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CHO10 - Simultaneous Observations of SiO and H2O Masers Toward Symbiotic Stars

Short title: Cho & Kim (2010)
Authors: Cho, Se-Hyung Kim, Jaeheon
Journal: The Astrophysical Journal, Volume 719, Issue 1, pp. 126-130 (2010).
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (10 detection)
Target type: star

Abstract
We present the results of simultaneous observations of SiO v = 1, 2, J = 1-0, ²⁹SiO v = 0, J = 1-0, and H₂O 6₁₆-5₂₃ maser lines performed with the KVN Yonsei 21 m radio telescope from 2009 November to 2010 January. We searched for these masers in 47 symbiotic stars and detected maser emission from 21 stars, giving the first time detection from 19 stars. Both SiO and H₂O masers were detected from seven stars of which six were D-type symbiotic stars and one was an S-type star, WRAY 15-1470. In the SiO maser emission, the ²⁸SiO v = 1 maser was detected from 10 stars, while the v = 2 maser was detected from 15 stars. In particular, the ²⁸SiO v = 2 maser emission without the v = 1 maser detection was detected from nine stars with a detection rate of 60%, which is much higher than that of isolated Miras/red giants. The ²⁹SiO v = 0 maser emission was also detected from two stars, H 2-38 and BF Cyg, together with the ²⁸SiO v = 2 maser. We conclude that these different observational results between isolated Miras/red giants and symbiotic stars may be related with the presence of hot companions in a symbiotic binary system.

Abstract

We present the results of simultaneous observations of SiO v = 1, 2, J = 1-0, ²⁹SiO v = 0, J = 1-0, and H₂O 6₁₆-5₂₃ maser lines performed with the KVN Yonsei 21 m radio telescope from 2009 November to 2010 January. We searched for these masers in 47 symbiotic stars and detected maser emission from 21 stars, giving the first time detection from 19 stars. Both SiO and H₂O masers were detected from seven stars of which six were D-type symbiotic stars and one was an S-type star, WRAY 15-1470. In the SiO maser emission, the ²⁸SiO v = 1 maser was detected from 10 stars, while the v = 2 maser was detected from 15 stars. In particular, the ²⁸SiO v = 2 maser emission without the v = 1 maser detection was detected from nine stars with a detection rate of 60%, which is much higher than that of isolated Miras/red giants. The ²⁹SiO v = 0 maser emission was also detected from two stars, H 2-38 and BF Cyg, together with the ²⁸SiO v = 2 maser. We conclude that these different observational results between isolated Miras/red giants and symbiotic stars may be related with the presence of hot companions in a symbiotic binary system.

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Detection table from Cho & Kim (2010)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	V_range	V_peak	F_peak	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			(km/s)	(km/s)	(Jy)		Yes/No		(kpc)
1	02 05 32	-00 42 1.7	159.9399	-58.1454	G159.940-58.145	AS 221	0.00	-24	1.617	ENG_SIO	+SiO	GALAXY		CHO10
2	05 21 48.9	+32 30 43.2	174.2175	-2.3490	G174.217-2.349	UV Aur	0.00	-4.4	1.733	ENG_SIO	-H₂O +SiO	EVOLVED		CHO10
3	16 23 21.6	-27 40 13	350.0605	15.2372	G350.060+15.237	WRAY 15-1470	0.00	40.2	1.617	ENG_SIO	+SiO	EVOLVED		CHO10
4	16 34 4.3	-35 05 26.8	346.0266	8.5504	G346.027+8.550	Hen 2-171	0.00	-127.8	1.733	ENG_SIO	-OH +SiO	EVOLVED		CHO10
5	17 49 48.2	-37 01 27.9	353.5135	-4.9209	G353.513-4.921	H 1-36	0.00	-115.9	3.349	ENG_SIO	+OH +SiO	SFR_MIXED		CHO10
6	19 23 34.7	+00 37 58.4	37.1810	-6.8549	G37.181-6.855	V850 Aql	0.00	29.4	1.386	ENG_SIO	+SiO	EVOLVED		CHO10
7	19 57 05	+39 49 36.3	75.1727	5.6777	G75.173+5.678	V1016 Cyg	0.00	-46.1	1.733	ENG_SIO	-OH +SiO	EVOLVED		CHO10
8	21 02 9.8	+45 46 33	86.9826	-0.4820	G86.983-0.482	*V407 Cyg	0.00	-28.1	5.428	ENG_SIO	-OH +SiO	EVOLVED		CHO10
9	22 57 41	+58 49 12.5	108.6567	-0.8625	G108.657-0.862	V627 Cas	0.00	-55.3	49.549	ENG_SIO	+H₂O +OH +SiO	EVOLVED		CHO10
10	23 43 49.5	-15 17 4.2	66.5168	-70.3255	G66.517-70.325	*R Aqr	0.00	-22.5	64.911	ENG_SIO	-H₂O +OH +SiO	EVOLVED		CHO10

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

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Distribution of sources in IRAS color-color diagram

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Original color diagram is taken form van der Veen & Habing (1987)

Type	Description
I	Oxygen-rich non-variable stars without circumstellar shells
II	Variable stars with "young" O-rich circumstellar shells
IIIa	Variable stars with more evolved O-rich circumstellar shells
IIIb	Variable stars with thick O-rich circumstellar shells
IV	Variable stars with very thick O-rich circumstellar shells
V	Planetary nebulae and non- variable stars with very cool circumstellar shells
VIa	Variable stars with relatively cold dust at large distances; a significant part of the stars is carbon-rich
VIb	Variable stars with relatively hot dust close to the star and relatively cold dust at large distances; Some of the objects have proven to be O-rich
VII	Variable stars with more evolved C-rich circumstellar shells
VIII	Different sort of objects

Distribution of the detection velocities versus galactic longitude from CHO10

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