Free Access
Issue
A&A
Volume 562, February 2014
Article Number A26
Number of page(s) 17
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201322857
Published online 31 January 2014

Online material

thumbnail Fig. 12

Comparison of modeled and observed 12CO J = 6−5 intensity profiles and spectra, showing the effect of changing the inner radius of the gas disk at around 20 AU. Left panels: adopted surface density profiles with variations of the representative model. The red line is the representative model. Center panels: intensity profile extracted along the major axis of the disk. The vertical dashed line indicates the radius of the dust-free cavity. Right panels: total spectrum. The yellow region indicates regions affected by the foreground. Vertical dashed lines show the source velocity vs = 4.55 km s-1 and velocities vs ± 4 km s-1 representing velocity ranges corresponding to the inner disk (radii ≲60 AU). a) (Upper row) using the gas surface density profile of the representative model. b) (Lower row) by varying the surface density such that the emission at the stellar position is approximately reproduced.

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thumbnail Fig. 13

Comparison of modeled and observed 12CO J = 6−5 intensity profiles and spectra, showing the effect of an inner gas disk extending from 0.4−10 AU. The surface density profile outside 20 AU is set to the representative model. Left panels: adopted surface density profiles with variations of the representative model. The red line is the representative model. Center panels: intensity profile extracted along the major axis of the disk. The vertical dashed line indicates the radius of the dust-free cavity. Right panels: total spectrum. The yellow region indicates regions affected by the foreground. Vertical dashed lines show the source velocity vs = 4.55 km s-1 and velocities vs ± 4 km s-1 representing velocity ranges corresponding to the inner disk (radii ≲60 AU). a) (Upper row) adopting δ20  AU = 8 × 10-2−1. b) (Lower row) adopting δ20  AU = 8 × 10-5−8 × 10-3.

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thumbnail Fig. 14

Comparison of the intensity profile and total spectrum of the representative model convolved to the ALMA beam or simulated using the observed (u,   v)-coverage. Left panel: intensity profile extracted along the major axis of the disk. The vertical dashed line indicates the radius of the dust-free cavity. Right panel: total spectrum. The yellow region indicates regions affected by the foreground. Vertical dashed lines show the source velocity vs = 4.55 km s-1 and velocities vs ± 4 km s-1 representing velocity ranges corresponding to the inner disk (radii ≲60 AU).

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thumbnail Fig. 15

Comparison of modeled and observed 12CO J = 6−5 intensity profiles and spectra, showing the intensity profile and total spectrum of models with different slope γ of the gas and dust surface density profile (Σ ∝ rγ). Left panel: adopted surface density profiles with variations of the representative model. The red line is the representative model. Center panel: intensity profile extracted along the major axis of the disk. The vertical dashed line indicates the radius of the dust-free cavity. Right panel: total spectrum. The yellow region indicates regions affected by the foreground. Vertical dashed lines show the source velocity vs = 4.55 km s-1 and velocities vs ± 4 km s-1 representing velocity ranges corresponding to the inner disk (radii ≲60 AU).

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© ESO, 2014

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