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information_for_astronomers:user_guide:reduction_of_spectroscopic_measurements [2018/12/12 16:13]
akraus
information_for_astronomers:user_guide:reduction_of_spectroscopic_measurements [2018/12/12 16:18] (current)
akraus
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-===== Reducing spectral line data =====+====== Reducing spectral line data ======
  
 The raw data (in MBFITS format) are converted to CLASS format automatically. This is done using the method described in Winkel, Kraus, & Bach, //Unbiased flux calibration methods for spectral-line radio observations//, [[http://adsabs.harvard.edu/abs/2012arXiv1203.0741W| A&A 540, A140, 2012]] (Section 3.4 and Section 4.5) - assuming a //constant system temperature// (Tsys) and //flat calibration signal// (Tcal). The latter is produced by a noise diode the power of which is in most cases directly fed into the waveguide within the receiver. //Neglecting the frequency-dependence of Tsys and Tcal introduces a bias, especially for wide-band observations!// (For more information see Winkel, Kraus, & Bach 2012 where we also show ways to do it better.) The raw data (in MBFITS format) are converted to CLASS format automatically. This is done using the method described in Winkel, Kraus, & Bach, //Unbiased flux calibration methods for spectral-line radio observations//, [[http://adsabs.harvard.edu/abs/2012arXiv1203.0741W| A&A 540, A140, 2012]] (Section 3.4 and Section 4.5) - assuming a //constant system temperature// (Tsys) and //flat calibration signal// (Tcal). The latter is produced by a noise diode the power of which is in most cases directly fed into the waveguide within the receiver. //Neglecting the frequency-dependence of Tsys and Tcal introduces a bias, especially for wide-band observations!// (For more information see Winkel, Kraus, & Bach 2012 where we also show ways to do it better.)
 
information_for_astronomers/user_guide/reduction_of_spectroscopic_measurements.txt · Last modified: 2018/12/12 16:18 by akraus     Back to top