**Table B.1:** The confusion limit reached by the IRAM 30-m telescope toward some molecular line sources.
Source	$\lambda$	Weakest	$t_{\rm int}^{a}$	Ref.^b
$\Delta v$		detect. lines
	mm	mK	h
IRC+10216	3	1.5	28	1)
28 km s^-1	2	3.5	10	1, 2)
	1.3	$\la$ 2	80	2)
Orion-KL	3	20	0.8	3)
5 km s^-1	2	50	0.3	4)
	1.3	70	0.4	3)
SgrB2(N)	3	$\sim$ 20	0.4	3)
$\sim$ 17 km s^-1	2	$\sim$ 30	0.4	3)
	1.3	$\sim$ 40	0.5	3)

^a Integration time (on+off) with present receivers at the IRAM 30-m telescope under normal winter conditions (good summer conditions), one polarization to obtain an rms of 1/3 $T_{\rm mb}$ with a velocity resolution of 1/5 the line width (one polarization receiver only).
^b References: 1) this paper 2) Ziurys et al. (2002); 3) unpublished data; 4) Mauersberger et al. (1988).
^c Weaker lines can be identified if one makes use of the unique line shapes of the spectra of this source (Cernicharo et al. 2004).

Source LaTeX | All tables | In the text