Testing star formation rate indicators using galaxy merger simulations and radiative transfer

Details Testing star formation rate indicators using galaxy merger simulations and radiative transfer Testing star formation rate indicators using galaxy merger simulations and radiative transfer

Apr 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010iaus..262..257h&link_type=abstract

Stellar Populations – Planning for the Next Decade, Proceedings of the International Astronomical Union, IAU Symposium, Volume 2

Astronomy and Astrophysics

Astronomy

Stars: Formation, Galaxies: Stellar Content, Galaxies: Fundamental Parameters, Galaxies: Starburst, Galaxies: High-Redshift, Dust, Extinction, Radiative Transfer

Scientific paper

We discuss our ongoing project analyzing N-body/smoothed-particle hydrodynamics simulations of isolated and merging galaxies, performed using GADGET-2 (Springel 2005), with the 3-D adaptive grid, polychromatic Monte Carlo radiative transfer code SUNRISE (Jonsson 2006). We apply commonly used UV, optical, and IR star formation rate (SFR) indicators to the integrated spectral energy distributions (SEDs) of the simulated galaxies in order to determine how well the SFR indicators recover the instantaneous SFR in the simulations. The models underlying each SFR indicator must necessarily make assumptions about physical properties of the galaxies, e.g., the star formation history (SFH), whereas all such properties are known in the simulations. This enables us to test and compare SFR indicators in a way that is complementary to observational studies. We present one preliminary result of interest: even after correcting the Hα luminosity for dust using the Calzetti et al. (2000) attenuation law the SFR is significantly underestimated for simulated galaxies with SFR ≳ 10 M&sun; yr-1.

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