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en:praktikum:versuche_master [2018/10/23 11:22] – schaffenrothen:praktikum:versuche_master [2023/04/19 16:43] (current) – [N1 - Stellar spectra of different spectral types] rhainich
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 ==== S1 - Solar Rotation ==== ==== S1 - Solar Rotation ====
  
 +<WRAP group>
 +<WRAP twothirds column>
 The sun will be observed during an excursion to the Einsteinturm (Einstein Tower) at the Telegrafenberg in Potsdam, The Einsteinturm is a tower telescope, consisting of a coelostat, a lens with a diameter of 60 centimetre, and a spectrograph that is 14 metre long. The data will be reduced with various software tools. Using the Doppler shift of solar spectral lines at the edge of the solar disk one can calculate the rotational period of the Sun.  The sun will be observed during an excursion to the Einsteinturm (Einstein Tower) at the Telegrafenberg in Potsdam, The Einsteinturm is a tower telescope, consisting of a coelostat, a lens with a diameter of 60 centimetre, and a spectrograph that is 14 metre long. The data will be reduced with various software tools. Using the Doppler shift of solar spectral lines at the edge of the solar disk one can calculate the rotational period of the Sun. 
  
 [[en:praktikum:sonnenrotation|Instructions: Solar Rotation]] [[en:praktikum:sonnenrotation|Instructions: Solar Rotation]]
  
 +</WRAP>
 +<WRAP third column>
 +[{{ost:spektrograph:spectra:sun_einsteinturm_rotation.png|Solar spectra taken at the Einstein Tower}}]
 +</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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 to assemble a small catalogue of spectra for different spectral types, including a (short) discussion of their respective properties.*/ For this purpose either a normal slit spectrograph ([[en:ost:spektrograph:grunddaten|DADOS]]) or a powerful echelle spectrograph ([[en:ost:spektrograph:grunddaten|BACHES]]) will be used in combination with a cooled [[en:ost:ccds:grunddaten|CCD camera]].  to assemble a small catalogue of spectra for different spectral types, including a (short) discussion of their respective properties.*/ For this purpose either a normal slit spectrograph ([[en:ost:spektrograph:grunddaten|DADOS]]) or a powerful echelle spectrograph ([[en:ost:spektrograph:grunddaten|BACHES]]) will be used in combination with a cooled [[en:ost:ccds:grunddaten|CCD camera]]. 
 /*A list with currently visible stars of different spectral classes (more than one object per spectral class) needs to be prepared to ensure an efficient observation.*/ /*A list with currently visible stars of different spectral classes (more than one object per spectral class) needs to be prepared to ensure an efficient observation.*/
-We will provide a list of currently visible stars of different spectral classes, 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 (modern version)]] 
 +\\ 
 +\\ 
 +[[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: 2018/10/23 11:22
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