Mapping the roots of the galactic outflow in NGC1569

Details Mapping the roots of the galactic outflow in NGC1569 Mapping the roots of the galactic outflow in NGC1569

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009ap%26ss.324..187w&link_type=abstract

Astrophysics and Space Science, Volume 324, Issue 2-4, pp. 187-193

Astronomy and Astrophysics

Astrophysics

2

Ism: Jets And Outflows, Ism: Kinematics And Dynamics, Galaxies: Ism, Galaxies: Starburst

Scientific paper

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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