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information_for_astronomers:user_guide:reduc_pointing [2016/11/03 16:49]
ubach [Reducing a number of scans at once]
information_for_astronomers:user_guide:reduc_pointing [2022/07/04 20:35] (current)
twedel
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 |rfi=n| Will filter RFI peaks looking for peak increasing n times the rms.| |rfi=n| Will filter RFI peaks looking for peak increasing n times the rms.|
 |window=n| Defines the window size in multiples of the beam width for the second iteration of the Gaussian fit (orange box in the plot window). Default is 1.22| |window=n| Defines the window size in multiples of the beam width for the second iteration of the Gaussian fit (orange box in the plot window). Default is 1.22|
 +|rms| Prints the rms of the scan after subtracting the fit.|
 ^mapping options:| For viewing maps or converting them to FITS or nod2 standards.| ^mapping options:| For viewing maps or converting them to FITS or nod2 standards.|
 |color| Shows color plots instead of black and white.| |color| Shows color plots instead of black and white.|
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 ==== Raw Data Processing ==== ==== Raw Data Processing ====
  
-The scripts and programs mostly use a file that contains all the scan numbers to be reduced. The scripts **log2scan.py** or **logbook2scan.py** produce such lists from observing logs written ​by log.py or Logbook.py, respectively+The scripts and programs mostly use a file that contains all the scan numbers to be reduced. The scripts **dblog2scan.py** or **dblog2scan_wea.py** produce such lists from observing logs written ​Obslogger. 
 + 
 +In dblog2scan.py one can optionally restrict the frequency by the receiver version and frequency in GHzif the log contains entries at different frequencies.
  
-In log2scan.py one can optionally restrict the frequency if the log contains entries at different frequencies. 
 <​code>​ <​code>​
-log2scan.py +ubach@observer4:​~$ dblog2scan_wea.py  
- ​Usage: ​log2scan.py log-file [freq GHz]+ 
 + ​Usage: ​dblog2scan.py log-file ​[receiver] ​[freq GHz] 
 + 
 +Give a frontend designation (e.g. 28.1) and additional a frequency
 </​code>​ </​code>​
  
-----+**dblog2scan.py** will just produce the files scans (input file for weather.py and corr_point.py) and scanlist (to be attached to the reduce.par file), **dblog2scan_wea.py** will produce an additional weather.dat file with weather information for each scan. The weather file is useful for the opacity correction described below.
  
 +----
 +\\
 The script **reduce.py** can be used to reduce a number of given scans using the toolbox with a list of options. Some example parameter files are stored in /​home/​obs2/​flux_monit/​reduce-par. E.g., reduc28.par for the 2.8cm SFK receiver. Calling just reduce.py prints out some help as well. The script **reduce.py** can be used to reduce a number of given scans using the toolbox with a list of options. Some example parameter files are stored in /​home/​obs2/​flux_monit/​reduce-par. E.g., reduc28.par for the 2.8cm SFK receiver. Calling just reduce.py prints out some help as well.
  
 <​code>​ <​code>​
-obs2@observer3:~$ reduce.py ​+obs2@observer9:~$ reduce.py ​
  
  ​Usage:​ reduce.py par-file  ​Usage:​ reduce.py par-file
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 Since the amplitudes from the toolbox are in units of the Tcal one just have to multiply the given numbers by the Tcal to get the correct system temperature. The reduce.py procedure provides an all.fit file that contains all the single fit-files. The further programs work with this all.fit. Since the amplitudes from the toolbox are in units of the Tcal one just have to multiply the given numbers by the Tcal to get the correct system temperature. The reduce.py procedure provides an all.fit file that contains all the single fit-files. The further programs work with this all.fit.
  
-The script **weather.py** reads the weather information ​for the MBFITS filesmultiplies the Tsys found in the all.fit by a given Tcal and prints out a weather.dat and a LIST.tsys, with the opacity information for each scan that is listed in the scanlist-file. The minimum zenith opacity is fitted from the Tsys vs. airmass distribution and is presented in the plot Opacities.eps. Weather.eps contains the weather info.+The script **weather.py** reads the weather information ​from the weather.dat file or directly from the MBFITS files. It multiplies the Tsys found in the all.fit by a given Tcal and prints out a LIST.tsys, with the opacity information for each scan that is listed in the scanlist-file. When the weather data is read from the raw MBFITS file the script will write a new weather.dat for alter use. The minimum zenith opacity is fitted from the Tsys vs. airmass distribution and is presented in the plot Opacities.eps. Weather.eps contains the weather info.
  
 <​code>​ <​code>​
-obs2@observer3:~$ weather.py ​+obs2@observer9:~$ weather.py ​
  Task to read weather data from MBFITS files,  Task to read weather data from MBFITS files,
  save them in ASCII format, and compute LIST.tsys.  save them in ASCII format, and compute LIST.tsys.
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 <​code>​ <​code>​
-obs2@observer3:~$ corr_point.py ​+obs2@observer9:~$ corr_point.py ​
    
  Task to reduce fit-files from Peters Toolbox  Task to reduce fit-files from Peters Toolbox
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 </​code>​ </​code>​
  
-For example the Tcal at 2.8cm is 7.5 K and scan numbers are stored in scanlist+For example the Tcal at 2.8cm is 7.5 K and scan numbers are stored in the file scans.
  
 <​code>​ <​code>​
-obs2@observer3:​~/​ubach/​measurements/​2011_03_16_poi/​2.8cm/​0.Raw$ corr_point.py ​scanlist ​7.5+obs2@observer3:​~/​ubach/​measurements/​2011_03_16_poi/​2.8cm/​0.Raw$ corr_point.py ​scans 7.5
  
  ​****************************************************  ​****************************************************
information_for_astronomers/user_guide/reduc_pointing.1478188149.txt.gz · Last modified: 2016/11/03 16:49 by ubach