en:praktikum:sternspektren_baches

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en:praktikum:sternspektren_baches [2025/01/07 13:14] – [Reduce the data] rhainichen:praktikum:sternspektren_baches [2025/04/02 09:10] (current) – [Reduce the data] rhainich
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    Star_1/    Star_1/
-      Darks/ +      darks/ 
-      Flatdarks/ +      flat_darks/ 
-      Flats/+      ThAr_darks/ 
 +      flats/
       ThAr/       ThAr/
       Star_1/       Star_1/
    Star_2/    Star_2/
-      Darks/ +      darks/ 
-      Flatdarks/+      flat_darks/
       ...       ...
  
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 </code> </code>
  
-In ''path_darks'', ''path_flat_darks'', ''path_flats'', ''path_wavelength_darks'', ''path_wavelength'', and ''path_spectra'' the corresponding subfolders are to be entered, which were created in section //Preparations//. ''out_path'' is the directory where the script places intermediate results. The reduced files (**master_dark.fit**, **master_flat.fit**, **master_wave.fit**, **master_spectrum.fit**) are stored in the local directory so that they are more easily available for the following analysis steps. +In ''path_darks'', ''path_flat_darks'', ''path_flats'', ''path_wavelength_darks'', ''path_wavelength'', and ''path_spectra'' the corresponding subfolders are to be entered, which were created in section //Preparations//. The variable ''path_wavelength_darks'' can be set to **'?'** if no darks were taken for the ThAr exposures. ''out_path'' is the directory where the script places intermediate results. The reduced files (**master_dark.fit**, **master_flat.fit**, **master_wave.fit**, **master_spectrum.fit**) are stored in the local directory so that they are more easily available for the following analysis steps. 
  
 If you want to mirror the recordings you have to set ''flip_images'' to ''True''. If the images should also be binned, set ''bin_images'' to ''True''. The binning factor can be determined via the variable ''binning_value''. If you want to mirror the recordings you have to set ''flip_images'' to ''True''. If the images should also be binned, set ''bin_images'' to ''True''. The binning factor can be determined via the variable ''binning_value''.
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 The identification of the individual orders, the identification of the emission lines in the ThAr spectrum, and the correlation between the pixel and the wavelength scale is performed by the //MIDAS// script ''calibrate/baches''. The call could look like: The identification of the individual orders, the identification of the emission lines in the ThAr spectrum, and the correlation between the pixel and the wavelength scale is performed by the //MIDAS// script ''calibrate/baches''. The call could look like:
  
-   calibrate/baches master_flat.fit master_thar.fit 26 26 24+   calibrate/baches master_flat.fit master_wave.fit 26 26 24
  
 The five parameters have the following meaning: The five parameters have the following meaning:
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    ===============================    ===============================
    Flat field  = master_flat.fit    Flat field  = master_flat.fit
-   Calibration lamp = master_thar.fit+   Calibration lamp = master_wave.fit
    Calibration table = thar.fit    Calibration table = thar.fit
    Num. of orders  = 0026    Num. of orders  = 0026
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 In this case, the script should be stopped by entering a ''2''. Afterwards the script can be restarted with a reduced number of orders, e.g.: In this case, the script should be stopped by entering a ''2''. Afterwards the script can be restarted with a reduced number of orders, e.g.:
  
-   calibrate/baches master_flat.fit master_thar.fit 23 20 20+   calibrate/baches master_flat.fit master_wave.fit 23 20 20
  
 A solid method is to gradually reduce the number of orders until the script executed successfully. Afterwards, the flatfield with the identified orders will be displayed in an external window (see below). It should be checked whether the marks of the orders are horizontal and whether they coincide with the actual orders that are visible on the flatfield. The left figure shows a successful test run, whereas the middle figure depicts a failure. The right figure shows a flatfield image taken with the QHY268M, where it can happen that //MIDAS// does not finish drawing all identified orders. From the order numbers, however, it can be assessed if all orders were successfully identified or not. The numbers also depend on whether the images are binned. As we usually use 2x2 binning, the above values should suffice. In case we have used 1x1 binning for the spectra however, you might have to double the second and third value. A solid method is to gradually reduce the number of orders until the script executed successfully. Afterwards, the flatfield with the identified orders will be displayed in an external window (see below). It should be checked whether the marks of the orders are horizontal and whether they coincide with the actual orders that are visible on the flatfield. The left figure shows a successful test run, whereas the middle figure depicts a failure. The right figure shows a flatfield image taken with the QHY268M, where it can happen that //MIDAS// does not finish drawing all identified orders. From the order numbers, however, it can be assessed if all orders were successfully identified or not. The numbers also depend on whether the images are binned. As we usually use 2x2 binning, the above values should suffice. In case we have used 1x1 binning for the spectra however, you might have to double the second and third value.
  • en/praktikum/sternspektren_baches.1736255645.txt.gz
  • Last modified: 2025/01/07 13:14
  • by rhainich