Methanol maps of low-mass protostellar systems - I. The Serpens molecular core

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Volume 516 (June-July 2010)

A&A, 516 (2010) A57

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Table 1:

Integrated line intensities, $\int T_{\rm MB}\ {\rm d}\varv$ (K km s^-1) over the central 22 $.\!\!^{\prime\prime}$ 5 $\times$ 22 $.\!\!^{\prime\prime}$ 5 of each source^a and emission-weighted, average line-widths.
Transition	$\nu$ (GHz)^b	$E_{\rm up}$ (K)^b	SMM1	SMM3	SMM4	S68N	SMM1-S	SMM4-W	SMM4-S
+0E	338.1245	78.1	0.25	0.22	0.30	0.85	...	0.09	0.41
-1E	338.3446	70.5	0.58	0.45	1.09	2.90	0.52	0.90	1.38
+0A	338.4087	65.0	0.71	0.62	1.35	3.66	1.06	1.26	2.21
-2A	338.5129	102.7	0.06	0.01	...	0.24	0.08	0.20	...
$\pm$ 3A^c	338.5420	114.8	0.11	0.16	0.15	0.40	...	...	...
+1E	338.6150	86.1	0.16	0.08	0.18	0.45	...	0.34	...
+2A	338.6399	102.7	0.09	0.07	...	0.26	...	...	...
$\pm$ 2E^c	338.7223	89.1	0.21	0.16	0.28	1.05	...	0.13	0.11
$\Delta\varv$ (km s^-1)			$3.4 \pm 0.9$	$4.4 \pm 2.5$	$4.0 \pm 0.7$	$7.2 \pm 1.3$	$4.3 \pm 0.9$	$4.0 \pm 0.3$	$4.1 \pm 0.3$

Notes. ^(a) Non-detections are marked by ``...'', for which an upper limit of 0.03 K km s^-1 applies. ^(b) Frequencies and upper level energies are from the Cologne Database for Molecular Spectroscopy (CDMS; Müller et al. 2001). ^(c) Lines are blended. The frequencies and upper level energies are average values.

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