Large- and Small-Scale Feedback in the Starburst Canters of Galaxies.pdf

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Large- and Small-Scale Feedback in the Starburst Canters of Galaxies.pdf

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Large- and Small-Scale Feedback in the Starburst Canters of Galaxies

a r X i v : a s t r o - p h / 0 4 0 4 4 4 6 v 1 2 2 A p r 2 0 0 4 The Interplay among Black Holes, Stars and ISM in Galactic Nuclei Proceedings IAU Symposium No. 222, 2004 Th. Storchi Bergmann, L.C. Ho H.R. Schmitt, eds. c? 2004 International Astronomical Union DOI: 00.0000/X000000000000000X Large– and Small–Scale Feedback in the Starburst Centers of Galaxies Daniela Calzetti1 1Space Telescope Science Institute, Baltimore, MD 21218, USA email: calzetti@stsci.edu Abstract. The interplay between stellar populations and gas in local starburst galaxies is analyzed using images from the Hubble Space Telescope to map the ages of the young stellar components and to isolate the contribution of shocks on spatial scales ranging from a few tens of pc to ～1 kpc. The shocked gas represents a small fraction of the total ionized gas in these objects, yet it can have profound effects on the long–term evolution of the starburst, which may include the triggering of new star formation. 1. Introduction The evolution of galaxies and of the intergalactic/intracluster medium (IGM/ICM) are closely connected, via the continuous interchange between the ISM and the IGM/ICM. The heating and metal enrichment of the IGM/ICM, and the enrichment of galaxies’ ISM with pristine gas via infall from the IGM are manifestations of this close con- nection. Evidence for gas outflows from galaxies has been found at redshift as high as ～3 (Pettini et al. 2000), and may have contributed to the early pollution of the IGM (Ellison et al. 2000). The driving mechanism for the energy and metal pollution of the IGM/ICM is the feedback from star formation. In the basic scenario, the combined effects of ejecta and energy release from supernovae and massive stars in regions of intense star formation form superbubbles that sweep up the surrounding medium and produce cavities containing hot, shocked gas (Weaver et al. 1977). If the bubble has enough energy to expand to a size of a few times the scale height of th