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
Accepted author manuscript, 4.31 MB, PDF document
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Research output: Contribution to Journal/Magazine › Journal article › peer-review
Research output: Contribution to Journal/Magazine › Journal article › peer-review
}
TY - JOUR
T1 - Multiwavelength observations of nova SMCN 2016-10a -- one of the brightest novae ever observed
AU - Aydi, E.
AU - Page, K. L.
AU - Kuin, N. P. M.
AU - Darnley, M. J.
AU - Walter, F. M.
AU - Mróz, P.
AU - Buckley, D.
AU - Mohamed, S.
AU - Whitelock, P.
AU - Woudt, P.
AU - Williams, S. C.
AU - Orio, M.
AU - Williams, R. E.
AU - Beardmore, A. P.
AU - Osborne, J. P.
AU - Kniazev, A.
AU - Ribeiro, V. A. R. M.
AU - Udalski, A.
AU - Strader, J.
AU - Chomiuk, L.
N1 - 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
PY - 2018/2/21
Y1 - 2018/2/21
N2 - 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.
AB - 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.
KW - astro-ph.SR
U2 - 10.1093/mnras/stx2678
DO - 10.1093/mnras/stx2678
M3 - Journal article
VL - 474
SP - 2679
EP - 2705
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -