INCLUDES FADC HI-LO GAIN
 

GrISUDet Configuration

The configuration file defines the telescope array. As with all input files, a line with no asterisk is a comment line. The comments in the file make it self-explanatory (hopefully)

The following table shows excerpts from the veritas4tel.cfg configuration file.

Because of the length of this file, we only give a small number of entries for the telescope mirrors and photomultiplier tubes (rather than listing hundreds of lines of mirror and pmt definition lines. We also only list several neighbor-list records).

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IMPORTANT COMMENT:

For accurate determination of peds/pedvars with the FADC option, use a large noise-loop size (see the SIMUL record in the configuration file) and possibly a large number of samples in the pedestal event records depending on your analysis software(see FADCS record in the configuration file).  Multiple pedestal records will now be independent of each other (not so with the previous version of GrISU).


 For the QADC option, use a large noise-loop size as described above. Create
a large number of pedestal events, e.g. 400, in the NBRPR record in detector.pilot. In this GrISU release, the maximum noise-loop size is 6000 time bins. Simarily, you may create pedestal files for the QADC option from analysis.c. 
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_______________________________
| |
| VERITAS CONFIGURATION |
|_______________________________|


Eventually this file will be produced by some userfriendly
interface. As with other input files, a line not starting with a '*'
is considered as a comment. When a line starts with a '*', the program
will start looking for a 5-character flag used to identify the data to
be read from that same line. In order to make this file human readable
comments presenting the format of the various records are welcome. When
information is missing or out of range the code should issue an error
message.

version number appropriate for this configuration file. read_array will check.
VERSN must be the first parameter line in the configuration file.
* VERSN 4.1.5

Numbre of telescope (NBRTL)
The telescope identification index must be 1 or larger (equal to the number
of telescopes in the array).
* NBRTL 4

Telescope location in the field (TLLOC) the parameters are:
-the telescope identification number
-the X (oriented towrd east) location cordinate in meters.
-the Y (oriented toward north)location cordinate in meters.
-the Z (oriented toward up) location cordinate in meters.
-the telescope rotation offset in meters.
The telescope rotation offset is the distance below the focal point
of the mirror along the optical axis about which the telescope
rotates. (intersection of the elevation and azimuth axis)
-the pointing offset in the x direction
-the pointing offset in the y direction

* TLLOC 1 0.0 0.0 0.0 12.0 0.0 0.0
* TLLOC 2 -69.282 40.0 0.0 12.0 0.0 0.0
* TLLOC 3 69.282 40.0 0.0 12.0 0.0 0.0
* TLLOC 4 0.0 -80.0 0.0 12.0 0.0 0.0

The SGRFC record specifies the name of the configuration file
to be used for Sgarface modeling. If this record is used the standard
electronics will not be simulated. Only the SGarface specific
electronics will be simulated.
SGRFC ../../Config/Files/whipple_sgarface.cfg

THE ELECTRONICS IS SO FAR ASSUMED TO BE THE SAME
FOR ALL TELESCOPES IN THE ARRAY.

The simulation parameter record SIMUL contains
-the time between samples in ns (this is also the sampling time
for the simulation calculation to be carried with.)
-the number of samples over which the simulation produces the signals
-the number of samples over which the noise database is produced
* SIMUL 2.0 100 4000

The FADC record (FADC) contains
-the FADC output ON-OFF status (1=ON, 0=OFF)
-the FADC output voltage per digital count in mV
-the FADC pedestal in digital counts
-the FADC digital output dynamic range
-the number of sample to be written on the output for each channel.
-the number of samples between the trigger and the beginning of the
FADC record. A positive number corresponds to a record starting
at a time anterior to the trigger time.
-the number of samples in pedestal event records
-The ratio between high and low gain for system with hi-lo gain switch
        dynamic range extention. If this number is less than 1.0 the function
        is disabled.
   -The threshold in FADCdigital counts for the low gain activation.
* FADCS 1 7.84 20.0 256 64 10 2000 6.0 250

To determine the total number of dc's per photon electron, see the
grisudet documentation pages following links from GrISU/Documentation/grisu.html


The QADC record (QADC) contains
-the QADC output ON-OFF status (1=ON, 0=OFF)
-the QADC gate width
-the QADC gate opening time with respect to the trigger time in
nanosecondes. A positive time corresponds to the opening of the
gate at a time anterior to the trigger time.
-the QADC conversion factor(pC/digital count)
-the QADC pedestal
-the QADCdynamic range
-QADC input impedance
* QADCS 0 25.0 5.0 0.25 20.0 1024 50.0


The trigger record (TRIG) contains
-the single PMT threshold in mV
-the discriminator output pulse width in ns
-the pixel coincidence time window in ns
-the minimum number of triggered channels required by the coincidence logic
-the minimum number of telescopes required
-the telescope coincidence time window width in nanosecondes
TRIGG 32.0 25.0 10.0 2 1 15.0
normal line for 2001 whipple
* TRIGG 70.0 7.0 5.0 3 4 10.0

To disable the pattern trigger, remove the asterisks on PSTON and all PATCH
records
Pattern Selection trigger (PSTON).
-the minimum number of adjacent triggered channels required by the
pattern trigger logic. For example if the minimum number of adjacent channels is 3, then there will only be a local trigger if at least three adjacent pixels trigger. This logic eliminates triggering on sky noise.
-the number of 19 pixel trigger patches
* PSTON 3 91

Trigger patch list records (PATCH)
-Patch identification number
-A flag indicating if the patch is enabled (1) or not (0).
-List of id numbers for pixels in patch (0 indicates no pixel connected)
The order of the 19 pixel list is important.

