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SZY99 - A comparison of OH and H_2O maser properties of Mira and semiregular variable stars

Short title: Szymczak & Le Squeren (1999)
Authors: Szymczak, M. Le Squeren, A. M.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 304, Issue 2, pp. 415-420.
Bibcode:

Abstract
A sample of 17 Miras and nine semiregular variable stars was simultaneously observed in the OH and H_2O maser lines with sensitivities of 0.15 and 0.6 Jy, respectively. One new H_2O source was detected. Among Miras the H_2O maser luminosity is well correlated with the OH maser luminosity. The ratio of H_2O to OH maser luminosities decreases by about four orders of magnitude from the semiregulars to the Miras as a result of an increase in the mass-loss rate. Some semiregulars have maser properties typical of Mira stars. H_2O emission is most likely to be detected from Miras at velocities close to the stellar velocity, while emission at blueshifted velocities dominates the detections from semiregulars. OH emission from the semiregulars usually occurs at greater redshifts and blueshifts with respect to the stellar velocities than OH emission observed from the Miras. The differences in the average composite maser profiles in both groups of stars can be related to the velocity gradients in the maser regions. It is suggested that some semiregular variables with maser emission may be in a later stage of stellar evolution than the Miras.	Comments: Velocity resolution: 0.28 km/s Upper limit for non-detections: <0.3 Jy (3σ) Data not given in Table 1 was provided by M. Szymzcak.

Abstract

A sample of 17 Miras and nine semiregular variable stars was simultaneously observed in the OH and H_2O maser lines with sensitivities of 0.15 and 0.6 Jy, respectively. One new H_2O source was detected. Among Miras the H_2O maser luminosity is well correlated with the OH maser luminosity. The ratio of H_2O to OH maser luminosities decreases by about four orders of magnitude from the semiregulars to the Miras as a result of an increase in the mass-loss rate. Some semiregulars have maser properties typical of Mira stars. H_2O emission is most likely to be detected from Miras at velocities close to the stellar velocity, while emission at blueshifted velocities dominates the detections from semiregulars. OH emission from the semiregulars usually occurs at greater redshifts and blueshifts with respect to the stellar velocities than OH emission observed from the Miras. The differences in the average composite maser profiles in both groups of stars can be related to the velocity gradients in the maser regions. It is suggested that some semiregular variables with maser emission may be in a later stage of stellar evolution than the Miras.

Comments:
Velocity resolution: 0.28 km/s
Upper limit for non-detections: <0.3 Jy (3σ)

Data not given in Table 1 was provided by M. Szymzcak.

