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Transcript of WP2: Physics Analysis and Simulation Objectives & Priorities Deliverables & Milestones Manpower...
WP2: Physics Analysis and Simulation
• Objectives & Priorities
• Deliverables & Milestones
• Manpower
• Optimisation considerations
P. Coyle, J. Brunner, CPPMarseille
Objectives & PrioritiesPriority Objectives
1 1 Define benchmark neutrino fluxes
2 1 Development of event selection software
3 1 Development of simulation software
4 1 Development of reconstruction software
5 1 Definition of data format, storage, distribution
6 1Comparison of detector geometries in terms of physics sensitivity
7 2Comparison of candidate sites in terms of physics sensitivity
8 1 Development of calibration strategies
Deliverables & Milestones6 months : benchmark neutrino fluxes and energy range
(+uncertainties)• Astrophysics
•sources - galactic SNR:RXJ1713, VELA-Jr
uquasars: LS5039CR interactions with gas near GC
- extragalactic AGNs, GRBs, starburst galaxies… •Diffuse flux WB bound
• Dark matter •Sun, earth, galactic centre, IMBHs
• EHE •GZK (Sigl)•Top-down models
• Exotica•monopoles, nuclearites cross-section modifications at EHE•Lorentz invariance ……•Neutrino decay•decoherence
Web page resource of relevant papers
Deliverables & Milestones
14 months : first release of simulation software packages
•Event generators•Neutrino interactions•Atmospheric muons•Muon propagation
•Detector response•Cherenkov light production•Light propagation•PMT & Front end electronics (needed dynamic range?)
•Calibrations•Timing, amplitude•Positioning, absolute pointing
Deliverables & Milestones
16 months : CDR contributions
•Description of software packages•Event generator, Detector response, Calibrations•Event selection, Reconstruction
•Scheme for data format, storage, distribution•First results on detector architecture•First results on site comparison•First results on calibration studies
Deliverables & Milestones
34 months : TDR contributions
•Description of final software packages•Event generator, Detector response, Calibrations•Event selection, Reconstruction
•Scheme for data format, storage, distribution•Final results on architecture optimization•Final results on site comparison•Final results on calibration systems
ManpowerFTEM
total
FTEM
requested
Personnel
total
Personnel
requestedtotal
IN2P3 144 72 900 354 930
CEA 250 36 650 171 821
Erlangen 36 36 193 193 (*2) 274
INFN 252 108 225112.5(+42 travel
+21.5 cons)
352
FOM 108 306 317
Sheffield 42 18 13357 (*2)(+5 travel)
172
Basic request: 1-2 position for 3 years per institute
Optimization goals
3D grid of active detector elements(distances, distribution)(string, tower, dense core, empty core)
OM orientationsPMT size, multiplicities
(e.g. large versus small PMTs)(coincidence versus high pulses)
Maximal neutrino effective area (volume) over full parameter space
Best angular resolution for neutrinosBest energy resolution for neutrinosOptimal S/B for some standard signals (E-2)
Optimization criteria
Optimization condition
Ideally: Compare various detectors which can be built and operated with the same budget
difficult to do
Or: Compare detectors withSame number of OMsSame number of floorsSame number of total eff. area of PMTs….
Choice to be made to allow fair comparison
Choice of parameter space
Which energy range ?
AstronomyPoint sources 1TeV-1PeV Diffuse flux 10TeV-10PeVGZK 1EeV-100EeV
Particle Physics Neutralinos 10GeV-1TeV
Difficult to have a detector with optimal behaviourover 8 orders of magnitude !
Separate optimisations for high/low energies?
Choice of parameter space
Which angular range ?
Classic: Upward going hemisphere Highest energies no atm. muon BG: full sphere Opacity of Earth: close to horizon calibration with moon shadow
OM arrangements depend on these choices
Downward lookingAntares likeUp/down symmetrichorizontal
Choice of parameter space
Which particle type ?
