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The outburst of Nova Sgr 2011 N.2 (=V5588 Sgr) was followed with optical andnear-IR photometric and spectroscopic observations for 3.5 years, beginningshortly before the maximum. V5588 Sgr is located close to Galactic center,suffering from E(B-V)=1.56 (+/-0.1) extinction. The primary maximum was reachedat V=12.37 on UT 2011 April 2.5 (+/-0.2), and the underlying smooth decline wasmoderately fast with t(2,V)=38 and t(3,V)=77 days. On top of an otherwisenormal decline, six self-similar, fast evolving and bright secondary maxima(SdM) appeared in succession. Only very few other novae have presented so clearsecondary maxima. Both the primary maximum and all SdM occurred at later timeswith increasing wavelengths, by amounts in agreement with expectations fromfireball expansions. The radiative energy released during SdM declinedfollowing an exponential pattern, while the breadth of individual SdM and thetime interval between them widened. Emission lines remained sharp (FWHM~1000km/s) throughout the whole nova evolution, with the exception of a broadpedestal with a trapezoidal shape (extending for 3600 km/sec at the top and4500 km/sec at the bottom) which was only seen during the advanced decline fromSdM maxima and was absent in between SdM. V5588 Sgr at maximum light displayeda typical FeII-class spectrum which did not evolve into a nebular stage. About10 days into the decline from primary maximum, a typical high-ionizationHe/N-class spectrum appeared and remained visible simultaneously with theFeII-class spectrum, qualifying V5588 Sgr as a rare "hybrid" nova. While theFeII-class spectrum faded into oblivion, the He/N-class spectrum developedstrong [FeX] coronal lines.

The hybrid, coronal lines nova V5588 Sgr (2011 N.2) and its six repeating secondary maxima