We investigate star formation rate ( SFR ) calibrations in light of recent developments in the modeling of stellar rotation .
Using new published non-rotating and rotating stellar tracks , we study the integrated properties of synthetic stellar populations and find that the UV to SFR calibration for the rotating stellar population is 30 % smaller than for the non-rotating stellar population , and 40 % smaller for the H \alpha to SFR calibration .
These reductions translate to smaller SFR estimates made from observed UV and H \alpha luminosities .
Using the UV and H \alpha fluxes of a sample of \sim 300 local galaxies , we derive a total ( i.e. , sky-coverage corrected ) SFR within 11 Mpc of 120 – 170 { M _ { \odot } yr ^ { -1 } } and 80 – 130 { M _ { \odot } yr ^ { -1 } } for the non-rotating and rotating estimators , respectively .
Independently , the number of core-collapse supernovae discovered in the same volume requires a total SFR of 270 ^ { +110 } _ { -80 } { M _ { \odot } yr ^ { -1 } } , suggesting a tension with the SFR estimates made with rotating calibrations .
More generally , when compared with the directly estimated SFR , the local supernova discoveries strongly constrain any physical effects that might increase the energy output of massive stars , including , but not limited to , stellar rotation .
The cosmic SFR and cosmic supernova rate data on the other hand show the opposite trend , with the cosmic SFR higher than that inferred from cosmic supernovae , constraining a significant decrease in the energy output of massive stars .
Together , these lines of evidence suggest that the true SFR calibration factors can not be too far from their canonical values .