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Merge pull request #29 from VERITAS-Observatory/v490-dev-0.1
v490-alpha
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‎DispBDTs/README.md‎

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# Support files for dispBDT angular reconstruction
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dispBDT files are provided in three different bins of zenith angle:
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- small (<40 deg): use dispBDT files trained for 20 deg zenith angle
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- medium (40 deg < ze < 50deg): use dispBDT files trained for 50 deg zenith angle
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- large (>50deg): use dispBDT files trained for 60 deg zenith angle
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Note that this is encoded both in the script `copy_dispBDTs.sh` as in the
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analysis steering scripts for MSCW.

‎DispBDTs/copy_dispBDTs.sh‎

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#!/bin/bash
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# copy dispBDT files from IRF production site
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#
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#
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IRFVERSION=$(cat ../IRFVERSION)
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ANALYSISTYPE="TS"
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SIMTYPE="CARE_June2020"
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for Z in LZE MZE SZE
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do
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if [[ $Z == "LZE" ]]; then
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ZE="60deg"
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elif [[ $Z == "MZE" ]]; then
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ZE="50deg"
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elif [[ $Z == "SZE" ]]; then
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ZE="20deg"
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fi
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echo $Z
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for A in ATM61 ATM62
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do
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if [[ ${A} == "ATM62" ]]; then
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EPOCHS=$(cat ../IRF_EPOCHS_SUMMER.dat | sort -u)
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else
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EPOCHS=$(cat ../IRF_EPOCHS_WINTER.dat | sort -u)
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fi
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for E in $EPOCHS
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do
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ODIR="${E}_${A}/${Z}"
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mkdir -p ${ODIR}
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IDIR="${VERITAS_IRFPRODUCTION_DIR}/${IRFVERSION}/${ANALYSISTYPE}/${SIMTYPE}"
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IDIR="${IDIR}/${E}_${A}_gamma/TMVA_AngularReconstruction/"
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IDIR="${IDIR}/ze${ZE}/"
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if [[ -d ${IDIR} ]]; then
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cp -v ${IDIR}/BDTDisp/*.xml ${ODIR}
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cp -v ${IDIR}/BDTDispError/*.xml ${ODIR}
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fi
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done
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done
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done
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‎GammaHadronCutFiles/ANASUM.GammaHadron-Cut-NTel2-PointSource-Moderate.dat‎

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cut values for quality and gamma hadron cuts
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========================================================
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Moderate point source cuts (box cuts)
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========================================================
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All lines without a '*' in the first column are ignored!
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--------------------------------------------------------
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i) stereo quality cuts
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successfull core and direction reconstruction (>=0.)
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* arraychi2 0. 1.e30
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distance of core position to telescopes [m]
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* arraycore -1. 350.
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size of the camera [deg], all events with direction
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outside of that intervall are ignored
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* cameraedge -1. 2.00
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second largest image size
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(this depends on the state of the instrument)
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* sizesecondmax 400. 1.e30 V4
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* sizesecondmax 400. 1.e30 V5
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* sizesecondmax 600. 1.e30 V6
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cut on mean emission height
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* emissionheight 6. 1.e12
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Telescope multiplicity
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arrayltrig <bit coded telescope combination> <0=off, 1=on> <epoch> <telescope combinations for which this selection is valid>
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* arrayltrig 0 0
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T1
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* arrayltrig 1 0
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T2
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* arrayltrig 2 0
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T1/T2
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* arrayltrig 3 1
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T3
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* arrayltrig 4 0
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T1/T3 V4: unlikely to get a 2-tel gamma-ray event with T1 and T3
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* arrayltrig 5 0 V4 1234
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* arrayltrig 5 1 V5
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* arrayltrig 5 1 V6
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T2/T3
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* arrayltrig 6 1 V4
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T2/T3 and V5/V6: unlikely to get a 2-tel gamma-ray event with T2 and T3
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* arrayltrig 6 0 V5 1234
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* arrayltrig 6 0 V6 1234
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T1/T2/T3
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* arrayltrig 7 1
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T4
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* arrayltrig 8 0
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T1/T4 and V4: telescopes too close to each other
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* arrayltrig 9 0 V4
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T1/T4 and V5/V6: unlikely to get a 2-tel gamma-ray event with T1 and T4
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* arrayltrig 9 0 V5 1234
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* arrayltrig 9 0 V6 1234
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T2/T4 and V4: unlikely to get a 2-tel gamma-ray event with T2 and T4
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* arrayltrig 10 0 V4 1234
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* arrayltrig 10 1 V5
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* arrayltrig 10 1 V6
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T1/T2/T4
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* arrayltrig 11 1
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T3/T4
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* arrayltrig 12 1
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T1/T3/T4
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* arrayltrig 13 1
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T2/T3/T4
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* arrayltrig 14 1
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T1/T2/T3/T4
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* arrayltrig 15 1
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ii) direction cut [deg2]
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* arraytheta2 -1. 0.008
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iii) gamma hadron cuts:
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b) mean scaled width cut (use cut selector 0 in runlist)
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* arraymscw -1.2 0.5
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* arraymscl -1.2 0.7
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iv) energy reconstruction cuts
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echi2 is a measure of the difference between the energies
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estimated per individual telescope
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* arrayechi2 0. 99999.
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cut on energy of reconstruction shower (on linear energy scale, in [TeV])
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* arrayerec 0. 1.e10

