tev ii particle astrophysics
DESCRIPTION
TeV II Particle Astrophysics. Summary comments. Outline. Introduction: Cosmic-ray spectrum Multi-messenger astronomy TeV astronomy g -ray astronomy n astronomy Gravitational-wave astronomy New detectors. Extra-galactic component ?. n F( n ) for cosmic rays. Air Showers. DIRECT. - PowerPoint PPT PresentationTRANSCRIPT
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 1
TeV II Particle Astrophysics
Summary comments
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 2
Outline
• Introduction: Cosmic-ray spectrum
• Multi-messenger astronomy– TeV astronomy
• -ray astronomy• astronomy
– Gravitational-wave astronomy
• New detectors
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 3
F() for cosmic rays
LHC
Tevatron
DIRECT AirShowers
Extra-galactic component ?
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1020 eV proton
16 joules energy
Kinetic energy of Yanick Noah’s second serve
But momentum of a snail
Macroscopic energy in a microscopic particle
No known astrophysicalsources “seem” able to produce such enormous energies
1/ km2/ century
3000 km2 -> 30 events / year
Simon SwordyUniversity of Chicago J. Cronin, Aug 29
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Observations I: SpectrumKnee 2nd Knee Dip GZK?
Observations – I: Spectrum
P. Blasi, Aug 28
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B. Peters on the knee and ankle
B. Peters, Nuovo Cimento 22 (1961) 800
Peters cyclePeters cycle: systematic increase of < A > : systematic increase of < A > approaching Eapproaching Emaxmax
<A> should begin to decrease again<A> should begin to decrease again for E > 30 x Efor E > 30 x Ekneeknee
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Rigidity-dependence• Acceleration, propagation
– depend on B: rgyro = R/B– Rigidity, R = E/Ze– Ec(Z) ~ Z Rc
• rSNR ~ parsec Emax ~ Z * 1015 eV– 1 < Z < 30 (p to Fe)
• Slope change should occur within factor of 30 in energy
• With characteristic pattern of increasing A
• Problem: continuation of smooth spectrum to EeV
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KASCADE composition at the knee
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UHECR
J. Cronin, Aug 29
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(de) constructing the extra-galatic spectrum
Doug Bergman et al. (HiRes), Proc 29th ICRC, 7 (2005) 315
GZK feature
recovery (depends on source density)
dip (due to pair production)
End of Galactic population (not shown)
Distant sourcesContribution depends on evolution and propagation inBextra-galactic
Nearby sources clustering, anisotropy?
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N Busca, WG-4, Aug 29 Allard et al. astro-ph/0605327
Transition at 1019 eVTransition < 1018 eV
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Where is transition to extragalactic CR? Original Fly’s Eye (1993): transition coincides with ankle
3 EeV
G. Archbold, P. Sokolsky, et al.,Proc. 28th ICRC, Tsukuba, 2003
HiRes new composition result: transition occurs before ankle
or 0.3 EeV ?
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A & B galactic components + extra-galactic Hillas, J.Phys.G 31 (2005) R95-131
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De Marco, Blasiand Olinto 2006
15 years ofOperation of Auger South
Density of sources of extra-galactic cosmic rays determines post-GZK flux
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UHE/EHE fluxes
GZK (hard, high Emax) - Kalashev et al 2002GZK (strong evolution) - ibidGZK (standard) - Yoshida Teshima 1993TD - Sigl et al 1999Zburst – Yoshida et al 1998
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Multi-messenger Astronomy
• Particle, Nuclear & Gravitational Wave Astrophysics in the decadal survey (2000)– Theme: multi-messenger astronomy (Barwick)
• Cosmic rays (Blasi, Cronin)
• Gamma-ray astronomy (Lorenz, Krennrich)
• Neutrino astronomy (Coyle, Hanson)
• Gravitational waves (Cornish, Weiss)
• Dark Matter
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Future: … transition to a ‘multi-messengers’ approach
Elisa Resconi, WG-4, Aug 29
- IceCube as a ( half ) – All-Sky-Monitor in neutrino:
- Filed of view: northern sky - High duty cycle
- Idea: use neutrinos in order to trigger gamma-ray telescopes(see E. Bernardini, “The multimessenger approach..” Barcelona, 07.06)
- Critical points under discussion:- selection of the sources: the phenomenology is limited- statistical interpretation of possible coincidences: -ray flare rate, catalogue … - blindness of the data:
minimal impact with off-line analysis
- Status: TEST run between AMANDA and Magic of 3 months approved.
