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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)