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