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Description
The results of spectral observations of the region of massive star formation L379IRS3 (IRAS 18265-1517) are presented. The observations were carried out with the 30-m Pico Veleta radio telescope (Spain) at seven frequencies in the 1-mm, 2-mm, and 3-mm wavelength bands. Lines of 24 molecules were detected, from simple diatomic or triatomic species to complex eight- or nine-atom compounds such as CH_3_OCHO or CH_3_OCH_3_. Rotation diagrams constructed from methanol and methyl cyanide lines were used to determine the temperature of the quiescent gas in this region, which is about 40-50K. In addition to this warm gas, there is a hot component that is revealed through high-energy lines of methanol and methyl cyanide, molecular lines arising in hot regions, and the presence of H_2_O masers and Class II methanol masers at 6.7GHz, which are also related to hot gas. One of the hot regions is probably a compact hot core, which is located near the southern submillimeter peak and is related to a group of methanol masers at 6.7GHz. High-excitation lines at other positions may be associated with other hot cores or hot post-shock gas in the lobes of bipolar outflows. The rotation diagrams can be use to determine the column densities and abundances of methanol (10^-9^) and methyl cyanide (about 10^-11^) in the quiescent gas. The column densities of A- and E-methanol in L379IRS3 are essentially the same. The column densities of other observed molecules were calculated assuming that the ratios of the molecular level abundances correspond to a temperature of 40 K. The molecular composition of the quiescent gas is close to that in another region of massive star formation, DR21(OH). The only appreciable difference is that the column density of SO2 in L379IRS3 is at least a factor of 20 lower than the value in DR21(OH). The SO_2_/CS and SO2/OCS abundance ratios, which can be used as chemical clocks, are lower in L379IRS3 than in DR21(OH), suggesting that L379IRS3 is probably younger than DR21(OH).
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