Optical photometry of the rapidly declining Nova Scorpii 2014

ATel #6034; U. Munari (INAF Padova-Asiago), S. Dallaporta, F. Castellani, C. Marangoni (ANS Collaboration)
on 1 Apr 2014; 09:05 UT
Credential Certification: U. Munari (ulisse.munari@oapd.inaf.it)

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Nova Scorpii 2014 was discovered as optical transient TCP J17154683-3128303 by Nishiyama and Kabashima, and classified from optical spectra as a nova by Jelinek et al (ATEL #6025). X-ray emission was detected on Swift observations by Kuulkers et al. (ATEL #6015), which they fitted with an absorbed optically thin emission model, with most of the absorption intrinsic to the source. Joshi et al. (ATel #6032) performed near-IR photometry and spectroscopy, and suggested that Nova Scorpii 2014 could be a nova eruption within a symbiotic binary, similarly to V407 Cyg, RS Oph and V745 Sco.

We are monitoring the photometric evolution of Nova Scorpii 2014 at optical wavelenghts with various telescopes operated by the ANS Collaboration consortium. The same local photometric sequence is adopted for all of them, and it has been extracted from the APASS database and ported to the standard system as defined by the Landolt (2009 AJ 137, 4186) equatorial standards. So far we collected the following data:

The nova is rapidly and smoothly fading, a behaviour already seen in the other novae exploded within a symbiotic binary. The B-V color suggests a large reddening affecting the nova.