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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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Non-detection table: Show non-detection table
Detection table: Show detection table (1 detection) Non-detection table: Show non-detection table (8 non-detection)

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	Source name	Frequency	V_range	V_peak	F_peak	List	Detection	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			(MHz)	(km/s)	(km/s)	(Jy)		Yes/No
1	20 36 6.6	+60 05 17	95.7549	11.5090	G95.758+11.509	V778 Cyg	1667	17.0	-17.0	0.200	ENG15	+H₂O +OH -SiO	LIT94

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

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	F_peak	List	Detection	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			(Jy)		Yes/No
1	07 20 59	+24 59 59	193.1653	17.2416	G193.164+17.239	BM Gem	0.600	ENG15	-H₂O -OH -SiO	LIT94
	07 20 59	+24 59 59	193.1653	17.2416	G193.164+17.239	BM Gem	0.750	ENG15	-H₂O -OH -SiO	LIT94
	07 20 59	+24 59 59	193.1653	17.2416	G193.164+17.239	BM Gem	0.750	ENG15	-H₂O -OH -SiO	LIT94
2	08 02 5.4	-38 11 55	254.2850	-4.0002	G254.284-4.000	Hen 38	2.100	ENG15	-H₂O -OH -SiO	LIT94
	08 02 5.4	-38 11 55	254.2850	-4.0002	G254.284-4.000	Hen 38	0.600	ENG15	-H₂O -OH -SiO	LIT94
3	08 58 53.9	-60 47 37	278.0690	-9.7152	G278.069-9.715	Mc79-11	1.500	ENG15	+H₂O -OH	LIT94
	08 58 53.9	-60 47 37	278.0690	-9.7152	G278.069-9.715	Mc79-11	0.750	ENG15	+H₂O -OH	LIT94
4	23 20 1.8	+47 14 26	107.2433	-12.8276	G107.236-12.824	EU And	0.210	ENG15	+H₂O -OH -SiO	LIT94

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 LIT94

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