DR. VISHAL JOSHI

Near-IR spectroscopy of for Nova Scorpii 2014 infers that the outburst occurred in a symbiotic binary system - an extremely rare configuration for a classical nova outburst to occur in but appropriate for the eruption of a recurrent nova of the T CrB class. We estimate the spectral class of secondary as M5 (± one sub-class) and located at a distance of 9.5 ± 3.3 kpc in the direction of the galactic bulge. The spectra are typical of the He/N class of novae with strong HeI and H lines. The profiles are broad and flat topped with full width at zero intensities (FWZIs) approaching 9000-10000 km/s and also have a sharp narrow component superposed which is attributable to emission from the giant’s wind. Hot shocked gas, accompanied by X-rays and ¿ rays, is expected to form when the high velocity ejecta from the nova plows into the surrounding giant wind. Although X-ray emission was observed no ¿ ray emission was reported. It is also puzzling that no signature of a decelerating shock 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 small outburst amplitude and the giant secondary strongly suggest that Nova Sco 2014 could be a recurrent nova.