NGC 1614: A Laboratory for Starburst Evolution

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Abstract
The modest extinction and reasonably face-on viewing geometry make the luminous IR galaxy NGC1614 an ideal laboratory for study of a powerful starburst. HST/NICMOS observations show: 1.) deep CO stellar absorption, tracing a starburst nucleus about 45 pc in diameter; 2.) surrounded by a ~600 pc diameter ring of supergiant HII regions revealed in Pa$alpha$ line emission; 3.) lying within a molecular ring indicated by its extinction shadow in H-K; 4.) all at the center of a disturbed spiral galaxy. The luminosities of the giant HII regions in the ring are extremely high, an order of magnitude brighter than 30 Doradus. The relation of deep stellar CO bands to surrounding ionized gas ring to molecular gas indicates that the luminous starburst started in the nucleus and is propagating outward into the surrounding molecular ring. This hypothesis is supported by evolutionary starburst modeling that shows that the properties of NGC1614 can be fitted with two short-lived bursts of star formation separated by 5 Myr. The total dynamical mass of the starburst region of 1.3x10^9 Msol is mostly accounted for by the old pre-star burst stellar population. Although our starburst models use a modified Salpeter IMF, the tight mass budget suggests that the IMF may contain relatively more 10-30 Msol stars and fewer low mass stars than the Salpeter function. The dynamical mass is nearly 4 times smaller than the mass of molecular gas estimated from the standard ratio of 12CO(1-0) to H2. A number of arguments place the mass of gas in the starburst region at ~25% of the dynamical mass, nominally about 1/15 and with an upper limit of 1/10 of the amount estimated from 12CO and the standard ratio. (Abridged)
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