English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The disks around some Herbig Be stars have been observed to be more compactthan the expected dust sublimation radius for such objects, with highlyrefractory dust grains and optically thick gas emission having been proposed aspossible explanations for this phenomenon. Our aim is to search for directevidence for the presence of hot gas inside of the expected dust sublimationradius of MWC147. By combining VLTI/AMBER spectro-interferometry (R=12,000)with CRIRES spectroscopy (R=100,000) we can both spectrally and spatiallyresolve the Br-gamma line-emitting gas around MWC147. Our interferometricvisibility modelling of MWC147 indicates the presence of a compact continuumdisk with a close to face-on orientation. We model the continuum with aninclined Gaussian, as well as a ring with a radius of 0.60mas (0.39au) which iswell within the expected dust sublimation radius of 1.52au. We detect nosignificant change in the measured visibilities across the Br-gamma line,indicating that the line-emitting gas is located in the same region as thecontinuum-emitting disk. We fit our AMBER spectro-interferometry data with akinematic model of a disk in Keplerian rotation, with both the line-emittingand continuum-emitting components of the disk originating from the same compactregion close to the central star. The presence of line-emitting gas in the sameregion as the K-band continuum supports the interpretation that the K-bandcontinuum traces an optically-thick gas disk. Our spatially and spectrallyresolved observations of MWC147 reveal that the K-band continuum and Br-gammaemission both originate from a similar compact region, with Br-gamma emittedfrom the accretion disk or disk wind region and exhibiting a rotationalvelocity profile. We conclude that we detect the presence of a compact, gaseousaccretion disk in Keplerian rotation around MWC147.

A compact gaseous accretion disk in Keplerian rotation around MWC147