Resolving the hot dust around HD69830 and η Corvi with MIDI and VISIR

R. Smith; M. C. Wyatt; C. A. Haniff

doi:10.1051/0004-6361/200911626

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Volume 503 / No 1 (August III 2009)

A&A, 503 1 (2009) 265-279

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Table 3:

Measuring the significance of the dip in visibility of HD69830 at 10-11.5 $\mu$ m.
Baseline	Visibility
name	8-9 $\mu$ m	10-11.5 $\mu$ m	Ratio
A	0.944 $\pm$ 0.003	0.879 $\pm$ 0.005	0.931 $\pm$ 0.037
B	1.003 $\pm$ 0.003	0.928 $\pm$ 0.004	0.926 $\pm$ 0.027
C	1.093 $\pm$ 0.003	1.018 $\pm$ 0.004	0.931 $\pm$ 0.028
D	0.839 $\pm$ 0.006	0.803 $\pm$ 0.005	0.958 $\pm$ 0.039
$V_{\rm {res}}$	0.990	0.860	0.869

The values of visibility in each wavelength range are the weighted means taken over all spectral channels in that range, and uncertainties quoted are the standard errors on the weighted mean from statistical uncertainty only (uncertainty in the absolute visibility is higher due to calibration uncertainties). Final error on ratio includes error from the calibrator ratios discussed in Sect. 2.4 and a 1.3% error on the spectral slope of IRS observations (Beichman et al. 2006), as well as the statistical errors from each wavelength range. The $V_{\rm {res}}$ predicted visibility arises from assuming that $V_{\rm {disc}}=0$ (see Eq. (4)).

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