Other
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21344225g&link_type=abstract
American Astronomical Society, AAS Meeting #213, #442.25; Bulletin of the American Astronomical Society, Vol. 41, p.323
Other
Scientific paper
We present a multiwavelength study of the massive stellar population of the nearby, irregular, low-metallicity Wolf-Rayet galaxy IC 4662 (D ˜ 2 Mpc, Z ≈ 0.1-0.2 Z&sun;). Its central starburst is dominated by two embedded star-formation regions. Their radio-to-IR
spectral energy distributions are consistent with a simple model of their structure as a star cluster exciting an HII region within a dust
cocoon. These systems are similar to, but somewhat more evolved than the very compact massive embedded star-formation regions, dubbed ultra-dense HIIRs (UDHIIs), of He 2-10 and NGC 5253: the obscured clusters have less gas and dust still surrounding them, and their exciting star clusters appear older. High angular-resolution optical data from Hubble ACS and Spitzer mid-IR spectroscopy provide additional constraints on the properties of the underlying stellar populations in the central starburst and the surrounding matter. The exciting stellar populations have low metallicity and high excitation, and for a Kroupa IMF their ages are ˜4 Myr and masses are ˜3×105 M&sun;. They are resolved by ACS into several 103-104 M&sun; clusters and individual massive stars rather than massive monolithic Super Star Clusters (SSCs). From the mid-IR spectra we derive extinctions equivalent to AV ≈ 20-25 mag, which are much higher than found at shorter wavelengths; thus the dust is well-mixed with the emitting gas rather than in a foreground screen. The presence of long-lived dust mixed with hot, excited gas in a massive star-formation region supports other evidence for dust-driven winds in young SSCs, and it could help resolve the missing energy problem in cluster winds, superbubbles, and even galactic superwinds.
Gilbert Andrea M.
Vacca William D.
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