impact of water optical properties on tracks reconstruction
DESCRIPTION
IMPACT OF WATER OPTICAL PROPERTIES ON TRACKS RECONSTRUCTION. ANTARES Collaboration Meeting Moscow, June 06 th -10 th , 2011. H Yepes -Ramirez IFIC (CSIC – Universitat de València). OUTLINE. - PowerPoint PPT PresentationTRANSCRIPT
IMPACT OF WATER OPTICAL PROPERTIES ON IMPACT OF WATER OPTICAL PROPERTIES ON TRACKS RECONSTRUCTIONTRACKS RECONSTRUCTION
IMPACT OF WATER OPTICAL PROPERTIES ON IMPACT OF WATER OPTICAL PROPERTIES ON TRACKS RECONSTRUCTIONTRACKS RECONSTRUCTION
H Yepes -Ramirez H Yepes -Ramirez IFIC (CSIC – Universitat de València)IFIC (CSIC – Universitat de València)
ANTARES Collaboration Meeting
Moscow, June 06th-10th, 2011
OUTLINEOUTLINEOUTLINEOUTLINE
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth2
Brief reminder of light propagation Brief reminder of light propagation in sea water: in sea water: ANTARES Monte Carlo
model
Simulation: Simulation: absorption and scattering inputs, codes and data selection
Selected resultsSelected results
Conclusions and outlookConclusions and outlook
Brief reminder of light propagation Brief reminder of light propagation in sea water: in sea water: ANTARES Monte Carlo
model
Simulation: Simulation: absorption and scattering inputs, codes and data selection
Selected resultsSelected results
Conclusions and outlookConclusions and outlook
Brief reminder of light Brief reminder of light propagation in sea waterpropagation in sea water
Brief reminder of light Brief reminder of light propagation in sea waterpropagation in sea water
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth3
Scattering phase function (Scattering phase function ())
Morel and Loisel approach
Molecular scattering (Rayleigh) Isotropic (<cos>=0)
= contribution of Rayleigh scattering
Particle scattering (Mie) Strong forward peaked (<cos>Mie=0.924)
effscatabs
effatt
111
Attenuation Length (COLIMATED BEAM)
Effective Attenuation Length (ISOTROPIC SOURCE)
Absorption lengthAbsorption length Scattering LengthScattering Length
scatabsatt 111
Mie
scatscateffscat
cos)1(1cos1
924.0cos Mie
Scattering length wavelength dependence
(Kopelevich parameterization)
][550
312.0550
34.1550
0017.0 13.07.13.4
mvvb ls
scat
b1
b = scattering coefficient.
vs, vl = scattering centers.<Cos> = Average cosine of the global distribution
Petzold values for particle scattering
)()1()()( *** MieRay
SimulationSimulationSimulationSimulation
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth4
A set of water properties inputs reliable for study:
• AIM production of the absorption and scattering spectrum for different water models for muons and neutrinos, in agreement to the water models proposed for the data/MC CALIBOB comparison for optical beacon data (J Ruiz-Rivas, Collaboration Meeting in Paris 2010).
• Ten different water models (two runs each, just for a first approach) for muons and neutrinos (20 files for muons, 20 files for neutrinos).
SimulationSimulationSimulationSimulation
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth5
abs [m] Vs, Vl (scattering centers) [ppm] scat at 470 nm [m]
55 0.0075 53 0.17
55 0.01 41 0.17
55 0.02 22 0.17
55 0.01 41 0.11
55 0.02 22 0.02
63 0.0075 53 0.17
63 0.01 41 0.17
63 0.02 22 0.17
63 0.01 41 0.11
63 0.02 22 0.02
• Three runs with the same value and different scattering spectrum for a given absorption length.
• Three runs with different values, but is computed in such a way that the three runs will have the same effective scattering length at 470 nm, for a given absorption length.
• Three common models for comparisons (muons abs55-abs63, neutrinos abs55) with previous Monte Carlo productions.
• OM Angular acceptance of June 2009 (Genova Meeting 2009).
SimulationSimulationSimulationSimulation
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth6
GENGENWATER MODEL:
•Photon tables production (water tables) Water tables (hbook files) + Description files (ASCII files).
HITHITOM PARAMETERS:
• Hit probability computation from the water tables for a given OM parameters Hit tables (hbook files) + Description files (ASCII files).
KM3KM3SIMULATED EVENTS: GEOMETRY + KINEMATICS
• Physics events reading and OM hits production based on event geometry and hit probability tables Detector events: Signal hits (muons, not tracks from hadronic showers), physical background.
