**Table 1:** Lines of ethylene glycol observed in comet Hale-Bopp.
Transition ^a	Frequency	$E_{\rm u}$	Telescope	Date	r	$\Delta$	Int.^b	$\int T_b {\rm d}v$ [mK km s^-1]
	[GHz]	[cm^-1]		dd/mm/yy	[AU]	[AU]	[min]	Model^c	Observed
12 _{1, 12, 0}-11 _{1,11, 1}	106.9074	25.3	IRAM 30-m	03/04/97	0.91	1.37	145	70 $\phantom{\rule[-1.5mm]{0.1mm}{4.2mm}}$	$75 \pm 16$
15 _{7, 9, 0}-14 _{7, 8, 1}	147.1318	57.7	IRAM 30-m	08/04/97	0.92	1.42	130	72	$181 \pm 26$
15 _{7, 8, 0}-14 _{7, 7, 1}	147.1324	57.7						92
16 _{8, 9, 0}-15 _{8, 8, 1}	157.2863	68.3	IRAM 30-m	05/04/97	0.92	1.39	85	94	$239 \pm 58$
16 _{8, 8, 0}-15 _{8, 7, 1}	157.2864	68.3						74
17 _{2,15, 0}-16 _{2,14, 1}	168.3863	54.9	IRAM 30-m	03/04/97	0.91	1.37	205	198 $\phantom{\rule[-1.5mm]{0.1mm}{4.2mm}}$	$194 \pm 63$
25 _{1,25, 0}-24 _{1,24, 1}	226.6433	102.7	IRAM 30-m	11/04/97	0.93	1.45	65	222	$440 \pm 76$
25 _{0,25, 0}-24 _{0,24, 1}	226.6435	102.7						284
21 _{5,16, 1}-20 _{5,15, 0}	227.3158	88.5	IRAM 30-m	05/04/97	0.92	1.39	310	178 $\phantom{\rule[-1.5mm]{0.1mm}{4.2mm}}$	$135 \pm 22$
23 _{2,21, 0}-22 _{3,20, 0}	227.5035	96.2						54 $\phantom{\rule[-1.5mm]{0.1mm}{4.2mm}}$	$72 \pm 22$
22 _{4,18, 0}-21 _{4,17, 1}	227.5871	94.0						214 $\phantom{\rule[-1.5mm]{0.1mm}{4.2mm}}$	$114 \pm 22$
24 _{3,22, 0}-23 _{3,21, 1}	230.5771	104.0	IRAM PdBI	6, 11/03/97	1.00	1.40	34	116	$192 \pm 18$
22 _{4,19, 1}-21 _{4,18, 0}	230.5783	92.3						98
25 _{10,16, 1}-24 _{10,15, 0}	263.3025	144.4	CSO	08/04/97	0.92	1.42	44	52	$53 \pm 16$
25 _{10,15, 1}-24 _{10,14, 0}	263.3026	144.4						40
29 _{1,29, 0}-28 _{1,28, 1}	263.3921	136.4	CSO	08/04/97	0.92	1.42	44	62	$121 \pm 21$
29 _{0,29, 0}-28 _{0,28, 1}	263.3921	136.4						82

^a The energy levels are noted here J_{K_a,K_b,v}, where v is the quantum number associated with OH tunneling motions (Christen & Müller 2003).
^b Integration time (on comet + comparison field).
^c Line area predicted by our LTE model (Crovisier et al. 2004) for a production rate of ethylene glycol of 0.002 relative to that of H₂O (which is 0.8 to $1.1 \times 10^{31}$ molec. s^-1). A uniform rotational temperature of 110 K and a spherical coma expanding with a velocity of 1.04 km s^-1 are assumed (Biver et al. 1999). $\beta$ is set to $2 \times 10^{-5}$ s^-1 at 1 AU.

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