Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...489..636k&link_type=abstract
Astrophysical Journal v.489, p.636
Astronomy and Astrophysics
Astronomy
166
Ism: Abundances, Galaxies: Individual Ngc Number: Ngc 1569, Galaxies: Abundances, Galaxies: Evolution, Galaxies: Starburst, Galaxies: Star Clusters
Scientific paper
We present a long-slit optical spectrophotometric survey covering 0.05 kpc2 in the nearby irregular "post-starburst" galaxy NGC 1569 to search for chemical gradients and inhomogeneities in the interstellar medium. Despite the presence of two massive evolved star clusters and numerous H II regions, we find no evidence for chemical gradients or inhomogeneities that may be attributed to enrichment from the recent star formation activity. The chemical properties at all locations are consistent with the results from the highest signal-to-noise ratio spectra: 12 + log (O/H) = 8.19 +/- 0.02, log (N/O) = -1.39 +/- 0.05, He/H = 0.080 +/- 0.003. No localized chemical self-enrichment ("pollution") from massive star evolution is found, even though the data are sensitive to the chemical yields from as few as two or three massive stars. Flat chemical abundance profiles appear to be the rule rather than the exception in low-mass galaxies, even though the expected yield of heavy elements produced by massive stars in young starbursts is substantial. Based on a typical IMF, a dynamical mass of ~3 x 105 M&sun;, and an age of 20 Myr, roughly 450 stars in excess of 20 M&sun; should have already exploded as supernovae within the star cluster, A, in NGC 1569, releasing ~1000 M&sun; of oxygen and ~8 M&sun; of nitrogen. Strong chemical signatures in the surrounding interstellar material should be detected unless one or more of the following are true: (1) different star-forming regions throughout the studied galaxies "conspire" to keep star formation rates and global abundances uniform at all times; (2) ejecta from stellar winds and supernovae are transported to all corners of the galaxy on timescales of <107 yr and are mixed instantaneously and uniformly; or (3) freshly synthesized elements remain unmixed with the surrounding interstellar medium and reside in a hard-to-observe hot 106 K phase or a cold, dusty, molecular phase. We advance the third scenario as the most plausible, and we suggest ways to locate the chemical products of massive star formation in starburst galaxies. Any successful model for chemical enrichment in these systems must be able to reproduce the appearance of chemical homogeneity on spatial scales of ~20-1000 pc and on temporal scales that are longer than the lifetimes of prominent H II regions (~107 yr). Such long timescales imply that the instantaneous recycling approximation sometimes used in galactic chemical evolution modeling is not generally applicable.
Kobulnicky Henry A.
Skillman Evan D.
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