Also, the Help button of the software gives access to detailed explanations.

The following steps guide you to some basic operations:

• the main window is dominated by a display of the sky, as seen at the current time, looking in south direction (azmimuth = 180°). The blue dots mark a number of astronomical sources, for instance G30 is the position in the Galactic Plane at Galactic Longitude of 30°. The shaded areas indicate foreground objects, such as the ISU library and trees on the southern horizon.
• with the buttons +1 hr and -1 hr you can step forward and backward in time, Now brings you back to the current time.
• step forward or backward in time, until you see the Galactic Plane between the Galactic Centre (SgrA = Sagittarius A) and G90 and all the positions inbetween.
• click on any of those G-sources, say G40. Then the telescope will move from its "stow" position to the requested source position
• it takes a few seconds to reach the source - in reality it takes a bit longer. When it is reached, the spectrum display in the upper center will show the simulated spectrum. The black curve is the current spectrum, the red curve is the average over all spectra taken at that source.
• since the default spectral span of 500 kHz will show only a portion of the simulated galactic signal, you might find it more convenient to select with the choice at right centre a larger span, such as 2000 kHz span, and/or to shift the centre frequency a bit. Whatever your choice, click the green OK button to make the selection.
• larger frequency spans take more time - the default span of 500 kHz takes one second per spectrum, 2000 kHz takes four seconds!
• you will see the results in the spectrum display. If you click at any position within this plot, the frequency will be displayed in blue letters below the frequency menu on the right.
• the colour display near the upper rightish centre is a false colour waterfall display, showing the spectra in the form of a coloured bar, and placing one spectrum below the previous ones. The rainbow colours give an indication of the intensity at each frequency. When you have a spectral feature - like from one of the positions between SgrA and G90 - this feature will show up as in a 'brighter' colour, and as one stays at the same position, this will form a vertical band of that colour. In the simulated data generated in the trainer applet, nothing else will happen; however, in reality, this display is very important for identification of any interference: any momentary interference or fluctuation of the system sensitivity shows up as a horizontal band with changed colours, any narrow band interference might show up as a 'bright' signal at some frequency for some time ...
• other sources whose signal is simulated are: the Sun, Moon, CasA, M31, CygA ... but all except the Sun are very weak, as in reality!

• to record measurements, click on Record button to start the recording. Recording ist stopped by another click on Record. The file is labeled with the date and time of the start of recording, e.g. 1005301300.txt is from May 30th, 2010, and started at 1300 UT. You find the file in the folder c:/SRTcassi/

• the Help button opens a window with more explanations.
• there are options by the other buttons as well as more details which I did not cover in this brief "tutorial"
• WARNING: it might be that some details in the explanations are still missing or need to be updated ;-)