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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:

Non-detection table: Show non-detection table
Detection table: Show detection table (8 detection)
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	V_range	V_peak	F_peak	RMS	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			(km/s)	(km/s)	(Jy)	(Jy)		Yes/No		(kpc)
1	18 09 25	+34 46 17.3	61.4728	23.1625	G61.473+23.164	*IRAS 18076+3445	0.00	4.2	9	9.000	ENG_SIO	+H₂O +OH +SiO	EVOLVED		GOM90
2	18 20 36.7	-18 47 9.4	12.7689	-1.9401	G12.769-1.941	OH 12.8-1.9	0.00	10.9	39.7	9.000	ENG_SIO	+H₂O +OH +SiO	EVOLVED		GOM90
3	18 21 06	-15 03 24.1	16.1148	-0.2875	G16.117-0.291	OH 16.1-0.3	0.00	22	51	9.000	ENG_SIO	+H₂O -CH₃OH I +CH₃OH II +OH +SiO	SFR_MIXED		GOM90
4	18 35 29.9	-07 13 10.3	24.6940	0.2324	G24.693+0.235	*OH 24.7 +0.3	0.00	47.5	10.7	9.000	ENG_SIO	+H₂O -CH₃OH II +OH +SiO	SFR_MIXED		GOM90
5	18 45 52.7	-01 46 43.3	30.7150	0.4255	G30.715+0.427	OH 30.7 +0.4	0.00	68.9	14.8	9.000	ENG_SIO	+H₂O -CH₃OH II +OH +SiO	SFR_MIXED		GOM90
6	19 21 36.4	+09 27 51.4	44.7933	-2.3066	G44.795-2.307	OH 44.8-2.3	0.00	-71.6	14.2	9.000	ENG_SIO	+H₂O +OH +SiO	EVOLVED		GOM90
7	19 30 50.2	+29 29 56.8	63.4817	5.2799	G63.482+5.280	*IRAS 19288+2923	0.00	-37.8	6.1	9.000	ENG_SIO	+H₂O +OH +SiO	EVOLVED		GOM90
8	19 40 54.1	+15 20 8.5	52.2137	-3.6244	G52.218-3.627	IRAS 19386+1513	0.00	1.7	7.3	9.000	ENG_SIO	+H₂O -CH₃OH II +OH +SiO	EVOLVED		GOM90

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 GOM90

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