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In this paper we analyse the pre-explosion spectrum of SN2015bh by performingradiative transfer simulations using the CMFGEN code. This object has attractedsignificant attention due to its remarkable similarity to SN2009ip in both itspre- and post-explosion behaviour. They seem to belong to a class of events forwhich the fate as a genuine core-collapse supernova or a non-terminal explosionis still under debate. Our CMFGEN models suggest that the progenitor ofSN2015bh had an effective temperature between 8700 and 10000 K, luminosity inthe range ~ 1.8-4.74e6 Lsun, contained at least 25% H in mass at the surface,and half-solar Fe abundances. The results also show that the progenitor of SN2015bh generated an extended wind with a mass-loss rate of ~ 6e-4 to 1.5e-3Msun/yr and a velocity of 1000 km/s. We determined that the wind extended to atleast 2.57e14 cm and lasted for at least 30 days prior to the observations,releasing 5e-5 Msun into the circumstellar medium. In analogy to 2009ip, wepropose that this is the material that the explosive ejecta could interact atlate epochs, perhaps producing observable signatures that can be probed withfuture observations. We conclude that the progenitor of SN 2015bh was mostlikely a warm luminous blue variable of at least 35 Msun before the explosion.Considering the high wind velocity, we cannot exclude the possibility that theprogenitor was a Wolf-Rayet star that inflated just before the 2013 eruption,similar to HD5980 during its 1994 episode. If the star survived, late-timespectroscopy may reveal either a similar LBV or a Wolf-Rayet star, depending onthe mass of the H envelope before the explosion. If the star exploded as agenuine SN, 2015bh would be a remarkable case of a successful explosion afterblack-hole formation in a star with a possible minimum mass 35 Msun at thepre-SN stage.

Catching a star before explosion: the luminous blue variable progenitor of SN 2015bh