* PATCH 1 1 12 13 14 15 16 11 4 5 6 17 10 3 1 7 18 9 2 19 8
* PATCH 2 1 12 4 1 2 8 25 11 3 9 21 44 24 10 22 40 43 23 41 42
* PATCH 3 1 44 24 10 22 40 69 43 23 41 65 100 68 42 66 96 99 67 97 98

The analog electronics record (ANLG) contains
-the PMT current gain
-the equivalent system impedance(i.e. the conversion factor in Ohm
between amps on the output of the PMT and voltages on the
output of the analog signal processing) or similarly between the PMT output
and the input to the fadc. Amplification within the fadc board and cable loss
must be included in this equivalent impedance.

-the electronics voltage noise standard deviation in mV
* ANLOG 2.0E5 2722.0 3.6

For the Qadc option, the number of digital counts per photoelectron is:
dc/pe = (electronic charge in pC)*(PMT current gain) *(equivalent system impedance)/
( (Qadc input impedance)*(Qadc conversion factor) )
Similarly, for the Fadc option, the number of digital counts in a given time bin is: (electronic change )*(equivalent system impedance)/( width_of_time_bin * volts_per_digital_count).

Mirror design (MIROR). The parameters are
-the telescope identification number
-the mirror radius in meters
-focal length in meters
-the focusing error in meters (>0 when camera is too
far away from the dish)
-the mirror type (1=DavisCotton)
-the number of mirror elements.
* MIROR 1 7.0 12.0 0.0 1 357
* MIROR 2 7.0 12.0 0.0 1 357
* MIROR 3 7.0 12.0 0.0 1 357
* MIROR 4 7.0 12.0 0.0 1 357

Mirror reflectivity curve (RFCRV). The flag is followed by
-the the reflectivity curve identification index
-the number of points given on the quantum efficiency spectral curve.
This is followed by a serie of
-wave length(in nano-meter)
-reflectivity(fraction of unity)
If the number of points is in excess of the indicated number, the last
values will be ignored. If the number of points given is less than the
indicated number all the last points will adopts the last value from the
list. Reflectivity data should be given before being refered to by
mirror characteristics. If reflectivity data is given twice for the same
reflectivity curve identification index, the second occurence will be
taken into account.

reflectancies for new mirrors from Abe, 12/31/03
* RFCRV 1 14
260. .910096
280. .924227
300. .928669
320. .930207
340. .927741
360. .921187
380. .912374
400. .900516
450. .864815
500. .828433
550. .802362
600. .789813
650. .785047
700. .783756

Mirror element (MIREL) characterisation. For each we have
-the telescope identification number
-the mirror element identification number
-the element shape (1=circular, 2=hexagonal,
  3=square)
 -orientation angle(degrees). If 0.0, polygon side
   perpendicular to y-axis of the telescope coordinate
   system.
-the external radius
-the curvature radius
-the x position of the element on the dish (in meters)
-the y position of the element on the dish (in meters)
-the maximum mis-alignement in degrees
-the maximum blure radius in degrees
-the degradation factor (1.0=perfect 0.0=missing)
-the reflectivity curve identifier

* MIREL 1 1 2 0.0 0.355 24.00 -0.025845 0.00 0.020 0.030 0.00 1
* MIREL 1 2 2 0.0 0.355 24.00 -0.025845 0.609737 0.020 0.030 0.00 1
* MIREL 1 3 2 0.0 0.355 24.00 -0.025845 -0.609737 0.020 0.030 0.00 1
* MIREL 1 4 2 0.0 0.355 24.00 -0.025845 1.2179 0.020 0.030 1.00 1
* MIREL 1 5 2 0.0 0.355 24.00 -0.025845 -1.2179 0.020 0.030 1.00 1

etc, through all four telescopes

* MIREL 4 353 2 0.0 0.355 24.00 -5.97759 -0.913821 0.020 0.030 1.00 1
* MIREL 4 354 2 0.0 0.355 24.00 5.97759 1.51955 0.020 0.030 1.00 1
* MIREL 4 355 2 0.0 0.355 24.00 -5.97759 1.51955 0.020 0.030 1.00 1
* MIREL 4 356 2 0.0 0.355 24.00 5.97759 -1.51955 0.020 0.030 1.00 1
* MIREL 4 357 2 0.0 0.355 24.00 -5.97759 -1.51955 0.020 0.030 1.00 1

Quantum efficiency (QUEFF). The flag is followed by
-the quantum efficiency identification index
-the number of points given on the quantum efficiency spectral curve.
This is followed by a series of lines giving
-wave length(in nano-meters)
-quantum efficiency(fraction of unity)
If the number of points is in excess of the indicated number, the last
values will be ignored. If the number of points lines is less than the
indicated number the remaining points will adopt the last value from the
list. Quantum efficiency data should be given before being refered to by
PMT characteristics. If quantum data are given twice for the same
quantum efficiency identification index, the second occurence will be
used in the simulations.


