Multiwavelength observations of nova SMCN 2016-10a - one of the brightest novae ever observed

• Autor(a) principal: Aydi, E.
• Data de Publicação: 2018
• Outros Autores: Page, K. L., Kuin, N. P. M., Darnley, M. J., Walter, F. M., Mróz, P., Buckley, D., Mohamed, S., Whitelock, P., Woudt, P., Williams, S. C., Orio, M., Williams, R. E., Beardmore, A. P., Osborne, J. P., Kniazev, A., Ribeiro, V. A. R. M., Udalski, A., Strader, J., Chomiuk, L.
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)
• Texto Completo: http://hdl.handle.net/10773/21416
• topic: stars: individual (SMCN 2016-10a); novae, cataclysmic variables; white dwarfs; ultraviolet: stars; X-rays: binaries

We report on multiwavelength observations of nova Small Magellanic Cloud Nova 2016-10a. The present observational set is one of the most comprehensive for any nova in the Small Magellanic Cloud, including low-, medium-, and high-resolution optical spectroscopy and spectropolarimetry from Southern African Large Telescope, Folded Low-Order Yte-Pupil Double-Dispersed Spectrograph, and Southern Astrophysical Research; long-term Optical Gravitational Lensing Experiment V- and I-bands photometry dating back to 6 yr before eruption; Small and Moderate Aperture Research Telescope System optical and near-IR photometry from ˜11 d until over 280 d post-eruption; Swift satellite X-ray and ultraviolet observations from ˜6 d until 319 d post-eruption. The progenitor system contains a bright disc and a main sequence or a sub-giant secondary. The nova is very fast with t2 ≃ 4.0 ± 1.0 d and t3 ≃ 7.8 ± 2.0 d in the V band. If the nova is in the SMC, at a distance of ˜61 ± 10 kpc, we derive MV, max ≃ -10.5 ± 0.5, making it the brightest nova ever discovered in the SMC and one of the brightest on record. At day 5 post-eruption the spectral lines show a He/N spectroscopic class and an Full Width at Half Maximum of ˜3500 km s-1, indicating moderately high ejection velocities. The nova entered the nebular phase ˜20 d post-eruption, predicting the imminent super-soft source turn-on in the X-rays, which started ˜28 d post-eruption. The super-soft source properties indicate a white dwarf mass between 1.2 and 1.3 M in good agreement with the optical conclusions.