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AstroParticle Physics

PRC, May 2009Christian Spiering

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Baikal: 1988-2008 Amanda: 1995-2009 IceCube: since 2000

MAGIC (YIG): since 2006 CTA (prototype): since 2008

Astroparticle Theory starting 2009 (together with U. Potsdam)

Overview

Multi-messenger approach

total expendituresDESY/Astroparticle

IceCubeconstruction

CTA prototype construction

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MAGIC: Status, AGN Monitoring

CTA: status and plans

IceCube Construction: Status and schedule

IceCube/Amanda analysis: Selected results

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MAGIC: Status, AGN Monitoring

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MAGIC II: commissioning• Improved sensitivity

• lower threshold

MAGIC-IIMAGIC-I

Pratik MajumdarDESYYoung Invest. Group

DESY YIG contributed

HQE PMT (Helmholtz grant)

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DESY: Monitoring of bright blazars Un-biased statistics of different flux levels

Long-term flux level variability studies

Determination of flare probabilities

Studies of spectra for different flux levels

Triggers for ToO (self-trigger, other IACTs, X-ray, etc.)

Studies of correlations with other wavelengths and neutrino events

Mkn 501MAGIClong-term Light curve

Satalecka et al,SciNEGHE'08AIP Conf. Ser.in press

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CTA: Status and plans

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The Cherenkov Telescope Array

Increased sensitivity

Extended energy range

Improved angular resolution

Observatory with flexible and robotic operation

Arrays in North and South for full sky coverage

50 to 100 large, medium and small telescopes

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Sensitivity

Deep look at the TeV

sky

AGN pulsars

GRB

Galactic sources

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2006

2007

2008

2009

2010

2011

2012

2013

2014

2015

2016

2017

Design and Prototype Phase

Array layout

Components

Telescopes

Array construction

VERITAS

MAGIC II

H.E.S.S. IIFermi

Science operation

Startup meeting

FP7 proposal

Consortium

Japan will join CTAClose collaboration with AGIS (USA)

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DESY works on

12 m telescope prototype with large field of view

Drive and control and safety system Fast read-out system based on domino

ring sampler HV concept for camera Timing studies for background

suppression Trigger optimization

Detailed report

at next PRC

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IceCube Construction: Status and schedule

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IceCube

05/06: 8

Remaining: 22 IceCube Strings 5 DeepCore Strings

complete in January 2011

04/05: 1

07/08: 18

06/07: 13

08/09: 19 strings

IceCube

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IceCube/Amanda analysis: Selected results

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Shadow of the MoonShadow of the Moon

Cosmic RaysCosmic Rays

• Absolute pointing 1°• Angular resolution 1°

0.5°

5 months IC40

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relativedeviations

significance map

Large-scale anisotropyof downgoing muons recordedin IceCube

anisotropies on theper-mille scale

(skymap in equatorialcoordinates)

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MILAGRO

Compare to Northern hemisphere

Tibet air shower array

Simulation(Lallement et al.Science 2005)

• Compton-Getting effect ?

• Solar wind pressure ?• Nearby pulsar ?• Interstellar magnetic

field ?

• First observation on Southern hemi- sphere adds important piece of information.

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ICRC 2009: 42 four-page contributions, 5 from DESY- 2 x point source search- 1 x cascade search- 1 x cosmic ray with IceTop- 1 x acoustic detection technique

Journal Publications (recently published or accepted)

– Observation of solar flare with IceTop• Astrophys. Journ. 689/1 (2008) L65

– IceCube DAQ • Nucl.Instr.Meth. A601 (2009) 294

– AMANDA 7-year point source search• Phys. Rev. D79 (2009) 062001 (events available on the web)

– AMANDA 7-year atmosph. neutrinos & Quantum Gravity effects • Phys. Rev. D, accepted

– IceCube-22 WIMP search • Phys. Rev. Lett., accepted

– Naked-eye GRB080319Baked-eye GRB080319B• Astrophys. Journ., accepted

Next weeks: unblinding of many

Analyses (IC-22, IC40 first 5 months)

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Atmospheric NeutrinosSpectrum measuredup to >100 TeV

IceCube will providea few 105 atm neutrinos

- rich physics !

AMANDA

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Muon neutrino survival probability

oscillations

Neutrino Oscillations• Use large atmospheric neutrino sample, look for νμ

disappearance and appearance of

• DeepCore will help peering into the oscillation regionGoal for DeepCore: Threshold < 20 GeV

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Exotic Oscillations• Use large atmospheric neutrino sample, look for νμ

disappearance and appearance of – Violation of Lorentz

invariance– Quantum

decoherence

(both appear in quantum gravity theories)

Muon neutrino survival probability

Conventionaloscillations

VLI oscillations,δc/c = 10-27

parameters of interest:VLI: c/c, sin 2, phase QD: D3 and D8, D6 and D7

Different to standardoscillations (~ 1/E), effects of QG oscillationsgo ~ E

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Limits from 7 years AMANDA (2000-2006)

90% C.L.allowed 90% C.L.

allowed

99% C.L. excl.

99% C.L. excl.

