| Issue |
A&A
Volume 540, April 2012
|
|
|---|---|---|
| Article Number | L12 | |
| Number of page(s) | 5 | |
| Section | Letters | |
| DOI | https://doi.org/10.1051/0004-6361/201219126 | |
| Published online | 05 April 2012 | |
Online material
 |
Fig. 2
Normalized flux, squared visibility amplitudes, UD diameters, and closure phases (from top to bottom) of VY CMa obtained with the MR-K 2.1 μm mode (PA −89deg). The top panels also show fits of a UD (red) and a PHOENIX atmosphere model (blue). In these model visibility fits, the stellar component contributes ~50% of the total flux, and the remaining part is attributed to an over-resolved dust shell. The observed and model flux spectra show different slopes because of the additional dust shell that is not present in the model, and we have subtracted a best-fit linear function for a better comparison of the spectral features. The slopes that have been compensated are indicated by the dashed lines. |
| Open with DEXTER | |
 |
Fig. 3
As Fig. 2, but for the MR-K 2.3 μm mode (PA − 89deg). |
| Open with DEXTER | |
 |
Fig. 5
As Fig. 4, but for a near-continuum bandpass in the H-band at 1.70–1.75 μm. |
| Open with DEXTER | |
© ESO, 2012
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