Cosmic neutrino fluxes arrive at earthwith about 1/3 fraction of e
At high energies earth opacity increases further fraction
Distinction in a neutrino telescopeCC[ (-)] long muon trackCC[e (-e,h)], NC narrow, contained showerCC[ (-e,h)] above PeV double bang
Complementary in Resolution:
Energy Angle Muon mediocre excellentShower excellent mediocre
Choice of parameter space
Site parameters influence result
Absorption length of waterLight diffusion in waterDepth (atmosph. muon background)Noise light (bioluminescence level)
Optimized detector geometry in one site might be different from detector in another site
Need feedback from WP5
For the WP2 session at 11/04 in Erlangen I would like to have a short presentation from each institute which intends to participate in this work package.
In this presentation you should:- redefine the physics and software projects to which you would like to contribute- describe the current state of this work- estimate possible contributions for the first year of KM3NET- make reference to the "Objectives" and "Milestones" of the contract document (WP2) This round of introduction talks will be followed by presentations of"first results" as some of you have already started to do KM3Net related analyses.
KM3net kickoff meeting Erlangen
Date/Time: from Tuesday 11 April 2006 (09:00) to Thursday 13 April 2006 (18:00)
Location: Erlangen
Description: Details
Tuesday 11 April 2006 14:00->18:00
Tuesday 11 April 2006 WP2 (14:00->18:00) Loc
ation:
Erlangen
14:00 Introduction (20') Paschal Coyle (CPPM)
14:20 Status+Plans CEA/DAPNIA (20') Luciano Moscoso
14:40 Status+Plans INFN (20') Marco Circella
15:00 Status+Plans NIKHEF (20') Els De Wolf (NIKHEF)
15:20 Status+Plans Erlangen (20') Rezo Shanidze (University Erlangen)
15:40 Status+Plans Great Britain (20') Fabrice Jouvenot (University Liverpool)
16:00 Status+Plans Valencia (20')
16:20 Status+Plans Greece (20')
16:40 Coffe break
17:00 KM3Net Simulations (20') Sebastian Kuch
17:20 HESS sources for KM3 (20') Christian Stegmann
17:40 Shower reconstruction (20') Ralf Auer| HELP
Organisational IssuesSteering committee institute representatives
General Mailing list, webpage
Physics benchmark fluxes
more ambitious? SA=5km2, PMs 10,000
Common software framework-ROOT, C++, java? (rewrite Km3)
Adopt antares software as standard (freely available)
Monte Carlo generation to sea level (Corsika)-geometry independent
Agree on relevant quantities for optimisation – neutrino effective area - neutrino effective volume
Optimisation-priority to muons
Reconstruction algorithms- geometry independent? (optimise pdfs?)
Site specific parameters –wp5
All data to shore vs L1 trigger
Calibration simulation-less advanced, more work? -investigate optical positioning (rather than acoustic)
Next meeting
Software Framework
Interfaces to other WPs
WP1 – Cost Model software
WP3 – simulation of front-end costs
WP4 – simulation of data filter costs
WP5 – site parameters
source Distance
(kpc)
E
(GeV)
Nμ
(km-2 yr-1 )
Reference
SNR RX J1713.7
Sgr A East
SNR RX J1713.7
6
8
6
104
105
104
~40
~140
~10
Alvarez-Muñiz & Halzen 2002
Alvarez-Muñiz & Halzen 2002
Costantini astro-ph/0508152
E Flux Sensitivity of the KM3NeT n Telescope
requirement:10 hits/event
80% duty cycle
flux
Very preliminary !
