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• 1710.03716v1

Rights statement: This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The definitive publisher-authenticated version E Aydi, K L Page, N P M Kuin, M J Darnley, F M Walter, P Mróz, D A H Buckley, S Mohamed, P Whitelock, P Woudt, S C Williams, M Orio, R E Williams, A P Beardmore, J P Osborne, A Kniazev, V A R M Ribeiro, A Udalski, J Strader, L Chomiuk; Multiwavelength observations of nova SMCN 2016-10a – one of the brightest novae ever observed, Monthly Notices of the Royal Astronomical Society, Volume 474, Issue 2, 21 February 2018, Pages 2679–2705, https://doi.org/10.1093/mnras/stx2678 is available online at: https://academic.oup.com/mnras/article/474/2/2679/4554400

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

Research output: Contribution to journalJournal articlepeer-review

Published
• E. Aydi
• K. L. Page
• N. P. M. Kuin
• M. J. Darnley
• F. M. Walter
• P. Mróz
• D. Buckley
• S. Mohamed
• P. Whitelock
• P. Woudt
• S. C. Williams
• M. Orio
• R. E. Williams
• A. P. Beardmore
• J. P. Osborne
• A. Kniazev
• V. A. R. M. Ribeiro
• A. Udalski
We report on multiwavelength observations of nova SMCN 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 SALT, FLOYDS, and SOAR; long-term OGLE $V$- and $I$- bands photometry dating back to six years before eruption; SMARTS optical and near-IR photometry from $\sim$ 11 days until over 280 days post-eruption; $Swift$ satellite X-ray and ultraviolet observations from $\sim$ 6 days until 319 days post-eruption. The progenitor system contains a bright disk and a main sequence or a sub-giant secondary. The nova is very fast with $t_2 \simeq$ 4.0 $\pm$ 1.0 d and $t_3 \simeq$ 7.8 $\pm$ 2.0 d in the $V$-band. If the nova is in the SMC, at a distance of $\sim$ 61 $\pm$ 10 kpc, we derive $M_{V,\mathrm{max}} \simeq - 10.5$ $\pm$ 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 a FWHM of $\sim$ 3500 kms$^{-1}$ indicating moderately high ejection velocities. The nova entered the nebular phase $\sim$ 20 days post-eruption, predicting the imminent super-soft source turn-on in the X-rays, which started $\sim$ 28 days post-eruption. The super-soft source properties indicate a white dwarf mass between 1.2 M$_{\odot}$ and 1.3 M$_{\odot}$ in good agreement with the optical conclusions.