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MEN89B - Hot Water around Late-Type Stars: Detection of Two Millimeter-Wave Emission Lines from the nu 2 Vibrationally Excited State

Short title: Menten & Melnick (1989)
Authors: Menten, Karl M.Melnick, Gary J.
Journal: Astrophysical Journal Letters v.341, p.L91
Bibcode:

Target type: star,pAGB_PN
Transitions: H2O_96,H2O_232

Abstract
The first astronomical detection of two millimeter-wave emission lines from vibrationally excited water is reported. The 96 GHz 4(40)-5(33) and the 232 GHz 5(50)-6(43) rotational transitions within the nu2 vibrationally excited state of H2O have been discovered toward the supergiant star VY CMa. The latter transition was also detected toward the semiregular variable W Hya. The 4(40)-5(33) transition shows definite signs of maser action while the 5(50)-6(43) emission may be of (quasi-)thermal nature. Based on a comparison of the line profiles of the 22 GHz H2O masers, various SiO maser lines, and the nu2 H2O emission, it is concluded that the vibrationally excited H2O and the SiO masers probably arise from a region in which the expansion of the circumstellar envelope has not yet begun and some infalling motions are present. This region is closer to the star than the part of the envelope that gives rise to the 22 GHz H2O masers.

Abstract

The first astronomical detection of two millimeter-wave emission lines from vibrationally excited water is reported. The 96 GHz 4(40)-5(33) and the 232 GHz 5(50)-6(43) rotational transitions within the nu2 vibrationally excited state of H2O have been discovered toward the supergiant star VY CMa. The latter transition was also detected toward the semiregular variable W Hya. The 4(40)-5(33) transition shows definite signs of maser action while the 5(50)-6(43) emission may be of (quasi-)thermal nature. Based on a comparison of the line profiles of the 22 GHz H2O masers, various SiO maser lines, and the nu2 H2O emission, it is concluded that the vibrationally excited H2O and the SiO masers probably arise from a region in which the expansion of the circumstellar envelope has not yet begun and some infalling motions are present. This region is closer to the star than the part of the envelope that gives rise to the 22 GHz H2O masers.

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Detection table from Menten & Melnick (1989)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Line	V_range	∫T_a dv	Telescope	RMS	Beam	Detection	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)				H₂O	(km/s)	(K*km/s)		(K)	(arcsec)	Yes/No	(kpc)
1	07 20 54.5	-25 40 10	239.0487	-5.4317	G239.049-5.432	VY CMa	Image	5(50)->6(43);	6.4;34.8	2.8 (0.1)	IRAM	0.023	12	+H₂O		1989 January 24
2	07 20 54.5	-25 40 10	239.0487	-5.4317	G239.049-5.432	VY CMa		4(40)->5(35);	20.8;23.9	4.2 (0.1)	IRAM	0.021	25	+H₂O		1989 January 24
3	07 20 54.5	-25 40 10	239.0487	-5.4317	G239.049-5.432	VY CMa		22 GHz;	-8.5;45.1	18700 (100)	EFF	0.460	40	+H₂O		1989 January 31
4	13 46 12.1	-28 07 09	317.3801	33.2115	G317.380+33.212	W Hya	Image	5(50)->6(43);	32;47	0.7 (0.1)	IRAM	0.016	12	+H₂O		1989 January 24
5	13 46 12.1	-28 07 09	317.3801	33.2115	G317.380+33.212	W Hya		22 GHz;	33.6;46.6	1050 (10)	EFF	0.530	40	+H₂O		1989 January 31

Non-detection table from Menten & Melnick (1989)