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The formation scenario for massive stars is still under discussion. To further constrain
current theories, it is vital to spatially resolve the structures from which material
accretes onto massive young stellar objects (MYSOs). Due to the small angular extent of
MYSOs, one needs to overcome the limitations of conventional thermal infrared imaging,
regarding spatial resolution, in order to get observational access to the inner structure
of these objects. We employed mid-infrared interferometry, using the MIDI instrument on
the ESO/VLTI, to investigate the Kleinmann-Wright Object, a massive young stellar object
previously identified as a Herbig Be star precursor. Dispersed visibility curves in the
N-band (8–13 μm) have been obtained at
5 interferometric baselines. We show that the mid-infrared emission region is resolved. A
qualitative analysis of the data indicates a non-rotationally symmetric structure, e.g.
the projection of an inclined disk. We employed extensive radiative transfer simulations
based on spectral energy distribution fitting. Since SED-only fitting usually yields
degenerate results, we first employed a statistical analysis of the parameters provided by
the radiative transfer models. In addition, we compared the ten best-fitting
self-consistent models to the interferometric observations. Our analysis of the
Kleinmann-Wright Object suggests the existence of a circumstellar disk of
0.1 M⊙ at an intermediate inclination of 76°, while an
additional dusty envelope is not necessary for fitting the data. Furthermore, we
demonstrate that the combination of IR interferometry with radiative transfer simulations
has the potential to resolve ambiguities arising from the analysis of spectral energy
distributions alone
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