Other
Scientific paper
Jul 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...239..519g&link_type=abstract
Astrophysical Journal, Part 1, vol. 239, July 15, 1980, p. 519-525.
Other
39
Emission Spectra, Interstellar Masers, Milky Way Galaxy, Nebulae, Orion Nebula, Silicon Oxides, Star Formation, Data Acquisition, Data Reduction, Interstellar Matter, Spectroscopic Telescopes, Stellar Envelopes, Stellar Mass Ejection, Thermal Emission
Scientific paper
The J = 1-0 rotational transitions of SiO at 43 GHz have been observed toward Orion-KL with the Effelsberg 100 m telescope. The ground vibrational transition of SiO in Orion has a narrow line at -5.5 km s-1, superposed on a broad, flat-topped emission over a range of 35 ± 5 km s-1. The narrow "spike" is probably maser emission, and the broad feature may be interpreted as optically thin thermal emission or weak maser emission from an expanding circumstellar envelope. The υ = 0 emission in Orion is not resolved by our 24" beam and comes from the same position as the strong maser lines in the υ = 1 and 2 transitions. The mass loss from this source can only drive the high-velocity flow seen in other molecular lines if the SiO abundance in the circumstellar shell is very low, compared with the cosmic abundance of silicon. There are no SiO masers in other regions of star formation, to our 2 σ detection limits of 2-27 Jy. This suggests that there is either an evolved giant or supergiant in the Orion Molecular Cloud, or else the Orion SiO maser source is a unique object in the Galaxy.
Baars Jacob W. M.
Downes Dennis
Genzel Reinhard
Pankonin Vernon
Schwartz Phil R.
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