Testing the Effectiveness of the H-alpha/UV flux Ratio in Determining Star Formation Rates in Dwarf Galaxies

Details Testing the Effectiveness of the H-alpha/UV flux Ratio in Determining Star Formation Rates in Dwarf Galaxies Testing the Effectiveness of the H-alpha/UV flux Ratio in Determining Star Formation Rates in Dwarf Galaxies

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21732805m&link_type=abstract

American Astronomical Society, AAS Meeting #217, #328.05; Bulletin of the American Astronomical Society, Vol. 43, 2011

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We use an N-body/smoothed particle hydrodynamic simulation to study the evolution of H-alpha and UV star formation indicators in a starbursting dwarf galaxy. H-alpha based observations of star-formation under-predict the star formation rate (SFR) relative to the FUV determined SFR. The two implied scenarios: bursty star formation in dwarf galaxies or a non-uniform stellar initial mass function (IMF), cannot currently be distinguished by observation. Simulations allow us to trace star formation as stellar populations evolve, and directly measure the star formation history. In addition to being fully cosmological, with high mass resolution and a physically motivated description of star formation and feedback, our simulation is the first to correctly describe the dark matter and baryon distribution of small galaxy. Using mock multi-wavelength observations, we examine the H-alpha and UV SFRs in order to trace the evolution of the H-alpha to UV flux ratio as a function of SFR. Examining the evolution of these star formation indicators will allow us to determine whether the observed discrepancies in the fluxes could stem from the more rapid decrease of H-alpha flux from aging stellar populations.

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