Full IceCube(sensitivity)

Amanda4 years

QD VLI

PRD accepted and arXiv:0902.0675

99% C.L.allowed

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Indirect Dark Matter Search

SunSun

DetectorDetector

EarthEarth

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Indirect Dark Matter Search

• Amanda: – analysis with standard

point source sample (2000-2006)

– analysis with dedicated sample (2001-2003)

– similar sensitivity & limits– to be submitted in June

• IceCube-22:– PRL, accepted and

arXiv:0902.2460

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Indirect Dark Matter Search ….. apply to spin-dependent cross section

• Models with strong spin-dependent coupling are the least constrained by direct DM searches.

• W.r.t. spin-dependent coupling, Amanda & IceCube are ~100 times more sensitive than direct search experiments (Sun is mostly hydrogen)

Effect of DeepCore

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t ~ -10-100s t ~ 0 t90 t ~ t90 ?

Waxman & Bahcall, PRL 78:2292 (1997)

Waxman & Bahcall, ApJ 541:707 (2000)

Razzaque et al., PRD 68 (2003)

Neutrinos from GRB

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t ~ -10-100s t ~ 0 t90 t ~ t90 ?

Waxman & Bahcall, ApJ 541:707 (2000)

Neutrinos from GRB

AMANDA limit from 408 bursts

1997-2003

Waxman-BahcallGRB prediction

10-10

10-7

10-8

10-9

104 106105 107 108

neutrino energy E (GeV)

E2

flu

x (

Ge

Vc

m-2s

-1s

r-1)

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Neutrinos from naked-eye GRB080319BNeutrinos from naked-eye GRB080319B Duration: 70 s RA: 217.9o Dec: 36.3o z=0.94 Brightest GRB (optical) ever Large number of -ray, x-ray, UV and optical,

observations

Pi of the Sky

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Neutrinos from naked-eye GRB080319BNeutrinos from naked-eye GRB080319B Detector running in maintenance mode at the time:

9 out of 22 strings. Signal expectation: 0.1 events ( = 300) No events at GRB position/time after cut Limit

~1.5 event in full IceCube

arXiv:0902.01311

APJ accepted andarXiv:0902.0131

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Steady Point Sources

First skymaps, 22 strings, 2007

New territory:

¼ IceCube / 1 year

~ 2 full Amanda / 7 years !

Ultra-High Energies looking to Southern hemisphere

Wisconsin, DESY, Heidelberg DESY

TeV-PeV range PeV-EeV range

Separate papers on standardand HE/above horizon analysisto be submitted in June/July

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Point Sources: The Progress

factor

1000in 15 years !

point source limits/sensitivities:

Common analyseswith Antares & KM3NeT inoverlap regions

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IceCube NorthernHemisphere

IceCube CPU

Iridiumsatellites

MAGIC(VERITAS/Whipple

also interested)

AGN Flare

Neutrino Target of Opportunity with MAGIC (DESY)Neutrino Target of Opportunity with MAGIC (DESY)

Commissioning

(online trigger)

- Selected objects- Time scale of multiplets is days-weeks

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IceCube NorthernHemisphere

IceCube CPU

Iridiumsatellites

MAGIC(VERITAS/Whipple

also interested)

AGN Flare

Neutrino Target of Opportunity with MAGIC (DESY)Neutrino Target of Opportunity with MAGIC (DESY)

Commissioning

(online trigger)

Alert rates for bin radius of 2°and pre-trial thresholds of 3and 5 (for one source)

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IceCube NorthernHemisphere

IceCube CPU

Iridiumsatellites

ROTSE III

SN/GRB

Fast reactionFast reactionto GRB alertsto GRB alerts

Optical Follow-Up with ROTSE ( Humboldt/Optical Follow-Up with ROTSE ( Humboldt/DESY DESY ))

Commissioning

(online trigger)

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Further activities/results DESY IceCube-40: Off-line search for time flares

- close to unblinding IceCube-40: reconstruction of cascades

- record accuracy for energy, position & angle ! IceTop: spectrum and mass composition of cosmic

rays - first spectrum derived

Search for slowly moving particles (~10-5 -10-3):- GUT magnetic monopoles, SUSY Q-balls, strange quark

matter, ongoing work

R&D on acoustic detection - considerably improved parameters from last season,

report at next PRC

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Summary IceCube

Amanda analyses completed IceCube-22 results being published Lot of interesting results Unblinding of first 5 months IceCube-40 data within

the next weeks summer conferences Sensitivity gradient strongest within next 3-5 years

MAGIC Soon first light with MAGIC-II. YIG: AGN monitoring, low energy sources

CTA Steep start. Wide front of activities DESY well positioned Application for additional Helmholtz investment

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Check for coincidences with BATSE, IPN, SWIFT, FERMI

WB model one of the most testable astrophys. Models for IceCube

Amanda came close to WB within < factor 2

full IceCube: 95% probability to detect WB flux with 5 within 1 year

~ 10 ongoing analyses

Coincidences with GRB

AMANDA limit from 408 bursts

1997-2003

Waxman-BahcallGRB prediction

10-10

10-7

10-8

10-9

104 106105 107 108

neutrino energy E (GeV)

E2

flu

x (

Ge

Vc

m-2s

-1s

r-1)

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Different alert philosophies

• Optical follow-up: 2 events from the same direction within t (minute scale). Look to the full sky.

• NToO: n events within t (days-weeks) from directions of a few pre-defined sources with known flaring behaviour. n and t optimized to a given significance threshold (e.g. 3,5)

Alert rates for bin radius of 2°and pre-trial thresholds of 3and 5 (for one source)