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GOM90 - H2O and SiO maser emission in OH/IR stars.

Short title: Gomez et al. (1990)
Authors: Gómez, Y. Moran, J. M. Rodríguez, L. F.
Journal: Revista Mexicana de Astronomia y Astrofisica, Vol. 20, No. 1, p. 55 - 66
Bibcode:

Target type: IRAS

Abstract
The authors searched for H₂O and SiO maser emission in 84 OH/IR stars that have measured IRAS fluxes at 12, 25, and 60 mum. They detected four new H₂O sources and eight new SiO sources. The authors have used previous detections reported in the literature to determine the percentage of OH/IR stars with H₂O and SiO maser emission as a function of [25-12] color. The percentage of objects with detectable H₂O and SiO maser emission decreases with increasing [25-12] color. This color is believed to be an age indicator. The statistical analysis of the data suggests that the percentage of OH/IR stars with SiO maser emission decrease as the [25-12] color increases. Current models for the time evolution of OH/IR stars suggest that it is around [25-12] &cong +0.2 that the mass loss ceases or decreases significantly. The percentage of OH/IR stars with H₂O maser emission decreases significantly at [25-12] &cong -0.2, before mass loss ceases. The reasons for the early drop in H₂O maser percentage are not known.

Abstract

The authors searched for H₂O and SiO maser emission in 84 OH/IR stars that have measured IRAS fluxes at 12, 25, and 60 mum. They detected four new H₂O sources and eight new SiO sources. The authors have used previous detections reported in the literature to determine the percentage of OH/IR stars with H₂O and SiO maser emission as a function of [25-12] color. The percentage of objects with detectable H₂O and SiO maser emission decreases with increasing [25-12] color. This color is believed to be an age indicator. The statistical analysis of the data suggests that the percentage of OH/IR stars with SiO maser emission decrease as the [25-12] color increases. Current models for the time evolution of OH/IR stars suggest that it is around [25-12] &cong +0.2 that the mass loss ceases or decreases significantly. The percentage of OH/IR stars with H₂O maser emission decreases significantly at [25-12] &cong -0.2, before mass loss ceases. The reasons for the early drop in H₂O maser percentage are not known.

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Detection table from Gomez et al. (1990)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_range	V_peak	F_peak	Telescope	RMS	List	Beam	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			H₂O	(km/s)	(km/s)	(Jy)		(Jy)		(arcsec)	Yes/No		(kpc)
1	18 21 06	-15 03 24.1	16.1148	-0.2875	G16.117-0.291	OH 16.1-0.3	22 GHz;		37.7	6.3	HAYS	2.000	ENG_H2O	90	+H₂O -CH₃OH I +CH₃OH II +OH +SiO	SFR_MIXED		GOM90
2	18 35 29.9	-07 13 10.3	24.6940	0.2324	G24.693+0.235	OH 24.7+0.2	22 GHz;	26.3;30.7	26.3	8.2	HAYS	2.000	ENG_H2O	90	+H₂O -CH₃OH II +OH +SiO	SFR_MIXED		GOM90
3	18 51 15.4	+01 56 17.9	34.6365	0.9240	G34.638+0.922	OH 34.7+0.9	22 GHz;		39.6	2.2	HAYS	2.000	ENG_H2O	90	+H₂O +OH +SiO	EVOLVED		GOM90
4	19 02 6.3	+03 20 15	37.1182	-0.8474	G37.118-0.847	OH 37.1-0.9	22 GHz;		67.9	3.7	HAYS	2.000	ENG_H2O	90	+H₂O -CH₃OH I -CH₃OH II +OH +SiO	EVOLVED		GOM90

Non-detection table from Gomez et al. (1990)