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SIV88 - Criteria for OH maser emission from circumstellar envelopes of oxygen-rich Mira-type red giants

Short title: Sivagnanam et al. (1988)
Authors: Sivagnanam, P. Le Squeren, A. M. Foy, F.
Journal: Astronomy and Astrophysics (ISSN 0004-6361), vol. 206, no. 2, Nov. 1988, p. 285-297.
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Abstract
A large and representative sample of oxygen-rich Mira stars was selected and observed in the 18 cm OH lines at their optical maximum. A total of 14 new OH sources were detected. The OH maser emission is found in the intrinsically bright far-IR objects with late M spectral type. Other characteristics of the Miras are high (H-K) and (K-L) colors. Their periods are on average longer and their (25-12) colors on average redder than those of non-OH Miras. The (J-H) and (60-25) colors are the same for OH and non-OH stars. In most cases, OH and H2O masers exist simultaneously. The observed stars form a sequence along which the period and the stellar luminosity increase, the stellar radius increases, the dust shell radius increases by a smaller factor, the photospheric temperature decreases but the dust shell temperature is roughly constant, and the mass loss rate and thus the thickness and the brighntess of the envelope increase considerably.	Comments: Velocity resolution: 1.00 km/s Upper limit for non-detections: 0.10 Jy (3σ) Velocities and fluxes were determined from the spectra in Fig.1

Abstract

A large and representative sample of oxygen-rich Mira stars was selected and observed in the 18 cm OH lines at their optical maximum. A total of 14 new OH sources were detected. The OH maser emission is found in the intrinsically bright far-IR objects with late M spectral type. Other characteristics of the Miras are high (H-K) and (K-L) colors. Their periods are on average longer and their (25-12) colors on average redder than those of non-OH Miras. The (J-H) and (60-25) colors are the same for OH and non-OH stars. In most cases, OH and H2O masers exist simultaneously. The observed stars form a sequence along which the period and the stellar luminosity increase, the stellar radius increases, the dust shell radius increases by a smaller factor, the photospheric temperature decreases but the dust shell temperature is roughly constant, and the mass loss rate and thus the thickness and the brighntess of the envelope increase considerably.

Comments:
Velocity resolution: 1.00 km/s
Upper limit for non-detections: 0.10 Jy (3σ)
Velocities and fluxes were determined from the spectra in Fig.1

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Detection table from Sivagnanam et al. (1988)

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ID	Obs. RA	Obs. Dec	l	b	Group id	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	03 11 2.9	+14 47 58	166.1419	-36.1012	G166.142-36.100	U Ari	1665 MHz;	1665	56.5	-56.5	0.460	ENG15	-H₂O +OH +SiO	EVOLVED		SIV88
2	05 42 09	+32 02 24.1	176.9647	0.9902	G176.965+0.990	U Aur	1665 MHz;	1665	9.0	2.0	0.290	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
3	05 42 09	+32 02 24.1	176.9647	0.9902	G176.965+0.990	U Aur	1667 MHz;	1667	10.0	2.0	0.250	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
4	20 32 33.6	-21 41 26	22.9423	-31.4455	G22.942-31.445	RU Cap	1612 MHz;	1612	6.0	3.5	0.330	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
5	20 32 33.6	-21 41 26	22.9423	-31.4455	G22.942-31.445	RU Cap	1665 MHz;	1665	5.5	4.0	0.200	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
6	20 32 33.6	-21 41 26	22.9423	-31.4455	G22.942-31.445	RU Cap	1667 MHz;	1667	6.0	4.0	0.190	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
7	13 51 25.5	-36 56 37.7	316.0572	24.3943	G316.057+24.394	RX Cen	1665 MHz;	1665	7.0	7.0	0.090	ENG15	+OH +SiO	EVOLVED		SIV88
8	13 51 25.5	-36 56 37.7	316.0572	24.3943	G316.057+24.394	RX Cen	1667 MHz;	1667	9.5	-2.0	0.190	ENG15	+OH +SiO	EVOLVED		SIV88
9	05 46 56.3	-31 41 28.4	236.6888	-26.7352	G236.689-26.735	S Col	1665 MHz;	1665	65.0	65.0	0.260	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
10	05 46 56.3	-31 41 28.4	236.6888	-26.7352	G236.689-26.735	S Col	1667 MHz;	1667	65.0	65.0	0.370	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
11	16 10 14.5	+25 04 14.3	41.9780	45.6111	G41.978+45.611	RU Her	1665 MHz;	1665	8.0	-15.5	0.160	ENG15	-H₂O +OH +SiO	EVOLVED		SIV88
12	16 10 14.5	+25 04 14.3	41.9780	45.6111	G41.978+45.611	RU Her	1667 MHz;	1667	6.5	-14.5	0.180	ENG15	-H₂O +OH +SiO	EVOLVED		SIV88
13	06 37 31.3	-01 23 43.6	212.5880	-3.7325	G212.588-3.732	SY Mon	1665 MHz;	1665	55.0	-55.0	0.610	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
14	06 37 31.3	-01 23 43.6	212.5880	-3.7325	G212.588-3.732	SY Mon	1667 MHz;	1667	55.5	-55.5	0.240	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
15	05 29 0.9	-04 41 32.8	207.5960	-20.4550	G207.596-20.455	S Ori	1665 MHz;	1665	2.0	-2.0	0.360	ENG15	-H₂O +OH +SiO	EVOLVED		SIV88
16	22 12 16.2	+14 33 12.2	75.1858	-33.1833	G75.186-33.183	RS Peg	1665 MHz;	1665	9.5	-24.5	0.250	ENG15	+OH	EVOLVED		SIV88
17	22 12 16.2	+14 33 12.2	75.1858	-33.1833	G75.186-33.183	RS Peg	1667 MHz;	1667	18.0	-18.0	0.160	ENG15	+OH	EVOLVED		SIV88
18	17 53 48.8	-34 24 3.2	356.1972	-4.2969	G356.197-4.297	SY Sco	1612 MHz;	1612	13.5	-13.5	0.440	ENG15	+OH	EVOLVED		SIV88
19	17 53 48.8	-34 24 3.2	356.1972	-4.2969	G356.197-4.297	SY Sco	1665 MHz;	1665	12.5	-12.5	0.170	ENG15	+OH	EVOLVED		SIV88
20	17 07 35.8	-31 49 30	353.0245	5.1963	G353.025+5.196	TU Sco	1665 MHz;	1665	17.5	-17.5	0.130	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
21	17 07 35.8	-31 49 30	353.0245	5.1963	G353.025+5.196	TU Sco	1667 MHz;	1667	17.5	-17.5	0.130	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
22	14 17 19.9	+66 47 39.2	110.4345	48.1966	G110.434+48.197	U Umi	1665 MHz;	1665	8.5	-8.5	0.200	ENG15	-H₂O +OH +SiO	EVOLVED		SIV88
23	14 17 19.9	+66 47 39.2	110.4345	48.1966	G110.434+48.197	U Umi	1667 MHz;	1667	10.0	-10.0	0.140	ENG15	-H₂O +OH +SiO	EVOLVED		SIV88
24	08 16 33.8	+11 43 34.5	211.7494	24.1390	G211.749+24.139	R Cnc	1665 MHz;	1665	11.8	11.8	3.910	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88
25	18 38 21.1	+08 50 2.8	39.3497	6.9044	G39.349+6.905	X Oph	1667 MHz;	1667	55.2	-55.2	0.260	ENG15	+H₂O +OH +SiO	EVOLVED		SIV88

Non-detection table from Sivagnanam et al. (1988)