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Multi-Messenger approach in IceCube E. Resconi

(Max-Planck-Institute for Nuclear Physics, Heidelberg)

LAUNCH, Heidelberg, 21-23 March 2007

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Multi-messenger

Phase 1:Use cosmic rays + photons information

HE neutrino sources identification (discovery !)

Phase 2:Use cosmic rays + photons + neutrinos

study hadronic interactions in astrophysical sites

cosmic ray origin

acceleration mechanisms

Elisa Resconi

CR

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Multi-messenger

Phase 1:Use cosmic rays + photons information

HE neutrino sources identification (discovery !)

Elisa Resconi

On-going activities Future (realistic) prospectives

CR

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IceCube Observables

Elisa Resconi

Arrivaltime

Incomingdirection

Estimatedenergy

AMANDA AMANDA+IceCube

~ 5-7 nsec ~ 3 nsec

2° - 3° < 1°

± 0.5 order of magnitude

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IceCube Methods

1. The diffuse flux

Proton luminosity Upper bound HE flux

K. Mannheim, R.J. Protheroe, J. P. Rachen, Phys.Rev. D63 (2001) 023003

AMANDA-II 4 yearsCosmic Rays Neutrinos

IceCube 1 year

W&B

MPR

Multi-messenger argument

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2. The point source search (time integrated)

IceCube Methods

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2. The point source search (time integrated)

AMANDA-II: 2000-2004 (1001 live days),

4282from northern hemisphere

24h 0h

15o

30o

45o

60o

75o

-3

-2

-1

0

1

2

33

2

1

0

-1

-2

No significant excess found

IceCube Methods

The IceCube coll., astro-ph/0611063,

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2. The point source search (time integrated)

IceCube Methods

Non-thermal activity Single source candidate

Multi-messenger argument

Active Galactic Nuclei

Mkn 421 6 / 7.37 0.42 Mkn 501 8 / 6.39 0.851ES1959+650 5 / 4.77 0.78

3C273 8 / 4.72 1.00M87 6 / 6.08 0.49

Nr. Observed / Nr. expected

Flux Upper Limit10-7 GeV cm-2 s-1

32 sources pre-selected

The IceCube coll., astro-ph/0611063

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2. The point source search (time integrated)

IceCube Methods

Non-thermal activity Single source candidate

Multi-messenger argument

X-ray BinarySystems

SS433 4 / 6.14 0.27LSI +61 303 5 / 4.81 0.74

Cyg X-1 8 / 7.01 0.77Cyg X-3 7 / 6.48 0.68

Nr. Observed / Nr. expected

Flux Upper Limit10-7 GeV cm-2 s-1

The IceCube coll., astro-ph/0611063

32 sources pre-selected

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2. The point source search (time integrated)

IceCube Methods

3C273

M. Ackermann, PhD Thesis

AMANDA-II Limits, 1001 days

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4. the point source search time optimized

Non-thermal activity Single source candidate

Multi-messenger arguments

Transient behavior Search for transient

Variability in astrophysics: an old problem

a plethora of methods

IceCube Methods

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4. the point source search time optimized

Phenomenology: selection of the “proxy” waveband(s)

Statistics: light curve combination / interpretation

Data Analysis: detection probability improvement

IceCube Methods

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4. the point source search time optimized

IceCube Methods

Mkn 421Mkn 5011ES1959+650

X- and -rays

3C273 Radio and X-rays

Active Galactic Nuclei

Phenomenology: selection of the “proxy” waveband(s)

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4. the point source search time optimized

IceCube Methods

SS433LSI +61 303Cyg X-1Cyg X-3…..

RadioPeriodicity (multiwavelength)

Selection of the “proxy” waveband(s)

X-ray BinarySystems

Phenomenology: selection of the “proxy” waveband(s)

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4. the point source search time optimizedStatistics: light curve combination M. Tluczykont et al., JoP 60 (2007) 318-320

IceCube Methods

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4. the point source search time optimized Statistics: light curve interpretationE.R. et al., JoP 60 (2007) 223-226

IceCube Methods

Time

Rat

eMaximum Likelihood Blocks:

Light curve … … into time intervals … in which count rate constant

(with a specified confidence)

Based on maximum-likelihood (iterative)

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4. the point source search time optimizedStatistics: light curve interpretationE.R. et al., JoP 60 (2007) 223-226

IceCube Methods

RXTE-ASMMLBsRXTE-PCA

E.R., L. Costamante, A. Gross

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IceCube Methods

Flares

Errors related to the “degree of extrapolation” Less data, more extrapolation, bigger errors Non-gaussian shape (Mkn421, Mkn501, 1ES1959+650, PKS2155) Most-Probable-Value (MPV) as characteristic level

IceCube Methods

E.R., L. Costamante, A. Gross

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IceCube Methods

Time windows of HE emission: neutrinos ??

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Good X- correlation “orphan” flare: difficult to be accommodated in leptonic models

The hint: 1ES1959+650

X-ray: ASM, PCA

-ray: Whipple

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4. the point source search time optimized

IceCube Methods

Data Analysis: detection probability improvement

P. Berghaus

Preliminary

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4. the point source search time optimized

IceCube Methods

Next tests:

Mkn501, 1997, AMANDA-B10 2005 – 2006, AMANDA-II 2007, AMANDA+IceCube23

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5.

Future Prospective

On-line Strategies

Significant NeutrinoObservation

Neutrino Trigger of Multi-wavelength Campaign

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5.

Future Prospective:prototype test

Prototype-test already done! NToT(see E. Bernardini et al …)

AMANDA – MAGIC• Alerts sent• Reaction within one day

27th September to 27th November 2006

( E. Bernardini et al., astro-ph/0509396 )

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Future Prospective

Large Field of View: ~2High Duty Cycle (60-70%)

Off-line efforts for optimal searches

CR

Multi-Messenger Arguments:

CR energetic Multi-wavelength picture of non-thermal sources Models …..

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Future Prospective

Large Field of View: ~2High Duty Cycle (60-70%)

On-line efforts: go to phase 2

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“ Perfect ” place to pursued this type of physics

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2. The point source search (time integrated)

IceCube Methods

Multi-messenger argument

The IceCube coll., astro-ph/0611063