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- W2108477466 abstract "Dense molecular clouds are critical to the activity occurring in galactic nuclei. They are the active component from which starbursts arise and this dense interstellar gas may be the fuel for AGNs. In both the nearby infrared bright galaxies (e.g., M82, NGC 253, and IC342) and the ultraluminous IRAS galaxies, high resolution millimeter line mapping has shown extremely high gas surface densities in the central kpc. Often a significant fraction (> 25%) of the total molecular line emission from the galaxy arises from these central regions. New maps at resolutions down to 0.8″ of the ultraluminous IRAS galaxies reveal kinematic gradients parallel to the major axis of the CO intensity distribution, suggesting that the gas is situated in a central rotating disk. The most extreme central concentrations are seen in Arp 220 and Mrk 231 (Sey 1), which have now been mapped in both the 2.6 and 1.3 mm CO transitions. In both galaxies, the high observed CO brightness temperatures indicate large area filling factors with mean H2 densities exceeding 104cm~3. To produce the observed luminosities, the star formation rates must be ∼100 M⊙ yr−1 within the central 500 pc radius. Estimated time scales for both the dynamical evolution and the exhaustion of the observed central ISM are typically 2 × 108 years." @default.
- W2108477466 created "2016-06-24" @default.
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- W2108477466 date "1997-01-01" @default.
- W2108477466 modified "2023-09-23" @default.
- W2108477466 title "Molecular Gas in Galactic Nuclei" @default.
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- W2108477466 doi "https://doi.org/10.1007/978-94-011-5414-7_53" @default.
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