* QUEFF 1 27
195.6430 0.0698
222.1966 0.0927
235.4735 0.1156
248.7503 0.1464
279.7296 0.1826
306.2832 0.2137
328.4112 0.2276
359.3905 0.2349
394.7954 0.2312
421.3490 0.2171
447.9026 0.1914
478.8819 0.1635
501.0099 0.1353
523.1379 0.1069
531.9891 0.0792
549.6915 0.0543
569.6068 0.0384
585.0964 0.0280
609.4372 0.0169
620.5012 0.0122
631.5652 0.0085
638.2036 0.0055
642.6292 0.0042
647.0548 0.0033
655.9060 0.0023
664.7572 0.0017
669.1828 0.0012

Camera design (CAMRA).
   -telescope identification number
   -the number of phototubes.
   -the angle (counter clockwise on the display) by which the camera is
    rotated. The given pixel corredinates will be rotated by minus that angle.
   -the relative gain/throughput for that camera. In the simulation, all the
    PMT signals from that camera will be multipled by that number. In analysis,
    all the PMT signals from that camera will be divided by that number
* CAMRA 1 499 0.0 1.0
* CAMRA 2 499 0.0 1.0
* CAMRA 3 499 0.0 1.0
* CAMRA 4 499 0.0 1.0

Phototubes (PMPIX). For each we have
-the telescope identification number
-the pixel identification number
-the pixel shape (1=circular, 2=hexagonal, 3=square)
-orientation angle(degrees). If 0.0, polygon side
 perpendicular to the y-axis
-the X position coordinate in the focal plane in mm
-the Y position coordinate in the focal plane in mm
Camera coordinates are such that increasing X corresponds to
going WEST when telescope is pointing SOUTH. Increasing Y
corresponds to increasing elevation.
-the PMT Radius in mm
The PMT radius really is the radius of the sensitive area (Radius of
the light cone input for example).
-the geometrical efficiency which may be used to include the effects
of light cone loss.
-the quantum efficiency identification number to be used for that tube.
-the single photoelectron signal relative amplitude fluctuation.
-the signal rize time in nanosecondes
-the signal fall time in nanosecondes
-the RC coupling time constant in nanosecondes
Note that the pulse shape can also be specified by a table. For this see instructions at the end of this file.
-the bellongin of the channel to the trigger (1 if it bellongs,
0 other wise)
-a flag indicating if the pixel should be used in the analysis(1) or not(0)
-a time offset in nanosecond. It measures how late the pulse is locate in
the stack for each channel. the analysis and the simulation search
for the smalles non negative value and subtract it from all the other
to apply a relative correction.
-a relative gain factor to account for the imperfect gain flat fielding.
In the anlysis, each pixel value is multiplied by this number while
in the simulation pulse amplitudes are divided by this number.

* PMPIX 1 1 1 0.0 0.000000 0.000000 15.0 0.97 1 0.45 2.57 8.50 0.000 1 1 0.0 1.0
* PMPIX 1 2
1 0.0 30.997116 0.000000 15.0 0.97 1 0.45 2.57 8.50 0.000 1 1 0.0 1.0
* PMPIX 1 3
1 0.0 15.498533 -26.808302 15.0 0.97 1 0.45 2.57 8.50 0.000 1 1 0.0 1.0
* PMPIX 1 4
1 0.0 -15.498533 -26.808302 15.0 0.97 1 0.45 2.57 8.50 0.000 1 1 0.0 1.0
etc, through all tubes for telescope 1

Neighbors list records (NGHBR)
-Telescope identification number
-Pixel identification number
-Number of neighbors
-List of neighbors identification numbers

* NGHBR 1 1 6 2 3 4 5 6 7
* NGHBR 1 2 6 1 3 7 8 9 19
* NGHBR 1 3 6 1 2 4 9 10 11
* NGHBR 1 4 6 1 3 5 11 12 13
* NGHBR 1 5 6 1 4 6 13 14 15

etc, through all tubes for telescope 1

then repeat for telescopes 2, 3, and 4

The detailed single photoelectron pulse shape can be entered with the PULSE entry followed by the number of points in the table and the time interval between points. The correct number of points is expected to follow. In principle, the integral of the tabulated pulse shape should be equal to 1.0 (or close enough). Specifying a tabular pulse shape over-rides any pule rise time and fall time given in the pixel table. The pulse shape will be the same for all pixels in all telescopes
  PULSE 10 2.0
0.0
0.25
0.25
0.0
0.0
0.0
0.0
0.25
0.25
0.0