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Mkn180PG1553
2006
NOT ALL SOURCES IN INNER GALACTIC PLANE SHOWN
KIFUNE PLOT
ALL SOURCES HAVE SPECTRA EXTENDING ABOVE 1 TEVRARELY SPECTRA EXTEND ABOVE 10 TEV (CRAB->80 GEVMANY AGNS HAVE A SOFT SPECTRUM
E Lorenz, Aug 28
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Study of Galactic Sources with H.E.S.S.Study of Galactic Sources with H.E.S.S.Dieter HornsDieter Horns**
for the H.E.S.S. collaborationfor the H.E.S.S. collaborationhttp://www.mpi-hd.mpg.de/hfm/hesshttp://www.mpi-hd.mpg.de/hfm/hess*Institute for Astronomy and Astrophysics, *Institute for Astronomy and Astrophysics,
Eberhard Karls Universität TübingenEberhard Karls Universität Tübingen
WG-1, Aug 28
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Madison, Aug. 29 2006TeV Particle Astrophysics II--> construct VERITAS-4 at FLWO
VERITAS-2 at basecamp of FLWO
F Krennrich
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Madison, Aug. 29 2006TeV Particle Astrophysics II
VERITAS-4 at basecamp of FLWO
Construction finished by Dec. 2006, operate 2007-2009, move in 2009F Krennrich
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 22
E Lorenz, Aug 28
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 23
SCAN OF THE NORTHERN TEV SKY BY MILAGRO
RIGHT ASC.
DECL.
6
HOTSPOT ATRA 79.6, DEC 25.8CLOSE TOEGRET 3EGJ0320+25564.5
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Madison - August 2006Jordan Goodman - The Milagro CollaborationMilagro
A Closer Look at the Galactic Plane
GP diffuse excess clearly visible from l=25° to l=90° Cygnus Region shows extended excess FCygnus ~ 2 x Fcrab
120 square degrees l (65,85), b (-3,3)
Sig
nifi
can
ce
Flux (> 12.5 TeV) = 1.59 ± 0.30stat ± 0.32sys x 10-11 cm-2 s-1 sr-1 (excluding new source & assuming E-2.6)
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 25
Chuck Dermer’s rule of thumb
“Best bet” Sources detection probability Gaisser, Halzen, Stanev 1995
Dermer & Atoyan NJP 2006
10)100/(1.0
,10)(
14
144
TeV
P
km-scale telescope (IceCube) has best detection probability near 100 TeV
Number of detected:
100 TeV
N
2424
14
2210
14
1010
/160
)(10)(
cmergscmergsN
ergs
cmergscmPN
at ~100 TeV
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 26
Is Cygnus region detectable in ?
• I (>12.5 TeV) = 1.6 x 10-11 (cm2 s sr)-1
nF(n) = E dN/dlnE = 10-4 erg / (cm2 yr)
if ( + 1) = 2.6 (differential spectral index)
• Problems– Diffuse source higher background– Factor 3 reduction due to oscillations
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 27
Chuck Dermer’s Summary
- Connection -ray fluence (extrapolated to 100 TeV) > 10-4 ergs cm-2 required for detection for optically thin sources
[ typically requires few years per source (TG) ]
Best bet for detectable neutrino point source with km-scale detector (IceCube): v from photohadronic processes
Blazar AGNs (FSRQs, not BL Lacs) [ few per year (TG) ]
Surrounding target radiation field; 1 PeV neutrinoGRBs Signatures of hadronic acceleration in GRBs [ few per year (TG) ]Microquasars (?) probably too weak
Best bet for detectable diffuse neutrino sources:GZK neutrinos from cosmological sources of UHECRs (GRBs)Cosmic-ray induced galactic diffuse emission
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Effect of oscillations
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Sensitivity to
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AMANDA
677 analog OMs deployed along 19 strings
10 strings 1997 (AMANDA B10) 3 strings 1998 (AMANDA B13) 6 strings 2000 (AMANDA II)
Analog PMT signals using electrical and optical transmission lines.
200 m diameter, 500 meters height; AMANDA II encompasses 20 Mton instrumented ice volume.
AMANDA will remain operational and form IceCube Inner Core Detector for low E physics (~ 100 GeV)
IceCube surrounding strings provide effective veto – lower background and can push AMANDA energy threshold down.
Conventional TDC / ADC technology for AMANDA has been entirely replaced by TWR system.
Beginning 2007 season, AMANDA / IceCube data streams will be conjoined; detector subsystems will share trigger information.
