Detection of a weak maser emission pedestal associated with the SiO maser

Details Detection of a weak maser emission pedestal associated with the SiO maser Detection of a weak maser emission pedestal associated with the SiO maser

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...224..512s&link_type=abstract

Astrophysical Journal, Part 1, vol. 224, Sept. 1, 1978, p. 512-519.

Astronomy and Astrophysics

Astrophysics

34

Emission Spectra, Interstellar Masers, Maser Outputs, Silicon Oxides, Stellar Radiation, Variable Stars, Graphs (Charts), Late Stars, Molecular Spectra, Radial Velocity, Semiregular Variable Stars, Spectral Signatures, Stellar Envelopes, Stellar Rotation

Scientific paper

Results are reported for high-spectral-resolution observations of the v = 1, J = 1-0 SiO maser sources at 43,122.027 MHz (6.95 mm wavelength) associated with the variable stars Omega Cet, NML Tau, VY CMa, R Leo, W Hya, VX Sgr, NML Cyg, and R Cas. A weak underlying maser emission pedestal is clearly observed in the spectra of all but NML Cyg and R Cas. The data indicate that the underlying pedestal of SiO emission appears to originate in a shell-like region around the star, has a thermal appearance even though it must be due to weak maser emission, and appears to be part of the spectral signature of SiO maser emission from late-type stars. It is found that the center velocities of the pedestals may be used to determine stellar radial velocities. Observations of large-scale time variations in the intensity of the Ori A SiO maser and the detection of weak maser pedestals associated with each of the two strong emission-feature groups in Orion are also discussed. It is suggested that the Orion molecular cloud might contain two late-type long-period variable stars that may be semiregular variables.

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