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The Recent Star Formation Histories of Nearby Galaxies

Published online by Cambridge University Press:  01 December 2006

Evan D. Skillman ,
John M. Cannon ,
Andrew E. Dolphin ,
Robert C. Kennicutt Jr. ,
Janice C. Lee ,
Fabian Walter  and
Daniel R. Weisz
Evan D. Skillman
Affiliation:
Astronomy Department, University of Minnesota, Minneapolis, MN 55455, USA email: skillman@astro.umn.edu
John M. Cannon
Affiliation:
Astronomy Department, Wesleyan University, Middletown, CT 06457, USA
Andrew E. Dolphin
Affiliation:
Raytheon Corporation, Tuscon, Arizona, USA Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA
Robert C. Kennicutt Jr.
Affiliation:
Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
Janice C. Lee
Affiliation:
National Optical Astronomy Observatory, P.O. Box 26732, Tucson, AZ 85726, USA
Fabian Walter
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
Daniel R. Weisz
Affiliation:
Astronomy Department, University of Minnesota, Minneapolis, MN 55455, USA email: skillman@astro.umn.edu
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Abstract

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Recent (≤ 0.5 Gyr) star formation histories have a large impact on the observable properties of galaxies. Using HST/ACS observations, we have used the blue helium burning (BHeB) stars to construct spatially resolved star formation histories of M81 group dwarf galaxies with a time resolution of roughly 30 Myr over the last 500 Myr. We have designed a sample of ten galaxies spanning ranges of 6 magnitudes in luminosity, 1000 in current star formation rate, and 0.5 dex in metallicity. The ACS observations allow us to directly observe the strength and spatial relationships of all of the recent star formation in these galaxies. These observations are complemented by high-quality ancillary data (e.g., Spitzer, UV/optical/H-alpha/NIR, VLA HI). Our resolved star formation maps will be compared with star formation rates inferred from H-alpha, UV, and IR observations – allowing an independent calibration of these techniques. Given the ranges in metallicity, these observations will provide calibrations of stellar evolution tracks for young, low metallicity stars. These observations will also enable us to construct prescriptions of how star formation and feedback depend on metallicity, size, gas content, and current star formation rates in galaxies. Finally, I note that the new observations becoming available as a part of the ANGST (ACS Nearby Galaxies Survey Treasury Program) will allow a large number of dwarf galaxies to be analyzed in this way.

Keywords

galaxies: stellar contentgalaxies: evolutiongalaxies: dwarf
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 286 - 289
Copyright
Copyright © International Astronomical Union 2007

References

Binney, J., & Tremaine, S. 1987, Galactic Dynamics, Princeton University Press, p. 442Google Scholar
Dohm-Palmer, R.C., & Skillman, E.D. 2002 AJ 123, 1433CrossRefGoogle Scholar
Dohm-Palmer, R.C., Skillman, E.D., Saha, A., Tolstoy, E., Mateo, M., Gallagher, J.S.Hoessel, J., Chiosi, C., & Dufour, R.J. 1997, AJ 114, 2514CrossRefGoogle Scholar
Dohm-Palmer, R.C., Skillman, E.D., Gallagher, J.S., Tolstoy, E., Mateo, M., Dufour,, R.J., Saha, A., Hoessel, J., & Chiosi, C. 1998, AJ 116, 1227CrossRefGoogle Scholar
Dohm-Palmer, R.C., Skillman, E.D., Mateo, M., Saha, A., Dolphin, A., Tolstoy, E., Gallagher, J.S. & Cole, A.A. 2002, AJ 123, 813CrossRefGoogle Scholar
Dolphin, A. E. et al. , 2003, AJ, 126, 187CrossRefGoogle Scholar
Kroupa, P. 1995, MNRAS, 277, 1522CrossRefGoogle Scholar
Terlevich, E. 1987, MNRAS, 224, 193CrossRefGoogle Scholar
Williams, B. F. 2003, AJ, 126, 1312CrossRefGoogle Scholar