Option 1:
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Use the JMMC Optical Interferometry database (https://oidb.jmmc.fr/index.html) to download
a reduced and calibrated interferometric dataset of your choice and do a basic analysis in PMOIRED.
The analysis should include displaying the data and fitting a basic model such as a point source,
uniform disk, Gaussian, or a binary star. Provide final parameter values with errors determined by
bootstrapping. For simple datasets, I recommend the VLTI instruments PIONIER or CHARA instruments
MIRC-X and MYSTIC. If the data are published, you can consult the corresponding paper for hints on
the analysis.

Option 2:
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Download one of the reduced and calibrated datasets from MIRC-X or MYSTIC for the Be star kappa Dra
from the JMMC Optical Interferometry database (https://oidb.jmmc.fr/index.html) and use the squared
visibilities to fit for a basic geometry of the Be star and its disk. Try fitting both
one-component (uniform disk or a Gaussian) and two-component models (e.g. a point source +
a Gaussian) to obtain an estimate of the disk inclination and projected angle on the sky. Choose
the preferred model and provide the final parameters values and errors determined by bootstrapping.

Option 3:
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Download the same dataset and in Option 2 and use the closure phases to try to obtain the relative
position of the faint subdwarf companion of the primary Be star with a grid search. If a reliable
fit cannot be obtained, determine the detection limit (a minimum magnitude difference between the
two components) of a possible companion.

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For all options, submit the results as a Jupyter notebook. For examples of similar PMOIRED
analyses, consult the official PMOIRED examples: https://github.com/amerand/PMOIRED_examples.