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Detection table from Szymczak & Le Squeren (1999)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Spectra	Frequency	V_range	V_peak	F_peak	List	Detection	Type	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)				(MHz)	(km/s)	(km/s)	(Jy)		Yes/No
1	23 58 24.9	+51 23 19.7	114.5608	-10.6191	G114.561-10.619	R Cas		1667	10.4	21.1	0.700	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	23 58 24.9	+51 23 19.7	114.5608	-10.6191	G114.561-10.619	R Cas		1665	6.7	23.1	0.520	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
3	02 44 45.5	+12 19 03	161.4735	-41.9194	G161.474-41.919	RU Ari		1612	7.9	16.2	0.560	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	02 44 45.5	+12 19 03	161.4735	-41.9194	G161.474-41.919	RU Ari		1667	1.2	23.6	0.610	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	02 44 45.5	+12 19 03	161.4735	-41.9194	G161.474-41.919	RU Ari		1665	6.2	17.5	0.094	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
6	00 03 21.3	+55 40 50	116.1440	-6.5562	G116.144-6.556	Y Cas	Spectra	1667	10.1	-22.2	0.420	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	00 03 21.3	+55 40 50	116.1440	-6.5562	G116.144-6.556	Y Cas		1665	9.5	-21.9	0.480	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
8	00 46 0.1	+69 10 53.4	122.4460	6.3149	G122.446+6.315	V524 Cas		1612	18.3	-34.8	1.280	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	00 46 0.1	+69 10 53.4	122.4460	6.3149	G122.446+6.315	V524 Cas		1667	24.5	-24.5	0.120	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	00 46 0.1	+69 10 53.4	122.4460	6.3149	G122.446+6.315	V524 Cas		1665	3.6	-28.1	0.080	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
11	10 53 37.4	+13 42 54.3	233.0220	59.4264	G233.022+59.426	W Leo		1667	9.3	41.8	0.210	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	10 53 37.4	+13 42 54.3	233.0220	59.4264	G233.022+59.426	W Leo		1665	1.1	50.6	0.200	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
13	16 25 47.5	+18 53 32.9	35.3451	40.3509	G35.345+40.351	U Her		1612	9.5	-18.5	2.480	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	16 25 47.5	+18 53 32.9	35.3451	40.3509	G35.345+40.351	U Her		1667	9.5	-18.7	5.160	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	16 25 47.5	+18 53 32.9	35.3451	40.3509	G35.345+40.351	U Her		1665	0.9	-18.8	4.150	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
16	05 55 49.2	+20 10 30.7	188.7151	-2.4921	G188.715-2.492	U Ori		1667	0.4	-41.5	1.630	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	05 55 49.2	+20 10 30.7	188.7151	-2.4921	G188.715-2.492	U Ori		1665	1.2	-41.6	2.210	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
18	04 28 18	+10 09 44.8	185.2174	-25.5813	G185.217-25.581	R Tau		1667	14.4	14.4	0.260	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	04 28 18	+10 09 44.8	185.2174	-25.5813	G185.217-25.581	R Tau		1665	14.7	14.7	0.180	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
20	15 21 39.5	+14 18 53.1	20.4982	52.7865	G20.498+52.787	S Ser		1667	25.2	25.2	0.310	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	15 21 39.5	+14 18 53.1	20.4982	52.7865	G20.498+52.787	S Ser		1665	6.2	19.3	0.140	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
22	06 37 31.3	-01 23 43.6	212.5880	-3.7325	G212.588-3.732	SY Mon		1667	6.2	-58.4	0.180	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	06 37 31.3	-01 23 43.6	212.5880	-3.7325	G212.588-3.732	SY Mon		1665	3.1	-55.3	0.190	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
24	22 12 16.2	+14 33 12.2	75.1858	-33.1833	G75.186-33.183	RS Peg		1667	20.3	-20.3	0.240	ENG15	+OH	EVOLVED	SZY99
	22 12 16.2	+14 33 12.2	75.1858	-33.1833	G75.186-33.183	RS Peg		1665	20.0	-20.0	0.480	ENG15	+OH	EVOLVED	SZY99
26	14 27 16.4	+04 40 41.1	352.6741	57.9715	G352.674+57.971	RS Vir		1612	8.2	-18.4	1.950	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	14 27 16.4	+04 40 41.1	352.6741	57.9715	G352.674+57.971	RS Vir		1667	7.1	-17.4	0.660	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	14 27 16.4	+04 40 41.1	352.6741	57.9715	G352.674+57.971	RS Vir		1665	17.9	-17.9	0.910	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
29	09 47 33.5	+11 25 43.6	223.7207	44.1598	G223.721+44.160	R Leo		1665	5.6	-1.5	0.090	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
30	09 45 34.3	+34 30 42.8	190.5954	49.7711	G190.595+49.771	R LMi		1612	3.9	-3.9	0.320	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	09 45 34.3	+34 30 42.8	190.5954	49.7711	G190.595+49.771	R LMi		1667	8.5	-3.4	0.360	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	09 45 34.3	+34 30 42.8	190.5954	49.7711	G190.595+49.771	R LMi		1665	9.3	-4.1	0.970	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
33	13 19 27.8	+45 31 37.7	107.8913	70.7739	G107.891+70.774	V CVn		1667	6.7	6.7	0.190	ENG15	+H₂O +OH -SiO	EVOLVED	SZY99
34	13 02 38	+05 11 8.4	310.3571	67.8959	G310.357+67.896	RT Vir		1665	10.0	13.6	0.630	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	13 02 38	+05 11 8.4	310.3571	67.8959	G310.357+67.896	RT Vir		1667	13.5	10.7	3.840	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
36	07 55 40.2	-28 38 54.8	245.4375	-0.1475	G245.438-0.147	HU Pup		1665	0.8	34.6	0.300	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	07 55 40.2	-28 38 54.8	245.4375	-0.1475	G245.438-0.147	HU Pup		1667	1.1	33.2	0.520	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
38	11 00 33.9	-18 19 29.6	269.2695	37.1958	G269.270+37.196	R Crt		1665	1.0	1.7	1.080	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99
	11 00 33.9	-18 19 29.6	269.2695	37.1958	G269.270+37.196	R Crt		1667	1.1	1.7	3.240	ENG15	+H₂O +OH +SiO	EVOLVED	SZY99

Non-detection table from Szymczak & Le Squeren (1999)