GEASIMGEASIM
MCEWMCEW
TETE
RECORECO
SIMULATIONS OF ATMOSPHERIC NEUTRINO INTERACTIONS.
• Process (and evaluation) tracks from particles coming from the hadronic showers (also muons from KM3).
TRANSLATION OF INFO ASCII FILES INTO ROOT FORMAT.
FORMAT CONVERSION TO “LOOK LIKE DATA”: electronics smearing effects (calibration, ARS response) and optical background.
RECONSTRUCTION: Reconstruction of track direction (AAfit) and ntuples information arrangement as number of hits, zenith distribution…(AntDST).
Simulation chain:
SimulationSimulationSimulationSimulation
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth7
Main options and software versions in muons and neutrinos simulation:
CODE/INPUT OPTIONS/VERSIONS
GEN v3r7
HIT v3r7
KM3 v3r7
DETECTOR r12_c00_s01
GEASIM v4r10
MCEW -
TriggerEfficiency Gaussian ARS threshold file: threshold_gaus_0.33_0.08_0.1.txt
SoS file: noise_basic_harold.root (Thanks to C Bogazzi)
-n 10000000 –t 104.858 –C3 – p 0.035
-t 104.858 Frame time in ms. To determine the number of background hits to be generated in case the summary data are used.
-C3 Hit generator type: 3, Gaussian, according observed charge distribution, with time-dependent contribution of after pulses.
2010-09-23 version
Aafit v0r6
AntDST v1r1
SimulationSimulationSimulationSimulation
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth8
Methodology: runs selection, lifetime computations and weights
1. Data subsample: “Point source search with 2007 and 2008 data” (ANTARES-PHYS-2010-008).
3. Lifetime and scaling for MC:
• Lifetime for neutrinos: 365 days.
• Lifetime for muons: 2*8320/86400 = 0.19 days.
4. Weights:
• Neutrinos: w3*(1.0/2*1.0e+10).
• 1044 files (12 lines detector) [08/05/2008-30/12/2008].
• Lifetime data: 76.77 days.
• ntuples from JP Gomez-Gonzales (thanks!!!).
2. MC sampling:
• SoS file prepared by C Bogazzi (thanks!!!) from the data subsample (noise_basic_harold.root): time slices taken from all different acquisition conditions.
• Mupage for muons.
• Geasim for neutrinos.
Thanks to Annarita and Carla also for the codes used as starting point and their support !!!
Thanks also to Patrick, Maarten and Aart from NIKHEF for their appropriate help about software details !!!
“Different” water tables – Same SoS file
“Different” water tables – Different SoS file
Same water tables – Same SoS file
Remarks:
1.Water tables produced by Annarita to Juan Pablo and the mine ones, are equivalent (absorption length 63 m).
2.Reproducibility of the simulation chain and equivalence among scripts are OK (just one run considered).
3.Run-dependent simulation effect is seen from the SoS Monte Carlo sampling (factor ~ 1.20).
4.Agreement data / MC should be independent of the SoS file. Confirmation in next slides MC Sampling with a SoS file based on 2008-2009 data subsample. Data/MC comparisons with the same data subsample.
SimulationSimulationSimulationSimulation
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth9
SimulationSimulationSimulationSimulation
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth10
My production (abs = 55 m)Juan Pablo (Amsterdam) (abs = 55 m)
• SoS File: noise_basic_harold.root
• Data ≈ MC (), Data > MC ().
• KM3 v3r7, Aafit v0r6.
• 2008 data.
• OM angular acceptance 09.
• SoS File: ?
• Data < MC (), Data ≈ MC ().
• KM3 v3r6, Aafit v0r6.
• 2007-2008 data.
• OM angular acceptance 08.
tcosth > 0 && beta < 1
tcosth > 0 && beta < 1
Juan Pablo (CERN)
RED:
abs = 63 m
SimulationSimulationSimulationSimulation
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth11
My production
RED:
abs = 63 m
• SoS File: noise_basic_harold.root
• MC > data.
• Aafit v0r6.
• SoS File: noiseblendL12-basic.root
• Data > MC.
• Aafit v0r6.
tcosth > 0 && beta < 1 tcosth > 0 && beta < 1
SimulationSimulationSimulationSimulation
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth12
What kind of information we have:
1. Reconstructed data (muons + neutrinos):
• Absorption + scattering info:
• Reconstruction quality parameter.
• Number of hits used in the fit.
• Total amplitude of the hits used in the fit.
• Zenith distributions.
• Etc…(backup).
• Scattering info Time residuals.
• No reconstructed data has not been analyzed yet.
A quick look over some distributions
• Some extremes models could be discarded (i.e, blue line).
