Other
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21431104w&link_type=abstract
American Astronomical Society, AAS Meeting #214, #311.04; Bulletin of the American Astronomical Society, Vol. 41, p.747
Other
Scientific paper
We use deep HST/ACS F555W and F814W photometry of resolved stars in the M81 Group dwarf irregular galaxy Holmberg II to study the hypothesis that the holes identified in the VLA HI synthesis observations are created by stellar feedback. Color-magnitude diagrams (CMDs) show that the stars interior to the HI holes are not coherent, single-aged clusters, but rather, multi-age populations. From the CMDs, we measure the star formation histories and find that significant star formation occurred during the kinematic age for the majority of the holes and that the energy due to this star formation is sufficient to have created the HI holes. Comparing the stellar populations inside the HI holes to those of select control fields, i.e., similar sized regions that span a range in HI column density, we find that while star formation can create HI holes, it does not always do so. We compare the deep HST/ACS photometry to other common tracers of recent star formation (OB stars, Hα, 24μm, and UV fluxes) and find that at best these other methods only find the young stellar population ˜ 50% of the time. The CMDs and spatial distribution of young stars suggest that the two main factors contributing to this low correlation are the quick dissolution of star clusters into the field (< 10 Myr) and stochastic effects due to the small number of young stars inside each hole. Using Monte Carlo simulations, we show that low level star formation could also be responsible for HI holes located beyond the optical radius of the galaxy. Support for this work was provided by NASA through grant GO-10605 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555.
Cannon John M.
Dolphin Andrew E.
Kennicutt Robert C. Jr.
Lee Julian
Skillman Evan D.
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