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information_for_astronomers:user_guide:pyonlplot
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information_for_astronomers:user_guide:pyonlplot [2012/11/16 11:48] 127.0.0.1 external edit |
information_for_astronomers:user_guide:pyonlplot [2022/06/27 17:11] (current) rkisky |
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| //Fig. 8: Spectroscopy data.// | //Fig. 8: Spectroscopy data.// | ||
| - | To produce maps, the user has to define a spectral interval first. Just click into the spectrum and press 'w' to set a window (indicated by green lines). With 'c' you can clear the window. When a window is set and the user clicks the //Plot button// a map is generated, or strictly speaking two maps: the first shows the **line** as color image, the second is overplotted as contours and visualizes the **continuum**. Numerically, the average of the flux outside the window, i.e. in the adjacent 200 spectral channels, is used as a proxy for continuum. The average of the flux inside the window minus this continuum defines the line map. Therefor, values in the map are Intensities in units of Tcal per channel (not per Hz or km/s!). All maps are also written as a fits-image into **/tmp**. Don't forget to copy the image file to your home directory if you want to keep it. (The Karma software is installed on observer2 and can be used to display the fits maps.) An example is shown in Figs. 9 and 10. | + | To produce maps, the user has to define a spectral interval first. Just click into the spectrum and press **'w'** to set a window (indicated by green lines). With **'c'** you can clear the window. When a window is set and the user clicks the //Plot button// a map is generated, or strictly speaking two maps: the first shows the **line** as color image, the second is overplotted as contours and visualizes the **continuum**. Numerically, the average of the flux outside the window, i.e. in the adjacent 200 spectral channels, is used as a proxy for continuum. The average of the flux inside the window minus this continuum defines the line map. Therefor, values in the map are Intensities in units of Tcal per channel (not per Hz or km/s!). All maps are also written as a fits-image into **/tmp**. Don't forget to copy the image file to your home directory if you want to keep it. (The Karma software is installed on observer2 and can be used to display the fits maps.) An example is shown in Figs. 9 and 10. |
| {{:information_for_astronomers:user_guide:w3main_absorption_profile.png?514|Using a spectral interval for mapping.}}\\ | {{:information_for_astronomers:user_guide:w3main_absorption_profile.png?514|Using a spectral interval for mapping.}}\\ | ||
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