Science Potential/Opportunities of AMANDA-II S. Barwick ICRC, Aug 2001 Diffuse Science Point Sources Flavor physics Transient Sources

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

Messengers of Astronomy

AMANDA-II Feb. 00

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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

Am-II MC: Energy response

After BGrejection

Aeff(E) much improved compared to AMANDA-B10

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

Upper Bounds on Diffuse Flux

AMANDA-II Anticipated sensitivity

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

Mk501

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)

Z-burst

~50 Mpc

E~1022 eVvrelic

Z0

Decays to 3N, 28π±, 15πo

Signatures:γ/p largepoints to sourcedirectional pairingmeasurable fluxE cut-off at mrelic