1. IMF of the Trapezium cluster, a young star cluster (Muench et al. 2002)

2. IMF inferred based on field stars (red) and based on a variety of clusters (blue, green, and black) (Kroupa 2002)

4. Observed HR diagrams (left) in four regions of NGC 2976 (below) (Williams et al. 2009). Contours show observed stars; colored lines show properties for stellar populations 20 Myr Myr old.

5. Observed HR diagram (left) and best-fitting model (right) for the OUTER region in NGC 2976.

6. Star formation history for the four regions in NGC 2976, showing that, in this galaxy, star formation has occurred more recently in the inner parts than the outer parts of the galaxy.

7. Atomic hydrogen distribution (green) and star formation distribution (blue)

8. SFR versus atomic gas (left) and molecular gas (right) (Bigiel et al