plot is being updated-SWB
Angular distribution
10-4
10-3
10-2
10-1
100
101
102
-1 -0.5 0 0.5 1
cos(θ)
( )AGN Protheroe*100GZK
DownUp
Most events are horizontal.
EeV sources cut offvery quickly belowhorizon.
Direction providesadditional BG reject.
Point Sources of
• If spectra ~E-2, then order of magnitude improvement in sensitivity
• Search for ’s from TeV gamma sources – Limitations imposed by energy resolution
Point Source
10-10
10-8
10-6
10-4
102 103 104 105 106
E2
(dN/dE ) [GeVcm
-2s
-1]
E( )GeV
- (3 )AMANDA II yr
- 10 ( 97)AMANDA B '
IceCube3 273C
Crab
AGN Core
501 (Mk =γ)
. Atm
Atmospheric + energy resolution
Point Source
10-10
10-8
10-6
10-4
102 103 104 105 106
E2
(dN/dE ) [GeVcm
-2s
-1]
E( )GeV
- (3 )AMANDA II yr
- 10 ( 97)AMANDA B '
IceCube3 273C
Crab
AGN Core
501 (Mk =γ)
. Atm
Focus onMk501 asexample
Mk501 Limits
(E-2)
• AMANDA-II can test if γ
AMANDA-II (3 yr)E-2
Non E-2 spectrum requires • larger array• Superb E
Search for from TeV γ Sources
• Milagrito all-sky search places limit at– Flux (>1 TeV) < 7 – 30 x 10-7 m-2 s-1
– 90% CL, E-2.5
• AMANDA-II probes similar flux if γ >1
Veff for AMANDA-II
• Veff ~ event rate
• Veff ( ) = 5-30 Veff(e, – Usually e, signatures are “contained events”
• Oscillation suggests comparable fluxes for all flavors
AMANDA-II provides evidence for measurable flux of e, in km3 arrays
Effective Volume of Am-II
0.1
0.3
0.5
101 102 103
<Veff
> (km
3)
E ( )TeV
Veff () is0.3-0.5 km3
•R > 10 km
Transient Phenomena
Sources– GRBs
• External trigger vs. self-trigger
• TeV vs 100 TeV
– SNa• Sensitive to full volume of galaxy
• Models for TeV emission if not toward galactic center
– AGN variability• New time scales to reduce
background
Experimental Advantages
-Reduce Atm BG
-Extend search to lower energies
-Search in downgoing direction for trans-PeV
Future: AMANDA-II +Ice3
• Combination provides best overall performance• Continuous science output during construction
– E.g., Am-II + 18 strings surrounding AMANDA-II
• ~1 km2 for GRB searches
• ~0.4 km2 for E-2 sources
• Possible DAQ upgrade for AMANDA-II– Full waveform readout– Increase trigger rate by factor of 5
Conclusions
• AMANDA-II dramatically expands the discovery space for continuous, diffuse phenomena
• Significant extension of sensitivity for point searches– Energy resolution and atm. BG limits search for
continuous emission from point sources
• Veff() much larger than e,
– Correlated probe of flavor physics
Bottom Up
• Energetics of acceleration with B-fields– Rg ~ 100 Z-1 (E/1020 eV) (B/G)-1 kpc
– E < 1018 Z (R/kpc) (B/G) eV
• Three Problems!– GZK cutoff, - no candidate accelerators within 50Mpc
– Few (if any) objects can accelerate to this energy
– Event directions do not correlate with interesting objects
Accelerate low energies to high energies
1019
1020
1021
1022
1 10 102 103 104
Energy (eV)
Distance(Mpc)
GZK Cutoff
1022 eV
1021 eV
1020 eV
p+γCMB ->π++n
Trans-GZK: way out
• New primary particles if M> 10 GeV– R-hadrons (SUSY of gluinos, quarks, gluons)
• (Problems: accelerator constraints)
– Monopoles and bound states of monopoles• (Problems: shower profile, no correlation with galaxy)
• Neutrino with >105SM
• (Problems: ad hoc, although extra-dimensions help)
• Z-burst (Weiler mechanism)– (Problems: enormous flux of at 1022 eV)