• Muons region seems to be specially in agreement for the cases at the same effective scattering length (lambda > -7).
• Neutrinos region for lambda > -4.5 have a nice agreement. MC Underestimation lambda < -4.5 .
ResultsResultsResultsResults
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth13
Reconstruction quality parameter ():
tcosth > 0 && beta < 1
• Some extremes models could be discarded (i.e, grey line).
• Muons region seems to be in agreement most cases.
• Neutrinos region agreement at absorption 55 m is not enough clear as is seen for the models at 63 m. And peaks ..?
ResultsResultsResultsResults
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth14
tcosth > 0 && beta < 1
• Some extremes models could be discarded (i.e, blue line).
• Some distributions scales to the peak and others to the tail…
ResultsResultsResultsResults
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth15
Number of hits used in the fit (Nhit):
tcosth < 1 && nhit > 5 && lambda > -5.4
• Some extremes models could be discarded (i.e, blue line).
• Scale to the peak is not seen as in the previous case, but a nice agreement seems to be for the tails of the green and light blue model.
ResultsResultsResultsResults
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tcosth < 1 && nhit > 5 && lambda > -5.4
• Some extremes models could be discarded (i.e, blue line).
• Some distributions scales to the peak (blue and magenta) and others to the tail (green and sky blue).
ResultsResultsResultsResults
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Total amplitude of the hits used in the fit (Ahit):
tcosth < 1 && nhit > 5 && lambda > -5.4
ResultsResultsResultsResults
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth18
• Some extremes models could be discarded (i.e, blue line).
• Agreement to the tails for green and sky blue models, seems to be for light yellow also.
tcosth < 1 && nhit > 5 && lambda > -5.4
• Some extremes models could be discarded (i.e, blue line). Peaks ???
• Muons region agreement could be take place for distributions at same effective scattering length.
• Lack of neutrino events for most cases STATISTICS DEPENDENT (few runs to compare) SEE NEXT SLIDE.
ResultsResultsResultsResults
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Zenith angle of the fitted track (cos):
lambda > -5.4 && beta < 1
ResultsResultsResultsResults
ANTARES Collaboration Meeting ANTARES Collaboration Meeting Moscow, Moscow, JuneJune 06 06thth-10-10thth20
Stat
istic
s ef
fect
on
zeni
th d
istr
ibut
ions
:
abs
= 5
5 m
@ 4
70 n
m (f
rom
offi
cial
pro
duct
ions
)
• Some extremes models could be discarded (i.e, grey line). Peaks ???
• Muons region agreement could be take place for distributions at same effective scattering length.
• Lack of neutrino events again !!!
ResultsResultsResultsResults
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lambda > -5.4 && beta < 1
ResultsResultsResultsResults
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Time residuals (thit - texp):
ResultsResultsResultsResults
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CONCLUSIONS AND OUTLOOKCONCLUSIONS AND OUTLOOKCONCLUSIONS AND OUTLOOKCONCLUSIONS AND OUTLOOK
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1. How much the correct model could matters?
2. What model could we trust on it?
3. P
4. L
5. A tentative “to do list”:
• Number of hits in the trigger.
• Total number of hits in the event.
• Arrival time of the hit on the PMT, before and after trigger.
• Detector performance: expect impact on effective areas and detector angular resolution.
MORE PLOTS CAN BE FOUND IN THE BACKUP OR:
http://ific.uv.es/~yepes/CM_MOSCOW_2011/finalPlots
1. How much the correct model could matters?
2. What model could we trust on it?
3. P
4. L
5. A tentative “to do list”:
• Number of hits in the trigger.
• Total number of hits in the event.
• Arrival time of the hit on the PMT, before and after trigger.
• Detector performance: expect impact on effective areas and detector angular resolution.
MORE PLOTS CAN BE FOUND IN THE BACKUP OR:
http://ific.uv.es/~yepes/CM_MOSCOW_2011/finalPlots
BACKUPBACKUPBACKUPBACKUP
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5 parameters fit - 2 minimization: t0, , , x0, y0
cgctheory
k
v
kl
ctt
sin
1
tan
10
Reconstruction quality factor L:
• Linear prefit photon hit coordinates x, y, z, t
• Minimization with hit-charge weights.
• Maximum likelihood (L) fit computed from MC PDF of time residuals.
)1(log
solutionsdof
NN
L
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Statistics effect on zenith distributions:
abs = 63 m @ 470 nm (official mupage production @ CERN)
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Angular error ():
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Azimuth:
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Number of lines used in the fit (Nlines):
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GLOSARY:
Time slices: