Evidence for CO depletion in the inner regions of gas-rich protoplanetary disks

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Table 3:

Spatial information for the *averaged* vibrational transitions shown in Figs. 5 and 7, and the radii used to model the kinematics.
HD 97048	cont.	v(2-1)	v(3-2)	v(4-3)	$R_{\rm in, out}^{\rm model}$
SPP [AU]	0	$14.8^{\pm 0.9}$	$16.5^{\pm 2.7}$	-	11
FWHM [AU]^a	$21.2^{\pm 1.6}$	$\geq$ 23.8 $^{\pm 1.1}$	$\geq$ $23.0^{\pm 1.1}$	-	100
HD 100546
SPP [AU]	0	$9.6^{\pm 0.5}$	$9.4^{\pm 0.5}$	$9.9^{\pm 1.5}$	8
FWHM [AU]	$10.0^{\pm 0.9}$	$\geq$ $13.7^{\pm 0.6}$	$\geq$ $13.1^{\pm 0.6}$	$\geq$ $11.5^{\pm 0.7}$	100

^a Note that this FWHM is a function of continuum + line emission, but that the SPP has been corrected for the continuum dilution, and thus is a direct function of the CO emission. All values are directly derived from the 2D spectrum, and not the maximum value resulting from an alignment of the slit with the semi-major axis.

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