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IVI94 - Discovery of OH and H2O Masers in R-Aquarii and h1 - 36-ARAE

Short title: Ivison et al. (1994)
Authors: Ivison, R. J. Seaquist, E. R. Hall, P. J.
Journal: Monthly Notices of the Royal Astronomical Society, Vol. 269, NO. 1/JUL1, P. 218, 1994
Bibcode:

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Abstract
We present the first results from an all-sky maser-line survey of symbiotic Miras. Interferometric spectral-line observations of R Aqr and Ht-36 have revealed a 22-0Hz water maser in the former and t612-MHz hydroxyl and weak 22-0Hz water maser emission from the latter. H1-36 has thus become the first known symbiotic OH/IR star. We have also detected weak OH line emission from the vicinity of R Aqr, but we note that there are small discrepancies between the OH- and H2 0-line velocities and positions. These demonstrate unequivocally that dust can shield some circumstellar hydroxyl and water molecules from dissociation, even in systems that possess intense local sources of uV. Finally, we discuss some of the implications of these observations. The narrow profile of the water maser in R Aqr means that there may finally be an opportunity to determine the system's orbital parameters. We also point out that high-resolution synthesis observations may trace the distribution of dust in Hl-36 and R Aqr, possibly throwing light on the mass-loss process in symbiotic Miras and placing constraints on the amount of collimation experienced by Uv radiation from their hot, compact companions. Key words: masers - binaries: symbiotic - stars: individual: R Aqr - stars: individual: Hi-36 Arae - dust, extinction - radio lines: stars. eprintid: arXiv:astro-ph/9402055	Comments: Velocity resolution: 0.7 km/s

Abstract

We present the first results from an all-sky maser-line survey of symbiotic Miras. Interferometric spectral-line observations of R Aqr and Ht-36 have revealed a 22-0Hz water maser in the former and t612-MHz hydroxyl and weak 22-0Hz water maser emission from the latter. H1-36 has thus become the first known symbiotic OH/IR star. We have also detected weak OH line emission from the vicinity of R Aqr, but we note that there are small discrepancies between the OH- and H2 0-line velocities and positions. These demonstrate unequivocally that dust can shield some circumstellar hydroxyl and water molecules from dissociation, even in systems that possess intense local sources of uV. Finally, we discuss some of the implications of these observations. The narrow profile of the water maser in R Aqr means that there may finally be an opportunity to determine the system's orbital parameters. We also point out that high-resolution synthesis observations may trace the distribution of dust in Hl-36 and R Aqr, possibly throwing light on the mass-loss process in symbiotic Miras and placing constraints on the amount of collimation experienced by Uv radiation from their hot, compact companions. Key words: masers - binaries: symbiotic - stars: individual: R Aqr - stars: individual: Hi-36 Arae - dust, extinction - radio lines: stars. eprintid: arXiv:astro-ph/9402055

Comments:
Velocity resolution: 0.7 km/s

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Detection table from Ivison et al. (1994)

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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	23 43 49.4	-15 17 0.9	66.5188	-70.3248	G66.517-70.325	R Aqr	1612	14.0	-14.0	0.060	ENG15	-H₂O +OH +SiO	EVOLVED		IVI94
2	17 49 48.2	-37 01 27.7	353.5135	-4.9209	G353.513-4.921	H1-36	1612	132.5	-132.5	0.270	ENG15	+OH +SiO	SFR_MIXED		IVI94

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 IVI94

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