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We have measured the correlation between the locations of core-collapsesupernovae (CCSNe) and host galaxy light in the Ha line, near ultraviolet(NUV), R-band and Ks-band to constrain the progenitors of CCSNe using pixelstatistics. Our sample consists of 86 CCSNe in 57 infrared (IR)-brightgalaxies, of which many are starbursts and ten are luminous infrared galaxies(LIRGs). We also analyse the radial distribution of CCSNe in these galaxies,and determine power-law and exponential fits to CCSN surface density profiles.To probe differences between the SNe of these galaxies and normal spiralgalaxies, our results were compared to previous studies with samples dominatedby normal spiral galaxies where possible. We obtained a normalised scale lengthof 0.23^{+0.03}_{-0.02} R_25 for the CCSN surface density in IR-brightgalaxies; less than that derived for CCSNe in a sample dominated by normalspiral galaxies (0.29 \pm 0.01). This reflects a more centrally concentratedpopulation of massive stars in IR-bright galaxies. Furthermore, thiscentralisation is dominated by a central excess of type Ibc/IIb SNe. This maybe due to a top-heavy initial mass function and/or an enhanced close binaryfraction in regions of enhanced star formation. Type Ic SNe are most stronglycorrelated with Ha light and NUV-bright regions, reflecting the shortestlifetime and thus highest mass for type Ic progenitors. Previous studies withsamples dominated by normal spiral galaxies have indicated a lower Ibc-Hacorrelation than our results do, which may be due to the central excess of typeIbc/IIb SNe in our sample. The difference between types II and Ib is minimal,suggesting that progenitor mass is not the dominant factor in determining if aSN is of type Ib or II. Similar differences in correlation can be seen in theKs-band, with type Ibc/IIb SNe tracing the Ks-band light better than type II inour sample.

Spatial distributions of core-collapse supernovae in infrared-bright galaxies