The Structure and Kinematics of Cold Molecular Gas in NGC 1068

Details The Structure and Kinematics of Cold Molecular Gas in NGC 1068 The Structure and Kinematics of Cold Molecular Gas in NGC 1068

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997ap%26ss.248...51h&link_type=abstract

Astrophysics and Space Science, Volume 248, Issue 1-2, pp. 51-57

Astronomy and Astrophysics

Astrophysics

4

Scientific paper

I summarize fully-sampled observations of the 3 mm emission from CO and HCN in the inner arcminute of NGC 1068. The CO emission is distributed in the form of a molecular bar, coincident with the infrared bar, from which emanate two spiral arms. A relatively weak concentration of CO line emission is found at the nucleus. By contrast, the HCN emission is strongly concentrated at the center, with relatively weak emission in the region of the star-forming arms. The ratio of HCN to CO integrated intensities is about 0.6 over the central r ≉ 175 pc and is the highest ratio measured in the center of any galaxy; the ratio reflects the high thermal pressure (TK ~ 50 K, n[H2] ~ 4 × 106 cm-3) in the few hundred parsecs surrounding the nucleus.

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