We present 7 spectroscopically confirmed Type II cluster supernovae ( SNe II ) discovered in the Multi-Epoch Nearby Cluster Survey , a supernova survey targeting 57 low redshift 0.05 < z < 0.15 galaxy clusters with the Canada-France-Hawaii Telescope .
We find the rate of Type II supernovae within R _ { 200 } of z \sim 0.1 galaxy clusters to be 0.026 _ { -0.018 } ^ { +0.085 } ( stat ) _ { -0.001 } ^ { +0.003 } ( sys ) SNuM .
Surprisingly , one SN II is in a red sequence host galaxy that shows no clear evidence of recent star formation .
This is unambiguous evidence in support of ongoing , low-level star formation in at least some cluster elliptical galaxies , and illustrates that galaxies that appear to be quiescent can not be assumed to host only Type Ia SNe .
Based on this single SN II we make the first measurement of the SN II rate in red sequence galaxies , and find it to be 0.007 _ { -0.007 } ^ { +0.014 } ( stat ) _ { -0.001 } ^ { +0.009 } ( sys ) SNuM .
We also make the first derivation of cluster specific star formation rates ( sSFR ) from cluster SN II rates .
We find that for all galaxy types , the sSFR is 5.1 _ { -3.1 } ^ { +15.8 } ( stat ) \pm 0.9 ( sys ) M _ { \odot } yr ^ { -1 } ( 10 ^ { 12 } M _ { \odot } ) ^ { -1 } , and for red sequence galaxies only , it is 2.0 _ { -0.9 } ^ { +4.2 } ( stat ) \pm 0.4 ( sys ) M _ { \odot } yr ^ { -1 } ( 10 ^ { 12 } M _ { \odot } ) ^ { -1 } .
These values agree with SFRs measured from infrared and ultraviolet photometry , and H \alpha emission from optical spectroscopy .
Additionally , we use the SFR derived from our SNII rate to show that although a small fraction of cluster Type Ia SNe may originate in the young stellar population and experience a short delay time , these results do not preclude the use of cluster SN Ia rates to derive the late-time delay time distribution for SNe Ia .