Water isotopologues in the circumstellar envelopes of M-type AGB stars

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Table 2

H₂O isotopologue observations using HIFI.

Molecule	Transition	ν	E_up	θ	IK Tau	R Dor	W Hya	R Cas
		[GHz]	[K]	[′′]	[K km s^-1]	[K km s^-1]	[K km s^-1]	[K km s^-1]

o-H₂¹⁷O	3_1,2 → 3_0,3	1096.414	249	19	1.97	1.46	0.56	<0.49^*
	3_0,3 → 2_1,2	1718.119	196	12	<2.7^*	–	1.66	–
p-H₂¹⁷O	1_1,1 → 0_0,0	1107.167	53	19	1.49	0.92	0.58	<0.37^*
o-H₂¹⁸O	3_1,2 → 3_0,3	1095.627	249	19	3.06	2.56	1.87	0.57
p-H₂¹⁸O	1_1,1 → 0_0,0	1101.698	53	19	4.23	2.25	1.85	0.86

Notes. E_up is the energy of the upper level in the transition, θ is the half-power beam width of the telescope at the corresponding frequency. The integrated line intensity is given for each source and transition. (–) Indicates a line not covered by the Herschel/HIFI observations and

^(*)

indicates a non-detection or a marginal detection, primarily used as an upper limit.

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