NH3 in the molecular ring at the Galactic Center

Details NH3 in the molecular ring at the Galactic Center NH3 in the molecular ring at the Galactic Center

Apr 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987aipc..155...99j&link_type=abstract

AIP Conference Proceedings, Volume 155, pp. 99-102 (1987).

Computer Science

2

Scientific paper

Using the VLA, the NH3 (J,K)=(3,3) inversion line has been mapped toward the Galactic center in a 2' field with 11` by 8` angular resolution (~0.5 pc at 10 kpc). A number of NH3 condensations coincident with the molecular ring mapped in HCN by Gusten et al. (1986) are detected. These condensations are well localized (<1 pc), have typical peak brightness temperatures ~1-5 K, and have typical linewidths ~15 km s-1. We estimate the masses of the individual condensation to be on the order of 100 Msolar. The differences in the distribution of HCN 1 and NH3 may be caused by chemistry, by foreground absorption of the HCN due to intervening cold gas, or by differences in excitation. Detailed comparison with Ne II data 2 supports a model of photoionization of cloud material on the surfaces of the condensations facing the Galactic center. Assuming that the ionized gas flows toward the Galactic center and that the NH3 emission defines the ``mass-weighted'' velocity, we conclude that the western side of the ring is behind the Galactic center while the eastern side is in front of the Galactic center.

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