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information_for_astronomers:user_guide:reduc_pointing
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| Both sides previous revision Previous revision Next revision | Previous revision Next revision Both sides next revision | ||
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information_for_astronomers:user_guide:reduc_pointing [2016/11/03 17:00] ubach [Raw Data Processing] |
information_for_astronomers:user_guide:reduc_pointing [2021/02/10 16:36] akraus |
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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 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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| 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 files, multiplies 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> | ||
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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 |
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information_for_astronomers/user_guide/reduc_pointing.txt ยท Last modified: 2022/07/04 20:35 by twedel
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