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DIC86 - OH masers in short-period Mira and semiregular variable stars

Short title: Dickinson et al. (1986)
Authors: Dickinson, D. F. Turner, B. E. Jewell, P. R. Benson, P. J.
Journal: Astronomical Journal (ISSN 0004-6256), vol. 92, Sept. 1986, p. 627-632.
Bibcode:

Abstract
The authors have made a systematic search in all four OH lines for maser emission from the short-period Mira variables and the known short-period semiregular maser stars. R Ceti was detected in the main lines, the first short-period (166 days) Mira ever found in OH. None of the short-period Miras searched showed water emission. The authors also present spectra of three SiO detections made in a very limited sample of the short-period Mira variables. Six new OH lines were detected in the semiregular variables all are Type I stars devoid of any satellite line emission. Both classes of star are weak OH emitters and there is a relative lack of circumstellar material as evidenced by the modest infrared excess shown in the 2.2 - 11 mu color index. These facts are probably related and lend support to the idea that far-infrared radiation is the primary OH maser pump in these stars.	Comments: Spectral type was set to: ""S"", where only one peak was found. ""D"", where two peaks were found. Velocity resolution: 1.07 km/s Upper limit for non-detections: 0.15 Jy (3σ)

Abstract

The authors have made a systematic search in all four OH lines for maser emission from the short-period Mira variables and the known short-period semiregular maser stars. R Ceti was detected in the main lines, the first short-period (166 days) Mira ever found in OH. None of the short-period Miras searched showed water emission. The authors also present spectra of three SiO detections made in a very limited sample of the short-period Mira variables. Six new OH lines were detected in the semiregular variables all are Type I stars devoid of any satellite line emission. Both classes of star are weak OH emitters and there is a relative lack of circumstellar material as evidenced by the modest infrared excess shown in the 2.2 - 11 mu color index. These facts are probably related and lend support to the idea that far-infrared radiation is the primary OH maser pump in these stars.

Comments:
Spectral type was set to:
""S"", where only one peak was found.
""D"", where two peaks were found.

Velocity resolution: 1.07 km/s
Upper limit for non-detections: 0.15 Jy (3σ)

Input tables: Table I and II
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Detection table from Dickinson et al. (1986)

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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	07 13 31.8	-44 38 39	255.7684	-15.0390	G255.768-15.039	L2 Pup	1665	33.0	33.0	14.000	ENG15	+OH	EVOLVED		DIC86
	07 13 31.8	-44 38 39	255.7684	-15.0390	G255.768-15.039	L2 Pup	1667	34.0	34.0	3.100	ENG15	+OH	EVOLVED		DIC86
3	11 00 33.9	-18 19 29	269.2696	37.1960	G269.270+37.196	R Crt	1665	14.2	2.5	2.500	ENG15	+H₂O +OH +SiO	EVOLVED		DIC86
	11 00 33.9	-18 19 29	269.2696	37.1960	G269.270+37.196	R Crt	1667	15.6	1.5	7.600	ENG15	+H₂O +OH +SiO	EVOLVED		DIC86
5	13 02 37.7	+05 11 09	310.3541	67.8962	G310.357+67.896	RT Vir	1665	23.3	23.3	1.700	ENG15	+H₂O +OH +SiO	EVOLVED		DIC86
	13 02 37.7	+05 11 09	310.3541	67.8962	G310.357+67.896	RT Vir	1667	13.0	11.0	2.300	ENG15	+H₂O +OH +SiO	EVOLVED		DIC86
7	13 19 27.9	+45 31 38	107.8903	70.7737	G107.891+70.774	V CVn	1665	5.2	1.3	0.160	ENG15	+H₂O +OH -SiO	EVOLVED		DIC86
	13 19 27.9	+45 31 38	107.8903	70.7737	G107.891+70.774	V CVn	1667	4.0	4.0	0.120	ENG15	+H₂O +OH -SiO	EVOLVED		DIC86
9	19 50 6.7	-07 37 04	32.7208	-16.4886	G32.723-16.486	GY Aql	1665	7.2	33.6	33.000	ENG15	-H₂O -CH₃OH II +OH +SiO	EVOLVED		DIC86
	19 50 6.7	-07 37 04	32.7208	-16.4886	G32.723-16.486	GY Aql	1667	7.6	33.5	11.000	ENG15	-H₂O -CH₃OH II +OH +SiO	EVOLVED		DIC86

Non-detection table from Dickinson et al. (1986)