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We study SN 2006oz, a newly-recognized member of the class of H-poor,super-luminous supernovae. We present multi-color light curves from the SDSS-IISN Survey, that cover the rise time, as well as an optical spectrum that showsthat the explosion occurred at z~0.376. We fitted black body functions toestimate the temperature and radius evolution of the photosphere and used theparametrized code SYNOW to model the spectrum. We constructed a bolometriclight curve and compared it with explosion models. The very early light curvesshow a dip in the g- and r-bands and a possible initial cooling phase in theu-band before rising to maximum light. The bolometric light curve shows aprecursor plateau with a duration of 6-10 days in the rest-frame. A lower limitof M_u < -21.5 can be placed on the absolute peak luminosity of the SN, whilethe rise time is constrained to be at least 29 days. During our observations,the emitting sphere doubled its radius to 2x10^15 cm, while the temperatureremained hot at 15000 K. As for other similar SNe, the spectrum is best modeledwith elements including O II and Mg II, while we tentatively suggest that FeIII might be present. We suggest that the precursor plateau might be related toa recombination wave in a circumstellar medium (CSM) and discuss whether thisis a common property of all similar explosions. The subsequent rise can beequally well described by input from a magnetar or by ejecta-CSM interaction,but the models are not well constrained owing to the lack of post-maximumobservations, and CSM interaction has difficulties accounting for the precursorplateau self-consistently. Radioactive decay is less likely to be the mechanismthat powers the luminosity. The host galaxy, detected in deep imaging with the10 m GTC, is a moderately young and star-forming, but not a starburst, galaxy.It has an absolute magnitude of M_g = -16.9.

SN 2006oz: rise of a super-luminous supernova observed by the SDSS-II SN Survey