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A Type IIn supernova (SN) is dominated by the interaction of SN ejecta withthe circumstellar medium (CSM). Some SNe IIn (e.g., SN 2006jd) have episodes ofre-brightening ("bumps") in their light curves. We present iPTF13z, a SN IIndiscovered by the intermediate Palomar Transient Factory (iPTF) andcharacterised by several bumps in its light curve. We analyse this peculiarbehaviour trying to infer the properties of the CSM and of the SN explosion, aswell as the nature of its progenitor star. We obtained multi-band opticalphotometry for over 1000 days after discovery with the P48 and P60 telescopesat Palomar Observatory. We obtained low-resolution optical spectra in the sameperiod. We did an archival search for progenitor outbursts. We analyse ourphotometry and spectra, and compare iPTF13z to other SNe IIn. A simpleanalytical model is used to estimate properties of the CSM. iPTF13z was a SNIIn showing a light curve with five bumps during its decline phase. The bumpshad amplitudes between 0.4 and 0.9 mag and durations between 20 and 120 days.The most prominent bumps appeared in all our different optical bands. Thespectra showed typical SN IIn characteristics, with emission lines of H$\alpha$(with broad component FWHM ~$10^{3}-10^{4} ~{\rm ~km ~s^{-1}}$ and narrowcomponent FWHM ~$10^2 \rm ~km ~s^{-1}$) and He I, but also with Fe II, Ca II,Na I D and H$\beta$ P-Cygni profiles (with velocities of ~$10^{3}$ ${\rm ~km~s^{-1}}$). A pre-explosion outburst was identified lasting $\gtrsim 50$ days,with $M_r \approx -15$ mag around 210 days before discovery. Large, variableprogenitor mass-loss rates (~> 0.01 $M_{\odot} \rm ~yr^{-1}$) and CSM densities(~> 10$^{-16}$ g cm$^{-3}$) are derived. We suggest that the light curve bumpsof iPTF13z arose from SN ejecta interacting with denser regions in the CSM,possibly produced by the eruptions of a luminous blue variable star.

The bumpy light curve of supernova iPTF13z