NGC 4314. IV. Photometry of Star Clusters with Hubble Space Telescope - History of Star Formation in the Vicinity of a Nuclear Ring

Details NGC 4314. IV. Photometry of Star Clusters with Hubble Space Telescope - History of Star Formation in the Vicinity of a Nuclear Ring NGC 4314. IV. Photometry of Star Clusters with Hubble Space Telescope - History of Star Formation in the Vicinity of a Nuclear Ring

2001-11-30

arxiv.org/abs/astro-ph/0111599v2

Astronomy and Astrophysics

Astrophysics

To appear in The Astronomical Journal, March 2002. For a version with higher quality figures, see http://clyde.as.utexas.edu

Scientific paper

10.1086/338895

Using HST WFPC2 images, we have obtained U, B, V, I, and H-alpha photometry for 76 star clusters in the nuclear star-forming ring of the barred spiral galaxy NGC 4314. These clusters are likely associated with an inner Inner Lindblad Resonance, or IILR. The blue colors and H-alpha emission for most of these clusters imply very young ages of 1-15 Myr. Age estimates based on several reddening-free parameters indicate that the present epoch of star formation has lasted at least 30 Myr. By estimating the masses of stars in the clusters and comparing with the H-alpha luminosity, we conclude that a significant fraction of ongoing star formation in the nuclear ring of NGC 4314 occurs in clusters. The cluster masses identify these as young open clusters, not young globular clusters. Further out in the galaxy, just exterior to the ring of young stars, previous ground-based observations revealed two symmetric stellar spiral arms which may be associated with an outer Inner Lindblad Resonance, or OILR. With our HST data, we have revealed part of this structure and its colors in more detail. The spiral arm colors are consistent with stellar ages between 40 and 200 Myr. The age difference between the inner ring of young stars (IILR) and the larger oval-like feature containing the blue arms (OILR) supports an interpretation of the morphology of the nuclear region of NGC 4314 that requires a reservoir of gas that becomes more compact over time. We speculate that as the gas distribution becomes more centrally concentrated, it interacts with these two resonances. Each resonance triggers star formation, resulting in two distinct epochs of star formation.

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