Evidence for an inner molecular disk around massive Young Stellar Objects

Details Evidence for an inner molecular disk around massive Young Stellar Objects Evidence for an inner molecular disk around massive Young Stellar Objects

2004-10-05

arxiv.org/abs/astro-ph/0410098v1

Astron.Astrophys. 427 (2004) L13-L16

Astronomy and Astrophysics

Astrophysics

accepted for publication in Astronomy and Astrophysics Letters

Scientific paper

10.1051/0004-6361:200400088

We present observations of CO overtone bandhead emission toward four massive Young Stellar Objects (spectral type O6--B5). The high signal-to-noise ratio K-band spectra were obtained with VLT-ISAAC at a resolution of 30 km/s, sufficient to resolve the bandheads, but not the individual J-lines. We are able to explain the shape of the lines by assuming a simple isothermal keplerian disk model seen at different inclinations. The gas temperature ranges from 1500 to 4500 K and the CO column density is between 0.1 and 4 10^21 cm^-2. The emission probably arises within the first few astronomical units of the disk, consistent with the high gas temperature. Our results indicate that molecules can survive close to a hot star and suggest that dense (n_H > 10^10 cm^-3) inner disks may be relatively common at an advanced stage of high-mass star formation.

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