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en:praktikum:versuche_master [2021/06/21 13:59] – [S1 - Solar Rotation] rhainichen:praktikum:versuche_master [2024/09/18 06:13] (current) – [N2 - Photometry of open star clusters] rhainich
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 </WRAP> </WRAP>
 </WRAP> </WRAP>
 +
 ==== S2 - Estimating the magnetic field strength of a sunspot ==== ==== S2 - Estimating the magnetic field strength of a sunspot ====
  
 +<WRAP group>
 +<WRAP twothirds column>
 Another observation of the sun at the Einsteinturm will focus on a sunspot. The slit of the spectrograph will be placed on the position of a sunspot to take the spectrum there. From the Zeeman-splitting of the spectral lines one can calculate the magnetic field strength of the sunspot. Another observation of the sun at the Einsteinturm will focus on a sunspot. The slit of the spectrograph will be placed on the position of a sunspot to take the spectrum there. From the Zeeman-splitting of the spectral lines one can calculate the magnetic field strength of the sunspot.
  
 [[en:praktikum:Sonnenspektroskopie|Instructions: Estimating the Magnetic Field Strength of a Sunspot]] [[en:praktikum:Sonnenspektroskopie|Instructions: Estimating the Magnetic Field Strength of a Sunspot]]
 +
 +</WRAP>
 +<WRAP third column>
 +[{{ost:gallery:sunsystem:sun_spots.jpg| Sunspots: imaged with the St-8 and the C11}}]
 +</WRAP>
 +</WRAP>
  
  
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 ==== N1 - Stellar spectra of different spectral types ==== ==== N1 - Stellar spectra of different spectral types ====
  
 +<WRAP group>
 +<WRAP twothirds column>
 The aim of this observation is to identify the spectral types of several stars using their spectral properties and to derive their radial velocities.  The aim of this observation is to identify the spectral types of several stars using their spectral properties and to derive their radial velocities. 
 We provide a spectral atlas of all spectral classes that can be used to identify the spectral class and a linelist of important lines.  We provide a spectral atlas of all spectral classes that can be used to identify the spectral class and a linelist of important lines. 
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 We will provide a list of currently visible stars of different spectral classes on the night of the observation, which will be observed and classified. We will provide a list of currently visible stars of different spectral classes on the night of the observation, which will be observed and classified.
 The spectra are reduced and calibrated with provided scripts.   The spectra are reduced and calibrated with provided scripts.  
 +
 +=== BACHES spectrograph ===
 +
 +[[en:praktikum:sternspektren_baches|Instructions: Stellar spectra of different spectral types (BACHES)]]
  
 === DADOS spectrograph === === DADOS spectrograph ===
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 [[en:praktikum:sternspektren|Instructions: Stellar spectra of different spectral types (DADOS)]] [[en:praktikum:sternspektren|Instructions: Stellar spectra of different spectral types (DADOS)]]
  
-=== BACHES spectrograph ===+</WRAP> 
 +<WRAP third column> 
 +[{{ost:spektrograph:spectra:beteigeuze_comp_large.png|DADOS spectra from Betelgeuse}}] 
 +</WRAP> 
 +</WRAP>
  
-[[en:praktikum:sternspektren_baches|Instructions: Stellar spectra of different spectral types (BACHES)]] 
  
 ==== N2 - Photometry of open star clusters ==== ==== N2 - Photometry of open star clusters ====
  
 +<WRAP group>
 +<WRAP twothirds column>
 During the accompanying seminar several talks on CCDs, photometry, and the data reduction will give an introduction to this observation. The observations will be carried out either at the [[en:ost:index|OST]] or at the 25.5" (70cm) reflecting telescope at the observatory of the AIP (Leibniz-Institut für Astrophysik Potsdam) in Babelsberg. Images of the open clusters as well as the necessary calibration data will be taken in different filters with a cooled [[en:ost:ccds:grunddaten|CCD camera]]. The data will be reduced and evaluated using provided and self-written software. At the end a colour-magnitude diagram shall be constructed for each open cluster, from which e.g. the age of the cluster can then be estimated. During the accompanying seminar several talks on CCDs, photometry, and the data reduction will give an introduction to this observation. The observations will be carried out either at the [[en:ost:index|OST]] or at the 25.5" (70cm) reflecting telescope at the observatory of the AIP (Leibniz-Institut für Astrophysik Potsdam) in Babelsberg. Images of the open clusters as well as the necessary calibration data will be taken in different filters with a cooled [[en:ost:ccds:grunddaten|CCD camera]]. The data will be reduced and evaluated using provided and self-written software. At the end a colour-magnitude diagram shall be constructed for each open cluster, from which e.g. the age of the cluster can then be estimated.
  
-[[en:praktikum:photometrie|Instructions: Photometry of open clusters]]+[[en:praktikum:photometrie_python|Instructions: Photometry of open clusters]] 
 +\\ 
 +/* 
 +\\ 
 +[[en:praktikum:photometrie|Instructions: Photometry of open clusters (GDL, old version)]] 
 +*/ 
 + 
 +</WRAP> 
 +<WRAP third column> 
 +[{{ost:gallery:starclusters:m36.jpg|M 36}}] 
 +</WRAP> 
 +</WRAP> 
  
 ===== Data analysis at the computer ===== ===== Data analysis at the computer =====
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  • Last modified: 2021/06/21 13:59
  • by rhainich