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Mapping the roots of the galactic outflow in NGC1569 |
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| Authors: | Mark S Westmoquette Linda J Smith Jay S Gallagher III Katrina M Exter |
| Institution: | 1. Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK 4. Space Telescope Science Institute and European Space Agency, 3700 San Martin Drive, Baltimore, MD, 21218, USA 2. Department of Astronomy, University of Wisconsin–Madison, 5534 Sterling, 475 North Charter St., Madison, WI, 53706, USA 3. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, 21218, USA |
| Abstract: | The exact nature of the interaction between hot, fast-flowing star-cluster winds and the surrounding clumpy interstellar medium (ISM) in starburst galaxies has very few observational constraints. Besides furthering our knowledge of ISM dynamics, detailed observations of ionised gas at the very roots of large-scale outflows are required to place limits on the current generation of high-resolution galactic wind models. To this end, we conduct a detailed investigation of the ionised gas environment surrounding the young star clusters in the starburst galaxy NGC1569. Using high spatial and spectral-resolution Gemini/GMOS integral-field unit observations, we accurately characterise the line-profile shapes of the optical nebular emission lines and find a ubiquitous broad (～300 km?s?1) component underlying a bright narrower component. By mapping the properties of the individual line components, we find correlations that suggest that the broad component results from powerful cluster wind–gas clump interactions. We propose a model to explain the properties of the line components and the general turbulent state of the ISM. |
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