The columns have the component designation (obviously binary components), the Julian Year, separation (mas) and position angle (deg from N), major and minor semi-axis of the error ellipse and its position angle.

To plot the data (and model, here xitau.model), I have read the model, computed the model values for the ASTROMETRY, and used Plot|ASTROMETRY to produce the ASTROMETRY plot widget. Choose Option|Orbit and Error, and this is what you will get.

Let's assume you don't have a model, what are the steps to derive one? First, plot the data and with Util|Ellipse and the mouse buttons interactively define an apparent ellipse to fit your data as best as you can. Don't try too hard, because you will improve the fit using Fit|ASTROMETRY. Select all ellipse parameters and click on Fit. The following figure demonstrates the procedure.

When you re-plot the data, it will show you the fitted ellipse. Now for a real treat. Under Util|Orbit, there is a Thiele-Innes procedure to estimate the orbital elements using your apparent ellipse and Kepler's laws! The results are shown here, with the orbit plotted (de-select Options|Ellipse, re-select Options|Orbit).

To improve the orbital elements, again using a Marquardt-Levenberg non-linear fit algorithm, use Fit|Orbit in the Fit widget already displayed. Once this is done, click on SetModel to transfer the orbital elements into your AMOEBA model (for this to work, you have to have a real or dummy model loaded, so that the data structure is available).

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