CO(6−5) and [C i](2−1) pointed observations of five protoplanetary disks: Warm gas in HD 142527

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Volume 553 (May 2013)

A&A, 553 (2013) A64

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Table 1

CHAMP+ observations of five protoplanetary disks.

	t^a	pwv^b	[C i](2−1)		CO(6−5)
			τ,T_sys^c	T_mb^d	τ,T_sys^c	T_mb^d

HD 142527	40	0.53	0.99, 3497	±2.05	0.88, 1338	1.03 ± 0.22^e
VV Ser	40	0.51	0.97, 4416	±2.65	0.85, 1544	±0.97
rxj 1842.9-35	40	0.48	0.84, 3941	±1.85	0.76, 1465	±0.71
HD 178253	70	0.44	0.80, 4455	±1.45	0.73, 1699	±0.56
HD 37389	50	0.40	0.75, 4475	±1.67	0.68, 1607	±0.64^f

Notes.All values preceded by “±” are the root-mean-square (rms) scatter noise in K, i.e. 1σ, without binning. Practical upper limits on the amplitude of Gaussian lines with a fwhm Δ_v are given by ≈, with 99.7% confidence, and where the channel widths δ_v are 0.068 km s^-1 in [C i](2−1) and 0.079 km s^-1 in CO(6−5).

^(a)

Duration of each observation, in mn, including overheads such as time on the reference positions, wobbler and slew times, and load calibrations;

^(b)

radiometer precipitable water vapour column, in mm;

^(c)

atmospheric opacity and system temperature (in K);

^(d)

main-beam temperature T_mb, in K, converted from with T_mb = 2.64 ;

^(e)

amplitude of Gaussian fit, with 1σ error bar. The unbinned rms scatter under the line was 0.79 K. See the text for Gaussian-fit parameters;

^(f)

extended emission in the central horn reaches T_mb ~ 1.4 K.

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