pasa
Updated: Jul15,2020

PASA statnds for Process A Single Acm. This code allows one to efficiently process (header repair, bias and dark subtraction) a single raw acm image. A before and after illustration of this process is shown in the figure below.


Usage: pasa /home/sco/acmdat/S/20190401T115437.0_acm_sci.fits Y N [-nd]  
arg1 - name of acm image (can be full path)  
arg2 - run in interactive gui mode mode 
arg3 - run in debug/verbose mode 
Additional options: 
   -nd = do not perform a dark signal subtraction 

For a more detiled description see:
%  pasa --help

As of Apr2019, this code is frequently being upgraded. Using the last "help" option above is advised. Note that to assemble the local bias files for a given night, the acm_bias_for_date. Basically, this will creat 2 files neede by pasa: BIAS.DATA and fbp.table. A related code, used for processing whole nights of acm data is do_acm_night.

An example of a raw acm image (left) after ccd processing (right). This is a ramdom acm image from the night of 20190505. This image has been processed with teh pasa code. A fixed bias pattern (FBP) and a mean bias level has been subtracted. A sclaed dark rate image was also subtracted.

In July2020 I was (once again!) studying the acm bias properties.

An example of not subtracting a dark signal and applying only the fixed bais pattern subtraction.


% cat BIAS.DATA 
 0.0  0.0 
% head -5 fbp.table 
# Bias-subtracted FBP from acm_fbp.sh  median bias =     1397.432
# data
   1.0      365.8170       0.0066       0.0002      771.0
   2.0     -267.3059       0.0056       0.0002      771.0
   3.0     -192.9463       0.0066       0.0002      771.0
% pasa /media/sco/DataDisk1/sco/AD/HET_work/acm_nights/20191027/acm/20191027T222438.5_acm_sci.fits Y N -nd

Note that by using "Y" for the second command line argument we were able to view the before and after processing of the single acm bias frame.

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