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2
The km3 package
• Used in ANTARES to simulate the photon detection from muons
• Code:- Fortran77 (I hate it)
- Written in the late 90s
- Documentation: various ANTARES internal notes
- Numerous updates by various authors – v2: David Bailey; v3- v4r2 Goulven Guillard, v4r3+ myself)
- v4r3 documented, v4r4 development version
• Gen, hit, km3mc:- Three separate programs
- Many interdependencies (explicit and implicit)
- Incorporate GEANT 3.21 and MUSIC
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
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Gen (physics lives here)
• Uses GEANT 3.21 to model particle interactions from an initial input (e.g. a muon)
• Generates Cherenkov photons from GEANT tracks.
• Propagates photons using (wavelength-dependent) scattering and absorption.
• Records photon properties to disk at each of several spheres.
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
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Gen geometry
C.W.James, ANTARES collaboration meeting Strasbourg, Nov 21st-24th 2011.
L = 1 m
r1 = 2 m
r 20 = 200 m
20 radial bins ~ log-spaced
*
* *
record photon properties at sphere 1
record new photon properties at sphere 2
…
• Problem: Few photons make it to the outer shells: generate many
photons
• Excess of photons on inner shells
• Solution: record a random fraction of photons, with p increasing with
r
record all photonsthat get here
Record a fraction ofphotons crossing here
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Gen output:
• Writes photon information at each shell:
- Writes only a fraction of the photons generated.
- Fraction increases with distance
(less photons make it to outer shells)
• Major disk-space requirement!- Photon statistics limited by 1 GB output file size of f77
• Currently more annoyance than a limitation: but may need to be overcome in the future.
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
6
Tables: electrons and muons
• Muons- Simulates 1 m of 100 GeV muon track
- Includes secondary electrons below 200 MeV
- Generates photons using Frank-Tamm formula
• Electrons- Photons from electron (sub) showers
- Tracks particles to Cherenkov threshold
- 4 runs: 100 Mev, 1 GeV, 10 GeV, 100 GeV
• Output: 5 x 1 GB files
• Run-time: O ~ 10 hr on a single CPU (=nothing)
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
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Major limitations to gen
• Only used to generate electron and muon tables (what about hadronic showers from neutrino interactions in the detector?)
• i/o (=f77) currently limits statistics
• Scattering and absorption models are imperfect – in situ measurements are often inconclusive.
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012.
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Hit (the boring program)
• Photon list -> summary histograms- Reads photon data from Gen.
- Creates histograms as function of distance, angles to the track segment.
- Folds in OM response (e.g. quantum efficiency of PMTs).
- Generates tables of photon-hit probabilities and hit-time distributions.
• Summary tables -> file.- Inverse cumulative time distributions & hit probabilities.
- All tables for given [gen] particle type/energyC.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
e-,100 GeV
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Histogramming (in gen and hit)
• Hit times (t)- 50 bins in time
• OM orientation (in angles θ,ϕ)- Direct: 10x1
- Scattered: 5x3
• Distance from track segment- 20 log-spaced bins in r for all photons
• Angle from track segment- 1 bin for direct photons from muons
- 20 bins for all other cases
• Emitting particle type/energy- 4 electron energies (102, 103, 104, 105 MeV)
- 1 muon energy (105 MeV)
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
Again – thanks Claudio for the figure!
+ binning scattered photons by hit
‘low’ bins‘high’ bins
θC
• OLD distribution: new distribution has a greater weighting towards the Cherenkov peak
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
10
Inverse cumulative distributions…
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
11
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Output:
• 5 files of size ~32 MB• 4 photon tables:
- Direct and scattered hit probabilities
- Direct and scattered hit times
• These are created once and used repeatedly for ANTARES simulation input
• Limitations:- Histograms are sparse (wrong choice of spacing has
caused problems in the past)
- Extremely memory-inefficient (by a factor of x30 or more)
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
Example of gen output
These are scattered photons!(most scatters are small)
Wavelength and directional information not shown)
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
13
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km3mc
• Inputs:- Hit tables
- PMT locations and orientations
- Incident particle (single muon)
• Step 1: run MUSIC- Muon propagation code
- Simulates muon interactions: muon energy-loss, and secondary EM sub-showers above 100 MeV
• Step 2: get detector hits- Interpolate between, and sample from, tables to get
photon hit times for each (2m) track segment, and each EM sub-shower
- Outputs a list of OM hit magnitudes (nphtons) and times
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
e-,100 MeV
e-,1
GeV
e-,10 GeV
μ,100 GeV
e-,100 GeV
μ
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km3mc
• A program to determine photon arrival times at optical modules from muon tracks.
