High-contrast imaging of protoplanetary disks

1.6.8 Conclusions and future prospects • A reliable estimate of the disc gas mass can be made based on the spatially resolved observations of optically thin rotational line emission

Figure 2.8: Comparison of the observed vector-averaged 12 CO (top panel), 13 CO (middle panel) and C 18 O (lower panel) line fluxes (dots) to a model (full lines) which assumes the

They con- clude that the disc is relatively massive, M ≈ 0.1 M  with an uncertainty by a factor of a few, has an outer dust radius not greater than ≈400 AU set by the dark lane

In this Chapter we present spatially resolved observations of molecular gas and warm dust of DoAr 21, a young star with a ‘transitional’ SED, and show that such measurements

In our approach, we focus on the parameters to which the pre- sumably optically thick 12 CO J=3–2 line is most sensitive, disc size, inclination and temperature, and make

13 CO J=1–0 line spectra (black lines) compared to the synthetic line spec- tra (thick grey-white lines) from the disc models that fit the dust continuum emission, calculated without

• Line asymmetry seen in the 12 CO J=6–5 and J=3–2 lines can be explained by a temperature asymmetry, with one side of the disc slightly colder than the other, possibly due to a

Since the snow region and the gas mass and flaring parameter are shown to significantly change rm (inner radius), rm and the water emission lines could be compared for these