Source Code
All of the source code is located in the subdirectories of
/export/home/poldata/Code
The executables can all be found in
/export/home/poldata/bin
All of the code currently used has makefiles. If it is necessary to
recompile the code, just go to the relevent directory and run make
(/usr/ccs/bin/make). After you're satisfied that the new version is
correct, copy the executable to /export/home/poldata/bin.
Changes to the code should be documented in the appropriate README
files and source code comments.
Brief Program Descriptions
Our reduction code for polarimetry currently consists of 4 programs,
integ, stokes, sparo-cso, and sparo-sp. A brief description can be found
below. If the program name is typed without any arguments a brief list of
required inputs and possible options will be listed. "program_name -h"
will yield a more detailed (though still brief) list of the available
options. These programs contain the computational kernels necessary to
reduce polarimetry data taken with SPARO. For the most part it is left up
to the user to create graphical displays.
integ
Integ reads the binary data files written by the Goddard DSP data system.
The raw data is processed photometrically and a polarization signal is
calculated. There are currently two versions, integ and integ.cnoise3.
Integ does the photometric processing first and then calculates the
polarization signals. Integ.cnoise3 combines the signals from
corresponding pixels before the photometric processing as described in
Dowell et al (1998).
Status - Was tested on March 1, 1998 with a test file. The cnoise3
program is not currently available. 3/2/98
stokes
Stokes reads the polarization signal files output by integ and calculates
stokes parameters. As input stokes takes a list of polarization signal
files. The output of stokes is a file containing the stokes parameters
for each measurement of each point on the sky.
Status - Was tested at CSO 5/6/98
rougher
rougher uses the output of stokes and an assumed instrument/telescope
polarization to calculate a source polarization. The relative rotation
between the source and instrument/telescope combination are accounted for.
In general the results are only accurate for the boresight pixel since the
other pixels sweep through a region of the sky as the object rotates
beneath the telescope.
Status - Initial tests at CSO. 5/6/98
csopol
csopol performs a least squares fit to data with sky rotation but no
rotator to solve for both the instrument and source polarization.
Status - Initial tests at CSO. 5/6/98
rough-sp
rough-sp uses the output of stokes and an assumed instrument/telescope
polarization to calculate a source polarization. It differs from rougher
in that the object and telescope/instrument do not rotate relative to one
another. As a result the instrument contribution is subtracted differently
than in rougher and results for all pixels will be accurate.
Status - SPARO version not currently available. 3/2/98
Last update May 28, 1998. Contact jdotson@belmont.astro.nwu.edu