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Shock tracers in the molecular cloud G1.6-0.025

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Abstract

Observations of the molecular cloud G1.6-0.025 in the 2K-1K and J 0-J −1 E series and 5−1-40 E line of CH3OH, the (2-1) and (3-2) lines of SiO, and the 7−7-6−6 line of HNCO are described. Maps of the previously observed extended cloud with V lsr∼50 km/s and high-velocity clump with V lsr∼160 km/s, as well as a newly detected clump with V lsr∼0 km/s, have been obtained. The extended cloud and high-velocity clump have a nonuniform structure. The linewidths associated with all the objects are between 20 and 35 km/s, as is typical of clouds of the Galactic center. In some directions, emission at velocities from 40 to 160 km/s and from −10 to +75 km/s is observed at the clump boundaries, testifying to a connection between the extended cloud and the high-velocity clump and clump at V lsr∼0 km/s. Compact maser sources are probaby contributing appreciably to the emission of the extended cloud in the 5−1-40 E CH3OH line. Non-LTE modeling of the methanol emission shows that the extended cloud and high-velocity clump have a relatively low hydrogen density (<104 cm−3). The specific column density of methanol in the extended cloud exceeds 6×108 cm−3s, and is 4×108−6×109 cm−3s in the high-velocity clump. The kinetic temperatures of the extended cloud and high-velocity clump are estimated to be <80 K and 150–200 K, respectively. Possible mechanisms that can explain the link between the extended cloud with V lsr∼50 km/s and the clumps with V lsr∼0 km/s and ∼160 km/s are briefly discussed.

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Translated from Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l}\) Zhurnal, Vol. 79, No. 12, 2002, pp. 1059–1073.

Original Russian Text Copyright © 2002 by Sali\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l}\), Sobolev, Kalinina.

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Salii, S.V., Sobolev, A.M. & Kalinina, N.D. Shock tracers in the molecular cloud G1.6-0.025. Astron. Rep. 46, 955–968 (2002). https://doi.org/10.1134/1.1529254

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