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information_for_astronomers:user_guide:faq [2014/12/11 08:22]
bwinkel [Previewing the data]
information_for_astronomers:user_guide:faq [2019/08/10 21:54] (current)
akraus
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 === How do I get to Effelsberg === === How do I get to Effelsberg ===
 [[information_for_astronomers:​user_guide:​hints|Observing at Effelsberg]]. [[information_for_astronomers:​user_guide:​hints|Observing at Effelsberg]].
 +
 +=== Contacting the operators ===
 +
 +The control room can be reached by phone via +49 2257 301 155. The operator'​s
 +mail address is operateure_at_mpifr.de .
  
 === What receivers/​instruments do you got? === === What receivers/​instruments do you got? ===
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 === What steps are necessary to calibrate my data? === === What steps are necessary to calibrate my data? ===
 The FITS files contain the Raw data (pure counts), while the "​reduced"​ spectra and continuum scans contained in the ''​Class''​ files are only partly calibrated by the pipeline. In fact, the pipeline removes the gain factor ("​bandpass"​) from the data using the position-switch or frequency-switch technique, but the result is in units of the noise diode'​s signal, $T_\mathrm{cal}$. You have to use calibration sources to measure $T_\mathrm{cal}$. For quick'​n'​dirty calibration you can use values from our [[information_for_astronomers:​rx_list|RX list]]. Furthermore,​ depending on observing frequency you will need to correct for elevation-dependent gain efficiency and atmospheric opacity. Details are discussed in a calibration memo by A. Kraus (on request) and partly in [[http://​adsabs.harvard.edu/​abs/​2012arXiv1203.0741W| A&A 540, A140, 2012]]. The FITS files contain the Raw data (pure counts), while the "​reduced"​ spectra and continuum scans contained in the ''​Class''​ files are only partly calibrated by the pipeline. In fact, the pipeline removes the gain factor ("​bandpass"​) from the data using the position-switch or frequency-switch technique, but the result is in units of the noise diode'​s signal, $T_\mathrm{cal}$. You have to use calibration sources to measure $T_\mathrm{cal}$. For quick'​n'​dirty calibration you can use values from our [[information_for_astronomers:​rx_list|RX list]]. Furthermore,​ depending on observing frequency you will need to correct for elevation-dependent gain efficiency and atmospheric opacity. Details are discussed in a calibration memo by A. Kraus (on request) and partly in [[http://​adsabs.harvard.edu/​abs/​2012arXiv1203.0741W| A&A 540, A140, 2012]].
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information_for_astronomers/user_guide/faq.txt ยท Last modified: 2019/08/10 21:54 by akraus