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We study the geometry and the physical conditions in the inner (AU-scale)circumstellar region around the young Herbig Be star MWC 147 usinglong-baseline spectro-interferometry in the near-infrared (NIR K-band,VLTI/AMBER observations and PTI archive data) as well as the mid-infrared (MIRN-band, VLTI/MIDIobservations). The emission from MWC 147 is clearly resolvedand has a characteristic physical size of approx. 1.3 AU and 9 AU at 2.2 micronand 11 micron respectively (Gaussian diameter). The spectrally dispersed AMBERand MIDI interferograms both show a strong increase in the characteristic sizetowards longer wavelengths, much steeper than predicted by analytic disk modelsassuming power-law radial temperature distributions. We model theinterferometric data and the spectral energy distribution of MWC 147 with 2-D,frequency-dependent radiation transfer simulations. This analysis shows thatmodels of spherical envelopes or passive irradiated Keplerian disks (withvertical or curved puffed-up inner rim) can easily fit the SED, but predictmuch lower visibilities than observed; the angular size predicted by suchmodels is 2 to 4 times larger than the size derived from the interferometricdata, so these models can clearly be ruled out. Models of a Keplerian disk withoptically thick gas emission from an active gaseous disk (inside the dustsublimation zone), however, yield a good fit of the SED and simultaneouslyreproduce the absolute level and the spectral dependence of the NIR and MIRvisibilities. We conclude that the NIR continuum emission from MWC 147 isdominated by accretion luminosity emerging from an optically thick innergaseous disk, while the MIR emission also contains contributions from theouter, irradiated dust disk.

astrophysical journal/the astrophysical journal

Detection of an inner gaseous component in a Herbig Be star accretion  disk: Near- and mid-infrared spectro-interferometry and radiative transfer  modeling of MWC 147