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LIN91 - SiO maser emission from OH/IR stars close to the Galactic centre

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Short title: Lindqvist et al. (1991)
Authors: Lindqvist, M. Ukita, N. Winnberg, A. Johansson, L. E. B.
Journal: Astronomy and Astrophysics (ISSN 0004-6361), vol. 250, no. 2, Oct. 1991, p. 431-436. Research supported by NFR.
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Abstract
Forty-three- and 86-GHz SiO maser emission is explored simultaneously from a sample of 31 OH/IR stars close to the Galactic center. Eleven envelopes were detected in the 43-GHz transitions and two solely in the v = 2 transition. Only upper limits were obtained at 86 GHz. Luminosities were obtained in the intervals (70-380) x 10 exp 42 and (80-370) x 10 exp 42 photon/s for v = 1 and v = 2, respectively. These luminosities are compared with those of seven OH/IR stars in the Galactic disk. No significant difference is found between the luminosity distributions of the two stellar samples, given the small number of objects. The luminosity of the v = 2 line is on the average about 1.5 times stronger than the luminosity of the v = 1 line. The upper limits of the 86-GHz data compared to the detected 43 GHz data suggest that the 86-GHz maser is weaker than the 43-GHz maser. The line widths and the line profiles are comparable to many of the simple structure spectra observed in ordinary Miras.

Abstract

Forty-three- and 86-GHz SiO maser emission is explored simultaneously from a sample of 31 OH/IR stars close to the Galactic center. Eleven envelopes were detected in the 43-GHz transitions and two solely in the v = 2 transition. Only upper limits were obtained at 86 GHz. Luminosities were obtained in the intervals (70-380) x 10 exp 42 and (80-370) x 10 exp 42 photon/s for v = 1 and v = 2, respectively. These luminosities are compared with those of seven OH/IR stars in the Galactic disk. No significant difference is found between the luminosity distributions of the two stellar samples, given the small number of objects. The luminosity of the v = 2 line is on the average about 1.5 times stronger than the luminosity of the v = 1 line. The upper limits of the 86-GHz data compared to the detected 43 GHz data suggest that the 86-GHz maser is weaker than the 43-GHz maser. The line widths and the line profiles are comparable to many of the simple structure spectra observed in ordinary Miras.

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