Recalibrating the Cosmic Star Formation History
  The calibrations linking observed luminosities to the star formation rate
depend on the assumed stellar population synthesis model, initial mass
function, star formation and metal enrichment history, and whether reprocessing
by dust and gas is included. Consequently the shape and normalisation of the
inferred cosmic star formation history is sensitive to these assumptions. Using
v2.2.1 of the Binary Population and Spectral Synthesis (\bpass) model we
determine a new set of calibration coefficients for the ultraviolet,
thermal-infrared, and, hydrogen recombination lines. These ultraviolet and
thermal infrared coefficients are 0.15-0.2 dex higher than those widely
utilised in the literature while the H$\alpha$ coefficient is $\sim 0.35$ dex
larger. These differences arise in part due to the inclusion binary evolution
pathways but predominantly reflect an extension in the IMF to 300 $M_{\odot}$
and a change in the choice of reference metallicity. We use these new
coefficients to recalibrate the cosmic star formation history, and find
improved agreement between the integrated cosmic star formation history and the
in-situ measured stellar mass density as a function of redshift. However, these
coefficients produce new tension between star formation rate densities inferred
from the ultraviolet and thermal-infrared and those from H$\alpha$.