‎IRFVERSION‎

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v487
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v490

‎IRF_EPOCHS_SUMMER.dat‎

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V6_2012_2013a
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V6_2012_2013b
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V6_2013_2014a
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V6_2013_2014b
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V6_2014_2015
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V6_2015_2016
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V6_2016_2017
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V6_2017_2018
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V6_2018_2019
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V6_2019_2019s
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V6_2020_2020s
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V6_2021_2021s

‎IRF_EPOCHS_WINTER.dat‎

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V6_2012_2013a
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V6_2012_2013b
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V6_2013_2014a
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V6_2013_2014b
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V6_2014_2015
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V6_2015_2016
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V6_2016_2017
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V6_2017_2018
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V6_2018_2019
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V6_2019_2020w
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V6_2020_2021w
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V6_2021_2022w

‎ParameterFiles/EVNDISP.reconstruction.runparameter.NN.v4x‎

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eventdisplay reconstruction parameter file
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===========================================
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next-neighbour cleaning (no angular DISP) - v4x versions
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===========================================
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Note: all line without '*' in the beginning are ignored
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Remember that after changing any values here, you have to redo lookup tables,
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effective areas and radial acceptances
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(so don't do it)
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The following file describes the reconstruction parameters for eventdisplay:
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i) trace integration and image cleaning parameter
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ii) quality cuts applied before the array analysis
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(reconstruction of shower core and direction).
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Each set of cuts listed below correspond to one set of array parameters in the
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eventdisplay output file (showerpars tree):
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for example: first set of cuts to Xcore[0], Ycore[0], etc., second set to Xcore[1], Ycore[1], ...
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The maximum number of different set is 100
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(can be changed in VGlobalRunParameter: variable VDST_MAXRECMETHODS
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mscw_energy reads the results of one set only, choose with -arrayrecid=RECID
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(e.g. for cut set 13: -arrayrecid=13)
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(Note: There is some confusion between the words method and cut set in the array analysis code of
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eventdisplay.)
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Note that these values override parameters given at the command line (!)
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---------------------------------------------------------------------------------------------------
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---------------------------------------------------------------------------------------------------
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i) trace integration and image cleaning parameter
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--------------------------------------------------
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trace integration <integration method (0=off/1=default/2=sliding window)>
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* -1 FADCANALYSIS 2
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double pass method
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Par1: <doublepass (on=1, off=0)>
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Par2: <integration window length for pass 1>
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Par3: <integration method for pass 1 (1/2)>
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Par4: <double pass error option (0/1)> (don't change if you don't understand)
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Par5: <maximum time difference between LG and HG T0 (default -4 samples)>
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* -1 FADCDOUBLEPASS 0 6 2 0 -4
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trace integration window <window 1> <window 2>
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* -1 FADCSUMMATIONWINDOW 6 6
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trace integration start (for window 1 for integration method 1)
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Par1: <sample # of window start>
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Par2: <shift of window start for double pass>
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Par3: <timing method used for calculation of window start (FIXED/TZERO/TAVERAGE)>
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Par4: <max difference between T0 and trace integration start>
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* -1 FADCSUMMATIONSTART 0 0 TAVERAGE
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image cleaning <method=TWOLEVELCLEANING/TIMECLUSTERCLEANING/TIMETWOLEVEL/CLUSTERCLEANING> <FIXED/VARIABLE>
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* -1 IMAGECLEANINGMETHOD TIMENEXTNEIGHBOUR FIXED
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probability to get fake image from NSB for this readout window
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* -1 IMAGECLEANING_FAKEPROBABILITY 0.5E-3
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* -1 IMAGECLEANING_ACTIVEMULTIPLICITIES 4NN 2NNp1 3NN 2NN
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* -1 WRITEGRAPHSTOFILE TRUE
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image calculation at the edge of the camera <start fit for image with at least this loss> <min number of tubes>
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* -1 LLEDGEFIT 0.05 5
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quality cut on distance of image/border pixel (applied for all cuts defined below)
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(this is currently used for plotting only)
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-1 BRIGHTSTARS CATALOGUENAME MIN_B_MAGNITUDE MIN_DISTANCE_DEG <apply cut for images with less then minimum number of tubes>
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* -1 BRIGHTSTARS Hipparcos_MAG8_1997.dat 3.0 0. 15
