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UKI84 - Stellar OH masers with polarized features at intermediate velocities

Short title: Ukita & Le Squeren (1984)
Authors: Ukita, N. Le Squeren, A. M.
Journal: Astronomy and Astrophysics (ISSN 0004-6361), vol. 138, no. 2, Sept. 1984, p. 343-352.
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Abstract
Peculiar profiles were discovered in EY And, one of five new sources found in an OH maser search. The 1612-MHz emission has a typical, double-peak structure, but the main-line masers show polarized features at the central velocity of the 1612-MHz emission. The line shape of the SiO maser resembles that of the 1665-MHz emission. Maser sources with polarized OH emission at intermediate velocities are discussed in the context of two kinematic models. Expanding envelopes with a smooth velocity field would require some of the polarized OH features to arise in the innermost part of the envelopes. Distortion of a smooth outflow by interaction with the ambient gas cannot explain the peculiar OH emission. It is interpreted as a fluctuation of the velocity field of the expanding envelope. The polarized features in both main-line spectra have the same sense of circular polarization when they appear at nearly the same velocity. This evidence is consistent with the mechanism proposed by Cook and Shklovskii.	Comments: Velocity resolution: 0.90 km/s Upper limit for non-detections: 0.1-0.3 Jy (3σ)

Abstract

Peculiar profiles were discovered in EY And, one of five new sources found in an OH maser search. The 1612-MHz emission has a typical, double-peak structure, but the main-line masers show polarized features at the central velocity of the 1612-MHz emission. The line shape of the SiO maser resembles that of the 1665-MHz emission. Maser sources with polarized OH emission at intermediate velocities are discussed in the context of two kinematic models. Expanding envelopes with a smooth velocity field would require some of the polarized OH features to arise in the innermost part of the envelopes. Distortion of a smooth outflow by interaction with the ambient gas cannot explain the peculiar OH emission. It is interpreted as a fluctuation of the velocity field of the expanding envelope. The polarized features in both main-line spectra have the same sense of circular polarization when they appear at nearly the same velocity. This evidence is consistent with the mechanism proposed by Cook and Shklovskii.

Comments:
Velocity resolution: 0.90 km/s
Upper limit for non-detections: 0.1-0.3 Jy (3σ)

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Detection table from Ukita & Le Squeren (1984)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Frequency	V_range	V_peak	F_peak	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			(MHz)	(km/s)	(km/s)	(Jy)		Yes/No		(kpc)
1	04 40 30.2	-38 14 10	241.3247	-41.3162	G241.323-41.316	R Cae	1665	3.5	3.5	0.200	ENG15	+H₂O +OH +SiO	EVOLVED		UKI84
	04 40 30.2	-38 14 10	241.3247	-41.3162	G241.323-41.316	R Cae	1667	3.5	3.5	0.170	ENG15	+H₂O +OH +SiO	EVOLVED		UKI84
3	05 46 52.4	+69 58 04	143.4427	20.0990	G143.432+20.091	IRC+70066	1665	13.5	13.5	0.500	ENG15	+H₂O +OH +SiO	EVOLVED		UKI84
	05 46 52.4	+69 58 04	143.4427	20.0990	G143.432+20.091	IRC+70066	1667	34.0	-18.0	0.350	ENG15	+H₂O +OH +SiO	EVOLVED		UKI84
5	15 11 40.8	-06 00 44	353.8234	42.5886	G353.826+42.588	Y Lib	1665	14.0	14.0	0.250	ENG15	+H₂O +OH +SiO	EVOLVED		UKI84
	15 11 40.8	-06 00 44	353.8234	42.5886	G353.826+42.588	Y Lib	1667	14.0	14.0	0.200	ENG15	+H₂O +OH +SiO	EVOLVED		UKI84
7	22 07 19	+11 53 53	71.9270	-34.2593	G71.927-34.259	IRC+10510	1667	11.5	22.5	0.150	ENG15	+OH			UKI84
8	23 45 3.2	+43 55 10	110.4849	-17.3420	G110.484-17.338	EY And	1612	23.0	-54.0	0.550	ENG15	+H₂O +OH +SiO	EVOLVED		UKI84
	23 45 3.2	+43 55 10	110.4849	-17.3420	G110.484-17.338	EY And	1665	42.0	-42.0	0.900	ENG15	+H₂O +OH +SiO	EVOLVED		UKI84
	23 45 3.2	+43 55 10	110.4849	-17.3420	G110.484-17.338	EY And	1667	42.0	-42.0	0.600	ENG15	+H₂O +OH +SiO	EVOLVED		UKI84

Non-detection table from Ukita & Le Squeren (1984)