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

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posted on 2018-04-19, 10:02 authored by 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
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.

Funding

A part of this work is based on observations made with the Southern African Large Telescope (SALT), under the program 2016-1-MLT-010 and 2016-2-LSP-001. EA, DB, PAW, SM, PW gratefully acknowledge the receipt of research grants from the National Research Foundation (NRF) of South Africa. We are grateful to Steve Crawford, Itumeleng Monageng, Daniel Viljoen, and Brent Miszalski for assistance with the SALT observations AK acknowledges the National Research Foundation of South Africa and the Russian Science Foundation (project no.14-50-00043). P.M. is supported by the ”Diamond Grant” No. DI2013/014743 funded by the Polish Ministry of Science and Higher Education. The OGLE project has received funding from the National Science Center, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. KLP, NPMK, APB and JPO acknowledge support from the UK Space Agency. FMW acknowledges support from the US National Science Foundation, grant 1614113. Based in part on observations from the SMARTS Observatory, which is hosted by the Cerro Tololo Inter American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. We thank the SMARTS queue schedulers and observers for their efforts. Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Minist´erio da Ciˆencia, Tecnologia, e Inova¸c˜ao (MCTI) da Rep´ublica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). VARMR acknowledges financial support from FCT in the form of an exploratory project of reference IF/00498/2015, from CIDMA strategic project UID/MAT/04106/2013 and supported by Enabling Green E-science for the Square Kilometer Array Research Infrastructure (ENGAGE SKA),

History

Citation

Monthly Notices of the Royal Astronomical Society, 2018, 474 (2), pp. 2679-2705 (27)

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

  • VoR (Version of Record)

Published in

Monthly Notices of the Royal Astronomical Society

Publisher

Oxford University Press (OUP), Royal Astronomical Society

issn

0035-8711

eissn

1365-2966

Copyright date

2018

Available date

2018-09-08

Publisher version

https://academic.oup.com/mnras/article/474/2/2679/4554400

Language

en