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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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Display associated data

IRAS source	IRAS coordinates (RA, Dec)	IRAS flux density (F12,F25,F60,F100)
2MASS source	2MASS coordinates (RA, Dec)	2MASS magnituted (J,H,K)

Variable star	Variable star parameters	Star Formation Region name	Star Formation Region parameters
WISE source	WISE coordinates (RA, Dec)	WISE magnitudes (w1, w2, w3, w4)
Akari IRC source	Akari IRC coordinates (RA, Dec)	Akari IRC fluxes (S09, S18)
Akari FIS source	Akari FIS coordinates (RA, Dec)	Akari FIS fluxes (S65, S90, S140, S160)

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DSS (optical)	2MASS (JHK)	WISE (4-22 um)	IRAC (3-8 um)	GLIMPSE 360 (3.6-4.5 um)	PACS color (70-160 um)	SPIRE color (250-500 um)
AKARI color (60-160 um)	NVSS (1.4 GHz)	SDSS (optical+NIR)	Image size: arcsec (default is 120 arcsec)
			Image size: arcsec (default is 120 arcsec)

Position of H₂O maser detection

DSS colored	2MASS colored	WISE colored
SDSS color	IRAC color I1,I2,I4	GLIMPSE 360
PACS color (70-160 um)	SPIRE color (250-500 um)	NVSS (1.4GHz)
UKIDSS K	2MASS K

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

Interferometry data

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Detection table from Lindqvist et al. (1991)

Non-detection table from Lindqvist et al. (1991)