Shock Tracers in the Molecular Cloud G1.6-0.025

Details Shock Tracers in the Molecular Cloud G1.6-0.025 Shock Tracers in the Molecular Cloud G1.6-0.025

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002arep...46..955s&link_type=abstract

Astronomy Reports, Vol. 46, Issue 12, pp. 955-968

Astronomy and Astrophysics

Astronomy

6

Scientific paper

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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