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GOM94 - Anomalous water masers in OH/IR stars.

Short title: Gómez et al. (1994)
Authors: Gómez, Y. Rodríguez, L. F. Contreras, M. E. Moran, J. M.
Journal: Revista Mexicana de Astronomia y Astrofisica, Vol. 28, No. 1, p. 97 - 102
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (4 detection) Non-detection table: Show non-detection table (1 non-detection)
Target type: star

Abstract
The authors present OH (1612 MHz) and H₂O (22.2 GHz) maser observations made with the VLA at an angular resolution of &equiv1""toward three OH/IR stars: OH 12.8-0.9, OH 37.1-0.8 and OH 42.3-0.1. These stars exhibit the H₂O maser components in a velocity range that exceeds the OH velocity range, a situation in disagreement with the standard model for maser emission in late-type stars. The authors find that the OH and H₂O maser positions agree within &equiv0""5 and that most likely both masers arise from the same source, ruling out the possibility of a fortuitous superposition of two different sources. The authors discuss some of the possible mechanisms that could explain the anomalous H₂O maser emission. The most likely explanation is that these stars have axisymmetric winds and that the H₂O emission originates in the polar regions with larger velocities than the regions closer to the equator where the OH emission arises. Very long baseline observations are required to test this explanation.

Abstract

The authors present OH (1612 MHz) and H₂O (22.2 GHz) maser observations made with the VLA at an angular resolution of &equiv1""toward three OH/IR stars: OH 12.8-0.9, OH 37.1-0.8 and OH 42.3-0.1. These stars exhibit the H₂O maser components in a velocity range that exceeds the OH velocity range, a situation in disagreement with the standard model for maser emission in late-type stars. The authors find that the OH and H₂O maser positions agree within &equiv0""5 and that most likely both masers arise from the same source, ruling out the possibility of a fortuitous superposition of two different sources. The authors discuss some of the possible mechanisms that could explain the anomalous H₂O maser emission. The most likely explanation is that these stars have axisymmetric winds and that the H₂O emission originates in the polar regions with larger velocities than the regions closer to the equator where the OH emission arises. Very long baseline observations are required to test this explanation.

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Detection table from Gómez et al. (1994)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	F_peak	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			H₂O	(km/s)	(Jy)		Yes/No		(kpc)
1	19 02 6.2	+03 20 15.5	37.1182	-0.8471	G37.118-0.847	OH 37.1-0.8	22 GHz;	64.4	1.7	ENG_H2O	+H₂O -CH₃OH I -CH₃OH II +OH +SiO	EVOLVED		GOM94
	19 02 6.2	+03 20 15.5	37.1182	-0.8471	G37.118-0.847	OH 37.1-0.8	22 GHz;	66.8	5	ENG_H2O	+H₂O -CH₃OH I -CH₃OH II +OH +SiO	EVOLVED		GOM94
3	19 09 8.2	+08 16 33.9	42.3084	-0.1324	G42.308-0.132	OH 42.3-0.1	22 GHz;	78.0	9	ENG_H2O	+H₂O +OH +SiO	EVOLVED		GOM94
4	18 16 49.1	-18 15 2.1	12.8156	-0.8946	G12.816-0.895	OH 12.8-0.9	22 GHz;	-78.6	0.8	ENG_H2O	+H₂O +OH	EVOLVED		GOM94

Non-detection table from Gómez et al. (1994)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	F_peak	Date	RMS	List	Detection	Class	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			H₂O	(Jy)		(Jy)		Yes/No
1	19 09 8.2	+08 16 33.9	42.3084	-0.1324	G42.308-0.132	OH 42.3-0.1	22 GHz;	0.12	1992-05-20	0.040	ENG_H2O	+H₂O +OH +SiO	EVOLVED	GOM94

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

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Distribution of sources in IRAS color-color diagram

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Original color diagram is taken form van der Veen & Habing (1987)

Type	Description
I	Oxygen-rich non-variable stars without circumstellar shells
II	Variable stars with "young" O-rich circumstellar shells
IIIa	Variable stars with more evolved O-rich circumstellar shells
IIIb	Variable stars with thick O-rich circumstellar shells
IV	Variable stars with very thick O-rich circumstellar shells
V	Planetary nebulae and non- variable stars with very cool circumstellar shells
VIa	Variable stars with relatively cold dust at large distances; a significant part of the stars is carbon-rich
VIb	Variable stars with relatively hot dust close to the star and relatively cold dust at large distances; Some of the objects have proven to be O-rich
VII	Variable stars with more evolved C-rich circumstellar shells
VIII	Different sort of objects

Distribution of the detection velocities versus galactic longitude from GOM94

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