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Relative Rates of Core Collapse SNe. Sample Type SECM08 LWVetal07 VLF05 PSB08 CET99 II-P 58.7 ± 8.0% 67.6 ± 10% 62.9 ± 4.7% 75.59±9.8% 77.7±10.8% II-L 2.7±1.7% IIn 3.8±2.0% 4.4±2.5% 9.2±1.8%

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  1. Relative Rates of Core Collapse SNe Sample Type SECM08 LWVetal07 VLF05 PSB08 CET99 II-P 58.7±8.0% 67.6±10% 62.9±4.7% 75.59±9.8% 77.7±10.8% II-L 2.7±1.7% IIn 3.8±2.0% 4.4±2.5% 9.2±1.8% IIb 5.4±2.7% 1.5±1.5% 3.2±1.0% Ib 9.8±3.3% 26.5±6.2% 24.7±3.0% 24.6±5.6% 22.3±5.8% Ic 19.6±4.5% Sample size 92 68 277 77 67 From Smartt 2009

  2. Location on the HR diagram of progenitors of a) SN2003gd (black point) and SN2005cd (blue shading) and b) SN2008bk. Evolutionary tracks for single stars with the listed masses are shown for the relevant metallicities. Red dots are supergiants in the Milky Way (a) and Large Magellanic Cloud (b). Progenitors of SNII Ps are red supergiants.

  3. Masses or upper limits for progenitors of SNII P • Best estimate of the lower mass limit and upper mass limit for SNII P progenitors.

  4. From Woosley & Janka 2005 Nature Physics 1, 147.

  5. Structure of the progenitor star at the onset of core collapse.

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