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Title: Multiwavelength observations of nova SMCN 2016-10a-one of the brightest novae ever observed
Authors: Aydi, E.
Page, K. L.
Kuin, N. P. M.
Darnley, M. J.
Walter, F. M.
Mróz, P.
Buckley, D. A. H.
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.
First Published: 1-Feb-2018
Publisher: Oxford University Press (OUP), Royal Astronomical Society
Citation: Monthly Notices of the Royal Astronomical Society, 2018, 474 (2), pp. 2679-2705 (27)
Abstract: 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 ∼ 11 days until over 280 days post-eruption; Swift satellite X-ray and ultraviolet observations from ∼ 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 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 a FWHM of ∼ 3500 km s−1 indicating moderately high ejection velocities. The nova entered the nebular phase ∼ 20 days post-eruption, predicting the imminent super-soft source turn-on in the X-rays, which started ∼ 28 days post-eruption. The super-soft source properties indicate a white dwarf mass between 1.2 M and 1.3 M in good agreement with the optical conclusions.
DOI Link: 10.1093/mnras/stx2678
ISSN: 0035-8711
eISSN: 1365-2966
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: Copyright © 2018, Oxford University Press (OUP), Royal Astronomical Society. Deposited with reference to the publisher’s open access archiving policy. (
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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