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

Abstract We report on multiwavelength observations of nova Small Magellanic Cloud Nova 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 So...

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Veröffentlicht in:Monthly notices of the Royal Astronomical Society 2018-02, Vol.474 (2), p.2679-2705
Hauptverfasser: 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
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container_issue 2
container_start_page 2679
container_title Monthly notices of the Royal Astronomical Society
container_volume 474
creator 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
description Abstract We report on multiwavelength observations of nova Small Magellanic Cloud Nova 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 Southern African Large Telescope, Folded Low-Order Yte-Pupil Double-Dispersed Spectrograph, and Southern Astrophysical Research; long-term Optical Gravitational Lensing Experiment V- and I-bands photometry dating back to 6 yr before eruption; Small and Moderate Aperture Research Telescope System optical and near-IR photometry from ∼11 d until over 280 d post-eruption; Swift satellite X-ray and ultraviolet observations from ∼6 d until 319 d post-eruption. The progenitor system contains a bright disc 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 an Full Width at Half Maximum of ∼3500 km s−1, indicating moderately high ejection velocities. The nova entered the nebular phase ∼20 d post-eruption, predicting the imminent super-soft source turn-on in the X-rays, which started ∼28 d post-eruption. The super-soft source properties indicate a white dwarf mass between 1.2  and 1.3 M⊙ in good agreement with the optical conclusions.
doi_str_mv 10.1093/mnras/stx2678
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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 Southern African Large Telescope, Folded Low-Order Yte-Pupil Double-Dispersed Spectrograph, and Southern Astrophysical Research; long-term Optical Gravitational Lensing Experiment V- and I-bands photometry dating back to 6 yr before eruption; Small and Moderate Aperture Research Telescope System optical and near-IR photometry from ∼11 d until over 280 d post-eruption; Swift satellite X-ray and ultraviolet observations from ∼6 d until 319 d post-eruption. The progenitor system contains a bright disc 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 an Full Width at Half Maximum of ∼3500 km s−1, indicating moderately high ejection velocities. The nova entered the nebular phase ∼20 d post-eruption, predicting the imminent super-soft source turn-on in the X-rays, which started ∼28 d post-eruption. 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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 an Full Width at Half Maximum of ∼3500 km s−1, indicating moderately high ejection velocities. The nova entered the nebular phase ∼20 d post-eruption, predicting the imminent super-soft source turn-on in the X-rays, which started ∼28 d post-eruption. The super-soft source properties indicate a white dwarf mass between 1.2  and 1.3 M⊙ in good agreement with the optical conclusions.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stx2678</doi><tpages>27</tpages><orcidid>https://orcid.org/0000-0001-8178-0202</orcidid><orcidid>https://orcid.org/0000-0003-0156-3377</orcidid><orcidid>https://orcid.org/0000-0002-4678-4432</orcidid><oa>free_for_read</oa></addata></record>
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subjects Ejection
Eruptions
Gravitational lenses
Line spectra
Magellanic clouds
Nebulae
Photometry
Satellite observation
White dwarf stars
title Multiwavelength observations of nova SMCN 2016-10a – one of the brightest novae ever observed
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