KM3NeT sensitivityestimated for
23 events flux = flux / 2
Microquasars: LS5039, LS I=61 303
LS5039 observed by HESS Index=2.12±0.15, up to 4 TeVAharonian et al, astro-ph/0508298
LS I+61 3033-5 muon type/km2/yrChristiansen et al., astro-ph/0509214
severe absorption of >100 GeV gamma-rays
( + starlight e+e-) up to a factor 10 to 100
higher initial luminosity
severe radiative (synchrotron and Compton)
losses difficult to accelerate electrons to
multi-TeV energies
Conclusion: TeV gamma-rays of hadronic origin
Extrapolation from HESS
observation: 3-6 neutrinos/yr/km2
Aharonian, Montaruli et al., Astro-ph/0508658
Interaction of CRs with Gas Clouds at GC
CR interactions in clusters of galaxies with IR photons also detectableDeMarco et al, astro-ph/0511535
AMANDA
KM3NET
CR density much higher than local density in solar systemevidence for young sourceof high energy CRs near GC-SNR?Arharonian et al, Nature 2006
neutrino signal from CR interactions detectable in KM3NET- enhancement in direction of GCCandia, Astro-ph/0505346
Measured UHECR flux provides most restrictive limit:
- optically thin sources: nucleons from photohadronic interactions escape
-CR flux above the ankle (>3 ·1018eV) are extragalactic protons with E-2 spectrum
E2F < 4.5 10-8 GeV /(cm2 s sr) Waxman & Bahcall (1999)
Magnetic fields and uncertainties in photohadronic interactions of protons can affect the bound, as these effectsrestrict number of protons able to escape Mannheim, Protheroe & Rachen (2000) CR rate evolves with z
CR rate evolves with z
Upper Bounds on Extra-Galactic fluxes
ICECUBE/KM3
MPR
CR rate evolves with z
Extragalactic: Starburst Galaxies
Radio observation of starburst galaxies imply a robust lower limit on the extragalactic neutrino background flux ~wbLoeb, Waxman astro-ph/0601695
M82 -xray
M82 -radioGalaxies undergoing large-scale star formation.-strong IR emission-strong radio emission from SNRs
Best studied: M82, NGC253
NGC253: TeV detection reported by CANGAROO
Possible source of UHECRsTorres, Anchordoquiastro-ph/0505283
3.2Mpc
Detection directe spin-independent cross-section
Télescopes a neutrino très compétitive et complémentaire au détection directe
ANTARES/KM3: Dark Matter (neutralino)
/km3e.g. mSUGRA model
A0=0, >0, tan=10,
M1/2=0-800 GeV,
M0=0-1000 GeV
+ wimph2 < 1
+ LEP constraint
efficient capture in the sun best sensitivity to spin dependent scattering
Neutrino telescope flux de soleil
Bertin, NezriOrloff 02
Dark Matter – Intermediate Mass Black Holes
Mini-spikes around IMBHsMimbh=105Msoleil
Sources concentrated towards galactic centre
Sensitive only to annihilation cross-section-complementaryTo sun search
KM3NET: 10 sources with >20 events/year
Bertonehep-ph/0603148
Armengaud, Sigl APPEC ROADMAP
Tau neutrinos
104 ly
Flavour Ratios: Experimental Signatures
E = 10 TeV E = 375 TeV
~300m for 10 PeV
e
Icecube simulationBeacom et al., hep-ph/0307025 v3 sept 2005
Horizontal MuonElectron ShowerTau (lolipop, double bang)
Particle Physics: Lorentz Violation, Decoherence
Hooper et al., hep-ph/0506091
Lorentz violationPion source
Decoherenceneutron source
Lorentz violation Atmospheric oscillations
Anchordoqui et al., hep-ph/0506168
E2 dependence
icecube
Neutron source (npee)may explain CR correlationsfrom GC & Cygnus
Anchordoqui et al., hep-ph/0510389
From angular depencenceof e/ ratio
Sudden onset
VERY LONG BASELINE
Particle Physics: Modification of (N) at High Energies
KK GravitonsTeV string resonancesscopic black holesp-Brane productioninstantons
increased cross-section
e.g. angular distribution above500 TeV in model of BHproduction astro-ph/0202081
SM
xmin=1
xmin=3
Amanda, Baikal2002
2007
AUGER
Anita
Amanda,Antares, Baikal, Nestor
2012
km3
Auger +new technologies
2004
RICE GLUE
Flux Diffus: Limites et Sensibilités
RICE AGASA
C. S
pie
ring
, J. P
hy
s. G
29
(20
03
) 8
43
Gamma Ray Bursts(Waxman & Bahcall)
Extragalacticp sources
(Mannheim et al.)AGN Jets
(Mannheim)
Topologicaldefects (Sigl)
GZK neutrinos(Rachen & Biermann)
WB98