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Near-IR spectroscopy is presented for Nova Scorpii 2014. It is shown that theoutburst occurred in a symbiotic binary system - an extremely rareconfiguration for a classical nova outburst to occur in but appropriate for theeruption of a recurrent nova of the T CrB class. We estimate the spectral classof secondary as M5III $\pm$ (two sub-classes). The maximum magnitude versusrate of decline (MMRD) relations give an unacceptably large value of 37.5 kpcfor the distance. The spectra are typical of the He/N class of novae withstrong HeI and H lines. The profiles are broad and flat topped with full widthat zero intensities (FWZIs) approaching 9000-10000 km s$^{-1}$ and also have asharp narrow component superposed which is attributable to emission from thegiant's wind. Hot shocked gas, accompanied by X-rays and $\gamma$ rays, isexpected to form when the high velocity ejecta from the nova plows into thesurrounding giant wind. Although X-ray emission was observed no $\gamma$-rayemission was reported. It is also puzzling that no signature of a deceleratingshock is seen in the near-infrared (NIR), seen in similar systems like RS Oph,V745 Sco and V407 Cyg, as rapid narrowing of the line profiles. The smalloutburst amplitude and the giant secondary strongly suggest that Nova Sco 2014could be a recurrent nova.

Infrared studies of Nova Scorpii 2014: an outburst in a symbiotic system sans an accompanying blast wave