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SZY95A - A survey of main-line OH maser emission from semiregular variables.

Short title: Szymczak et al. (1995A)
Authors: Szymczak, M. Le Squeren, A. M. Sivagnanam, P. Tran Minh, F. Fournier, A.
Journal: Astronomy and Astrophysics, v.297, p.494
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Abstract
We have made a high sensitivity (~0.15Jy) search in the OH main-lines for maser emission from a sample of 181 semiregular variables. OH emission was observed towards five stars. Two new OH lines were detected and one tentatively. About 10% of semiregulars with distances less than 300pc have associated OH maser emission. The OH semiregulars show much redder near and far infrared colors than similar non-OH stars. On the average, their mass loss rates and OH luminosities are slightly lower than in the long period Mira variables. Basing on the optical and infrared properties of the semiregulars and long period variables we confirmed that properties of the SRa stars are intermediate between those of SRb and Mira variables. The occurrence of strongly polarized, low luminosity OH main-line maser only, together with relatively low efficiency of pumping by the infrared photons, provides evidence that the semiregulars are less evolved than the Mira-type variables. This can support the existence of an evolutionary sequence of SRb-SRa-Mira variables. However, the expansion velocities of some OH semiregulars are higher than those observed in most type I OH Miras and their pulsational properties may suggest that they are in a peculiar evolutionary phase.	Comments: Velocity resolution: 0.56 km/s Upper limit for non-detections: 0.15 Jy (3σ)

Abstract

We have made a high sensitivity (~0.15Jy) search in the OH main-lines for maser emission from a sample of 181 semiregular variables. OH emission was observed towards five stars. Two new OH lines were detected and one tentatively. About 10% of semiregulars with distances less than 300pc have associated OH maser emission. The OH semiregulars show much redder near and far infrared colors than similar non-OH stars. On the average, their mass loss rates and OH luminosities are slightly lower than in the long period Mira variables. Basing on the optical and infrared properties of the semiregulars and long period variables we confirmed that properties of the SRa stars are intermediate between those of SRb and Mira variables. The occurrence of strongly polarized, low luminosity OH main-line maser only, together with relatively low efficiency of pumping by the infrared photons, provides evidence that the semiregulars are less evolved than the Mira-type variables. This can support the existence of an evolutionary sequence of SRb-SRa-Mira variables. However, the expansion velocities of some OH semiregulars are higher than those observed in most type I OH Miras and their pulsational properties may suggest that they are in a peculiar evolutionary phase.

Comments:
Velocity resolution: 0.56 km/s
Upper limit for non-detections: 0.15 Jy (3σ)

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Detection table from Szymczak et al. (1995A)

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ID	Obs. RA	Obs. Dec	l	b	Group id	grpv	Source name	Line	Frequency	V_range	V_peak	F_peak	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)				OH	(MHz)	(km/s)	(km/s)	(Jy)		Yes/No		(kpc)
1	07 55 40.4	-28 38 56	245.4382	-0.1470	G245.438-0.147	G245.4380-0.1473	IRAS 07536-2830	1665 MHz;	1665	34.3	34.3	0.300	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95A
2	07 55 40.4	-28 38 56	245.4382	-0.1470	G245.438-0.147	G245.4380-0.1473	IRAS 07536-2830	1667 MHz;	1667	34.3	34.3	0.700	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95A
3	11 00 33.5	-18 19 27	269.2676	37.1957	G269.270+37.196	G269.2695+37.1958	IRAS 10580-1803	1665 MHz;	1665	1.7	1.7	2.500	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95A
4	11 00 33.5	-18 19 27	269.2676	37.1957	G269.270+37.196	G269.2695+37.1958	IRAS 10580-1803	1667 MHz;	1667	18.0	1.7	4.500	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95A
5	13 02 38.1	+05 11 08	310.3584	67.8957	G310.357+67.896	G310.3572+67.8959	IRAS 13001+0527	1665 MHz;	1665	12.4	11.2	0.300	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95A
6	13 02 38.1	+05 11 08	310.3584	67.8957	G310.357+67.896	G310.3572+67.8959	IRAS 13001+0527	1667 MHz;	1667	13.2	10.8	3.300	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95A
7	13 49 2.4	-28 22 05	318.0239	32.8100	G318.022+32.811	G318.0224+32.8109	IRAS 13462-2807	1665 MHz;	1665	2.7	33.6	4.900	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95A
8	13 49 2.4	-28 22 05	318.0239	32.8100	G318.022+32.811	G318.0224+32.8109	IRAS 13462-2807	1667 MHz;	1667	7.3	36.1	32.000	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95A
9	14 24 11.2	+25 42 15	34.2779	69.2144	G34.278+69.213	G34.2778+69.2129	IRAS 14219+2555	1665 MHz;	1665	0.2	-0.2	0.400	ENG15	+H₂O -CH₃OH I +OH +SiO	EVOLVED		SZY95A
10	22 05 41.6	+35 20 52	88.7134	-16.2851	G88.715-16.285	G88.7152-16.2854	IRAS 22035+3506	1667 MHz;	1667	1.4	1.4	0.130	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95A

Non-detection table from Szymczak et al. (1995A)