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In recent years, many Type IIn supernovae have been found to share strikingsimilarities with the peculiar SN 2009ip, whose true nature is still underdebate. Here, we present 10 years of observations of SN 2011fh, an interactingtransient with spectroscopic and photometric similarities to SN 2009ip. SN2011fh had a M$_r \sim -16$ mag brightening event, followed by a brighter M$_r\sim -18$ mag luminous outburst in August 2011. The spectra of SN 2011fh aredominated by narrow to intermediate Balmer emission lines throughout itsevolution, with P Cygni profiles indicating fast-moving material at $\sim 6400\ \textrm{km s}^{-1}$. HST/WFC3 observations from October of 2016 revealed abright source with M$_{F814W} \approx -13.3$ mag, indicating that we are seeingthe ongoing interaction of the ejecta with the circumstellar material or thatthe star might be going through an eruptive phase five years after the luminousoutburst of 2011. Using HST photometry of the stellar cluster around SN 2011fh,we estimated an age of $\sim 4.5$ Myr for the progenitor, which implies astellar mass of $\sim 60$ M$_\odot$, using single-star evolution models, or amass range of $35 - 80 \ \textrm{M}_\odot$, considering a binary system. Wealso show that the progenitor of SN 2011fh exceeded the classical Eddingtonlimit by a large factor in the months preceding the luminous outburst of 2011,suggesting strong super-Eddington winds as a possible mechanism for theobserved mass-loss. These findings favor an energetic outburst in a young andmassive star, possibly a luminous blue variable.

Unveiling the Nature of SN 2011fh: a Young and Massive Star Gives Rise to a Luminous SN 2009ip-like Event