CO observations of water-maser post-asymptotic giant branch stars and detection of a high-velocity outflow in IRAS 15452–5459

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Table 2

Characteristics of CO observations in water fountain sources.

IRAS ID	OH	Coordinates		V _LSR ^a	Date	CO	rms^b
		α _J2000	δ _J2000	(km s^-1)	of observation	transition	mK

18327−0715	024.692 + 00.235^c	18:35:29.82	–07:13:09.4	42.0	2010-07-06	2−1	77
					2010-07-07	3−2	19
					2010-07-09	6−5	48
					2010-07-09	7−6	165
18043−2116	009.097−00.392^c	18:07:21.20	–21:16:14.0	87.3	2010-07-05,06	2−1	79
					2010-07-07	3−2	26
					2010-07-09	6−5	91
					2010-07-09	7−6	298
15103−5754	320.9063−00.2929^d	15:14:18.47	–58:05:20.9	–47.0	2010-07-06	2−1	71
					2010-07-07	3−2	22
19190 + 1102	046.2559−01.4764^d	19:21:25.30	+11:08:40.0	50.0	2010-07-06	2−1	53
					2010-07-07	3−2	25
–	012.816−00.895^c	18:16:49.23	–18:15:01.8	–55.8	2010-07-05,06	2−1	25
					2010-07-07	3−2	23
18103−1738	012.973 + 00.133^c	18:13:20.24	–17:37:17.3	17.0	2010-11-16	2−1	35

Notes.

^(a)

Object LSR radial velocity from Deacon et al. (2004) and Deacon et al. (2007).

^(b)

Noise rms level of the spectrum given per bin of 1 km s^-1 and in the T_mb units.

^(c)

From Sevenster (2002)

^(d)

From SIMBAD (http://simbad.u-strasbg.fr/simbad/).

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