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ii) quality cuts applied before the array analysis
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--------------------------------------------------
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USAGE:
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to start a new set of cuts:
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'* -1 RECMETHOD 4'
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syntax:
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<telescope type> <variable name> <variable value>
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all line without '*' in the beginning are ignored
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all operators are '>' or '<' (except for number of images, where it is '>=')
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DEFAULTS:
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minimum number of images required for stereo reconstruction
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-1 MNIMAGE 2
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minimum angle between image axes for two telescope analysis [deg]
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-1 MINANGLE 5.
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minimum number of channels for all telescopes
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-1 MINTUBES 4
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maximum number of low gain channels per telescope
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-1 MAXLOWGAIN 5000
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minimum local distance for all telescopes [deg]
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-1 MINDIST -1.e3
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maximum local distance for all telescopes [deg]
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-1 MAXDIST 1.e3
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minimum alpha for all telescopes [deg]
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-1 MINALPHA -1.e3
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maximum alpha for all telescopes [deg]
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-1 MAXALPHA 1.e3
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minimum image size for all telescopes [dc]
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-1 MINSIZE 400
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ignore all pointing corrections (default: off)
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-1 USEEVNPOINTING 0
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maximum loss of image size on edge of the camera [%]
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-1 MAXLOSS 0.05
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maximum width/length (to remove images to close to the telescopes)
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-1 MAXWIDTHLENGTH 1.e10
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---------------------------------------------------------------------------------------------------
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---------------------------------------------------------------------------------------------------
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Set 0 = default reconstruction method
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* -1 RECMETHOD 4
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* -1 MINANGLE 10.
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* -1 MINTUBES 5
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* -1 MINSIZE 100
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* -1 MAXLOSS 0.2
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* -1 MINWIDTH 0.02
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* -1 MAXDIST 1.75
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======== IMPORTANT IMPORTANT ============
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ignore the following lines for regular data analysis
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-1 MCONLY
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======== IMPORTANT IMPORTANT ============
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Set 1 = (placeholder, as this is a no-disp file)
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* -1 RECMETHOD 4
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* -1 MINANGLE 10.
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* -1 MINTUBES 5
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* -1 MINSIZE 100
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* -1 MAXLOSS 0.2
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* -1 MINWIDTH 0.02
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* -1 MAXDIST 1.75
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==============================
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3-telescope combinations
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==============================
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Set 2 = T1 off default reconstruction method
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* -1 RECMETHOD 4
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* -1 MINANGLE 10.
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* -1 MINTUBES 5
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* -1 MINSIZE 100
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* -1 MAXLOSS 0.2
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* -1 MINWIDTH 0.02
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* -1 MAXDIST 1.75
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* 1 USEIMAGE 0
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Set 3 = T2 off default reconstruction method
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* -1 RECMETHOD 4
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* -1 MINANGLE 10.
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* -1 MINTUBES 5
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* -1 MINSIZE 100
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* -1 MAXLOSS 0.2
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* -1 MINWIDTH 0.02
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* -1 MAXDIST 1.75
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* 2 USEIMAGE 0
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Set 4 = T3 off default reconstruction method
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* -1 RECMETHOD 4
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* -1 MINANGLE 10.
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* -1 MINTUBES 5
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* -1 MINSIZE 100
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* -1 MAXLOSS 0.2
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* -1 MINWIDTH 0.02
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* -1 MAXDIST 1.75
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* 3 USEIMAGE 0
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Set 5 = T4 off default reconstruction method
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* -1 RECMETHOD 4
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* -1 MINANGLE 10.
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* -1 MINTUBES 5
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* -1 MINSIZE 100
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* -1 MAXLOSS 0.2
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* -1 MINWIDTH 0.02
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* -1 MAXDIST 1.75
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* 4 USEIMAGE 0
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ParameterFiles/EVNDISP.reconstruction.runparameter.v48x renamed to ParameterFiles/EVNDISP.reconstruction.runparameter.v4x

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