K Hanson
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Point Sources and Diffuse Fluxes in the IceCube Era
ave
rag
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up
per
lim
it [
cm-2s-1
]
sin
AMANDA-B10
AMANDA-II
IceCube 1/2 year
*
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08/2006 Julia Becker, Universität Dortmund TeV particle astrophysics, Madison
Model-dependence of limit
Not always E-2 Energy range of limits change with spectral
index , E-
Higher energies for flatter spectra
E-1E-3
E-2
log(E/GeV)
log
(dN
/d
E*E
2)
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IceCube Events
Neutrino Candidate Joint IceTop-InIceIceTop /w/ Reco
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Downgoing muon
M Bouwhuis WG-4, Aug 29
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Atmospheric muon bundles
M Bouwhuis WG-4, Aug 29
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 36
GW
N Cornish, Aug 30
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 37N Cornish, Aug 30
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 38
WIMP Dark Matter
World-best limit today
CDMS II 2007
SuperCDMS Phase C 1000 kg of Ge
SuperCDMS 25kg 25 kg of Ge 2011
SuperCDMS Phase B 150 kg of Ge
ZEPLIN IEDELWEISSZEPLIN 2
XENON 10
DAMA
10-45 cm2
10-47cm2
10-46cm2
Direct searches: Cabrera, Aprile Indirect searches: Ullio
Indirect searches: from Sun
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 39
New experiments for knee to ankle
• KASCADE-Grande (e / )
• Tunka (air Cherenkov)
• TALE (hybrid)
• LOPES (radio)
• IceCube ( e / energetic )– Primary E to ~1017 eV now– to ~1018 eV when complete
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FD Aperture…SD Aperture…Hybrid aperture:
Hybrid aperture is determined by FD since SD single-tank TOT trigger has low threshold.
(Observatory trigger (T3) for hybrids is initiated by the FD and tank triggers are collected)
(aperture as of October, 2004)Bellido et al. (Auger Collab) 29th ICRC HE15 (2005)
single-tank TOT
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 41
A HaungsAug 28
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LOPES & KASCADE Grande
Haungs et al. 2006; Badea et al. 2005; Apel et al. (LOPES coll.), Astropart.Phys. 2006, in press
(not corrected for geomagnetic angle)
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LOFAR @ AugerNext step: Radio @ AUGER
First on-site tests starting this fall!
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 44
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 45
Air Showers with IceCube
IceTop
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 46
2006 (16 stations + 9 strings): 0.5% of full IceCube
What we have now
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 47
Waveforms and lateral distribution
A
B
C
AB
C
X. Bai
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 48
Fluctuations:
1. Fluctuations in response of a tank to energy deposition is smaller than
intrinsic fluctuations in the shower front
Between 2 DOMs
Between two tanks
2. Using two nearby tanks, we can measure time & density fluctuations and assign the
weights in maximum-likelihood fittings.
X. Bai
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South PoleNovember 27, 2005
Tom Gaisser 49
Muon / electron ratio reflects nuclear composition of primaries
Calculations of Ralph Engel, presented at Aspen, April, 2005KASCADE-Grande
IceCube
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Astroparticle Physics:Radio Detection of Particles
Cosmic Rays in atmosphere:Geosynchrotron emission (10-100 MHz)Radio fluorescence and Bremsstrahlung (~GHz)Radar reflection signals (any?)VLF emission, process unclear (<1 MHz)
Neutrinos and cosmic rays in solids: Cherenkov emission (100 MHz - 2 GHz)polar ice cap (balloon or satellite)inclined neutrinos through earth crust (radio array)CRs and Neutrinos hitting the moon (telescope)
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Acoustic (and radio) for UHE
L Thompson Aug 30
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prel
imin
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π+π-
C.Alt et al. hep-ex/0606028
NA49: p+C @158 NA49: p+C @158 GeVGeV
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TeV II, Particle AstrophysicsMadison, Aug 31, 2006
Tom Gaisser 54
T. Han prospective of LHC era
• Hadronic physcis with cosmic rays not hopeful
• Neutrinos of more interest
• Forward physics at LHC could clarify cascade physics for CR
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2005, 2006, 2007 Deployments
AMANDA
IceCube string and IceTop station deployed 12/05 – 01/06
IceTop station only 2006
604 DOMs deployed to date
Next year looking for ≥ 12 strings. IceTop will be backed off to remain in line with hole deployment
Want to achieve steady state of 14 strings / season.
21
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595857
6667
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IceCube string and IceTop station deployed 01/05
IceCube string and IceTop station to be deployed 12/06 – 01/07