Gas and dust in the inner protoplanetary disk: Combining CO ro-vibrational and NIR interferometry datasets

Both CRIRES and PIONIER have been used to explore protoplanetary disks. However, so far no large sample of protoplanetay disks has been looked at using CRIRES CO lines and PIONIER interferometry. The aim of this thesis is to create co-added CO ro-vibrational line profiles using CRIRES data to determine the inner radius of the CO gas. This is then compared with the inner dust radius of the same objects obtained with PIONIER. This is done using a self made IDL based program to co-add the CO lines and an IDL based program provided by Andres Carmona to fit these co-added line profiles using a single component intensity power law to calculate the χ2. We separate the objects depending on how well the object could be fit using this power law. For the objects that were well fit we found a strong confirmation of the relation between the HW10% and 1.7 × HWHM as well as a relation between the HW10% and the best fit for the inner radius. For high χ2 objects we found indication of a multi-component power law and for low signal-to-noise objects we found that the degeneracies made it impossible to estimate the inner CO radius. A number of suggestions are done regarding further observations and fitting attempts for these objects.