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LIT94 - A search for SiO, OH, CO and HCN radio emission from silicate-carbon stars

Short title: Little-Marenin et al. (1994)
Authors: Little-Marenin, I. R. Sahai, R. Wannier, P. G. Benson, P. J. Gaylard, M. Omont, A.
Journal: Astronomy and Astrophysics (ISSN 0004-6361), vol. 281, no. 2, p. 451-459
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Abstract
We report upper limits for radio emission of SiO at 86 and 43 GHz, of OH at 1612 and 1665/1667 MHz, of CO at 115 GHz and HCN at 88.6 GHz in the silicate-carbon stars. These upper limits of SiO imply that oxygen-rich material has not been detected within 2R_star of a central star even though the detected emission from silicate dust grains, H2O and OH maser establishes the presence of oxygen-rich material from about tens to thousands of AU of a central star. The upper limit of the SiO abundance is consistent with that found in oxygen-rich envelopes. Upper limits of the mass loss rate (based on the CO data) are estimated to be between 10^-6 to 10^-7 solar mass/yr assuming a distance of 1.5 kpc for these stars. The absence of HCN microwave emission implies that no carbon-rich material can be detected at large distances (thousands of AU) from a central star. The lack of detections of SiO, CO, and HCN emission is most likely due to the large distances of these stars. A number of C stars were detected in CO and HCN, but only the M supergiant VX Sgr was detected in CO.	Comments: Velocity resolution: 0.90 km/s Upper limit for non-detections: mostly <0.75 Jy (3σ)

Abstract

We report upper limits for radio emission of SiO at 86 and 43 GHz, of OH at 1612 and 1665/1667 MHz, of CO at 115 GHz and HCN at 88.6 GHz in the silicate-carbon stars. These upper limits of SiO imply that oxygen-rich material has not been detected within 2R_star of a central star even though the detected emission from silicate dust grains, H2O and OH maser establishes the presence of oxygen-rich material from about tens to thousands of AU of a central star. The upper limit of the SiO abundance is consistent with that found in oxygen-rich envelopes. Upper limits of the mass loss rate (based on the CO data) are estimated to be between 10^-6 to 10^-7 solar mass/yr assuming a distance of 1.5 kpc for these stars. The absence of HCN microwave emission implies that no carbon-rich material can be detected at large distances (thousands of AU) from a central star. The lack of detections of SiO, CO, and HCN emission is most likely due to the large distances of these stars. A number of C stars were detected in CO and HCN, but only the M supergiant VX Sgr was detected in CO.

Comments:
Velocity resolution: 0.90 km/s
Upper limit for non-detections: mostly <0.75 Jy (3σ)

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Detection table from Little-Marenin et al. (1994)

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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	20 36 6.6	+60 05 17	95.7549	11.5090	G95.758+11.509	G95.7580+11.5090	V778 Cyg	1667 MHz;	1667	17.0	-17.0	0.200	ENG15	+H₂O +OH -SiO	EVOLVED		LIT94

Non-detection table from Little-Marenin et al. (1994)