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
Tables of hit probabilities & times(function of relative photon/OM geometry)
e-,100 MeV
e-,1 GeV
Source & Detectors - Incident muon (e.g. genhen) - Detector geometry (ANTARES)
e-,10
GeV
μ,100 GeV
e-,100 GeV
INPUTS to km3
Detector hits
1: generate muon & secondary tracks (use MUSIC)
2: interpolate between, and sample from, tables to get photons hits from tracks.
What km3 does
Testing km3: toy experiments
• Use simple ‘detector’ to test performance of km3
- Use a single PMT
- Fix muon energy, e.g. 1 TeV
- Use characteristic geometry
• Repeat for many (O~106) identical muon tracks
• Plot time-distribution of photon hits
d = 50 m
l = 1
00 m
Direct Cherenkov photon path (430 nm)
74 m
θC
45 m
PMT
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
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Example of toy-experiment
• Red: what you get when histogramming goes wrong
• Green/blue: (more) correct time-distribution
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
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18
Desired improvements in km3mc
• Handling of hadronic cascades- Current tables are only for EM showers and muons
- Require the geasim package to handle neutrino ‘shower’ events
• Potential fixes:- Approximate cascades from recoil quark jet particles
(mostly pions) with an effective electron cascade (‘one-particle approximation’
- Produce pion tables in gen?
• More accurate histograms- More bins in all dimensions for better interpolation
- Requires restructuring the i/o of gen & hit
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012.
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What is km3 really?
• Five functions, three programs, one package
- Simulation of particle tracks (gen)
- Creation, propagation, and detection of photons (gen)
- Histogramming (hit)
- Simulation of stochastic energy-loss (km3mc)
- Interpolation between and sampling from histograms (km3mc)
• Thinking of km3 as a single ‘thing’ is difficult – and some parts work better than others
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
Storing this information is prohibitive - keeping it as one package is sensible
Storing this information is becoming difficult… merge into hit, or re-write i/o?
Tables produced are km3mc-specific: separate this process?
Generated information is small – processes could be separated
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Summary
• km3 handles photon production and detection from high-energy muons in ANTARES
• Consists of three sub-programs (gen, hit, km3mc)
• Implementation currently limits histogram precision (will be overcome… some time)
• Next set of modifications: test ‘one-particle approximation’
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012.
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Light scattering and propagation
• ‘Rayleigh’ scattering (should be Einstein-Smoluchowski scattering):
- Consider this ~100% accurate (theory + measurements)
• Particulates (Kopelevich model): ‘Mie scattering’
- Water = molecules + small + large particles
- vl and vs are the ppm concentrations: ANTARES uses 0.0075 ppm
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
Water molecules not spherical(otherwise =1)
(otherwise = 4)
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Comparison with measurements
• Best (~only) measurements of angular-dependent volume-scattering function in actual seawater: Petzold (1972)
• Kopelevich model OK at angles >1 degree (~514 nm)C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
Scattering due to turbulence: what is
the wavelength-dependence of
this???
(figure shamelessly plagiarised from Mobley
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Antares approach
• Scattering probability:- Onsite measurements of scattering + absorption
(difficult to deconvolve)- Fit to Kopelevich vs and vl for total scattering
probability (2004) (get 0.0075 ppm)
• Scattered angle:- Calculate ratio of ‘Rayleigh’ / ‘Mie’ scattering using
Kopelevich
- ‘Rayleigh’: use analytic formula to get scattering angle ψ
- ‘Mie’: use the measurements of Petzold
• Ratio of Mie/Rayleigh was fixed until ~now (v4r4 of km3 separates them)
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012
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Problems with current approach
• Petzold’s measurements not wavelength-dependent
• Wavelength-dependence of turbulent scattering probability unknown
• ‘Mie’ scattering will be time-dependent (mostly off biological material)
• Kopelevich theory fits Petzold’s measurements: does this mean it’s correct?
• …
• Does all of this really matter? (requires end-to-end MC study of errors)
C.W.James, ANTARES Monte-Carlo group workshop, Bologna, April 26th-28th, 2012