THE INTERMEDIATE LUMINOSITY OPTICAL TRANSIENT SN 2010DA: The PROGENITOR, ERUPTION, and AFTERMATH of A PECULIAR SUPERGIANT HIGH-MASS X-RAY BINARY

V. A. Villar; E. Berger; R. Chornock; R. Margutti; T. Laskar; P. J. Brown; P. K. Blanchard; I. Czekala; R. Lunnan; M. T. Reynolds

doi:10.3847/0004-637X/830/1/11

THE INTERMEDIATE LUMINOSITY OPTICAL TRANSIENT SN 2010DA: The PROGENITOR, ERUPTION, and AFTERMATH of A PECULIAR SUPERGIANT HIGH-MASS X-RAY BINARY

V. A. Villar, E. Berger, R. Chornock, R. Margutti, T. Laskar, P. J. Brown, P. K. Blanchard, I. Czekala, R. Lunnan, M. T. Reynolds

Physics and Astronomy

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31 Scopus citations

Abstract

We present optical spectroscopy, ultraviolet-to-infrared imaging, and X-ray observations of the intermediate luminosity optical transient (ILOT) SN 2010da in NGC 300 (d = 1.86 Mpc) spanning from -6 to +6 years relative to the time of outburst in 2010. Based on the light-curve and multi-epoch spectral energy distributions of SN 2010da, we conclude that the progenitor of SN 2010da is a ≈10-12 M _o yellow supergiant possibly transitioning into a blue-loop phase. During outburst, SN 2010da had a peak absolute magnitude of M _bol ≲ -10.4 mag, dimmer than other ILOTs and supernova impostors. We detect multi-component hydrogen Balmer, Paschen, and Ca ii emission lines in our high-resolution spectra, which indicate a dusty and complex circumstellar environment. Since the 2010 eruption, the star has brightened by a factor of ≈5 and remains highly variable in the optical. Furthermore, we detect SN 2010da in archival Swift and Chandra observations as an ultraluminous X-ray source (L _X ≈ 6 10³⁹ erg s^-1). We additionally attribute He ii 4686 Å and coronal Fe emission lines in addition to a steady X-ray luminosity of ≈10³⁷ erg s^-1 to the presence of a compact companion.

Original language	English (US)
Article number	11
Journal	Astrophysical Journal
Volume	830
Issue number	1
DOIs	https://doi.org/10.3847/0004-637X/830/1/11
State	Published - Oct 10 2016

Funding

This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. Additionally, the scientific results reported in this article are based in part on data obtained from the Chandra Data Archive. V.A.V. and P.K.B. acknowledge support from the National Science Foundation through a Graduate Research Fellowship under Grant No. DGE1144152.

Keywords

X-rays: binaries
stars: mass-loss
supernovae: individual (SN 2010da)

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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Villar, V. A., Berger, E., Chornock, R., Margutti, R., Laskar, T., Brown, P. J., Blanchard, P. K., Czekala, I., Lunnan, R., & Reynolds, M. T. (2016). THE INTERMEDIATE LUMINOSITY OPTICAL TRANSIENT SN 2010DA: The PROGENITOR, ERUPTION, and AFTERMATH of A PECULIAR SUPERGIANT HIGH-MASS X-RAY BINARY. Astrophysical Journal, 830(1), Article 11. https://doi.org/10.3847/0004-637X/830/1/11

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title = "THE INTERMEDIATE LUMINOSITY OPTICAL TRANSIENT SN 2010DA: The PROGENITOR, ERUPTION, and AFTERMATH of A PECULIAR SUPERGIANT HIGH-MASS X-RAY BINARY",

abstract = "We present optical spectroscopy, ultraviolet-to-infrared imaging, and X-ray observations of the intermediate luminosity optical transient (ILOT) SN 2010da in NGC 300 (d = 1.86 Mpc) spanning from -6 to +6 years relative to the time of outburst in 2010. Based on the light-curve and multi-epoch spectral energy distributions of SN 2010da, we conclude that the progenitor of SN 2010da is a ≈10-12 M o yellow supergiant possibly transitioning into a blue-loop phase. During outburst, SN 2010da had a peak absolute magnitude of M bol ≲ -10.4 mag, dimmer than other ILOTs and supernova impostors. We detect multi-component hydrogen Balmer, Paschen, and Ca ii emission lines in our high-resolution spectra, which indicate a dusty and complex circumstellar environment. Since the 2010 eruption, the star has brightened by a factor of ≈5 and remains highly variable in the optical. Furthermore, we detect SN 2010da in archival Swift and Chandra observations as an ultraluminous X-ray source (L X ≈ 6 1039 erg s-1). We additionally attribute He ii 4686 {\AA} and coronal Fe emission lines in addition to a steady X-ray luminosity of ≈1037 erg s-1 to the presence of a compact companion.",

keywords = "X-rays: binaries, stars: mass-loss, supernovae: individual (SN 2010da)",

author = "Villar, {V. A.} and E. Berger and R. Chornock and R. Margutti and T. Laskar and Brown, {P. J.} and Blanchard, {P. K.} and I. Czekala and R. Lunnan and Reynolds, {M. T.}",

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T2 - The PROGENITOR, ERUPTION, and AFTERMATH of A PECULIAR SUPERGIANT HIGH-MASS X-RAY BINARY

AU - Villar, V. A.

AU - Berger, E.

AU - Chornock, R.

AU - Margutti, R.

AU - Laskar, T.

AU - Brown, P. J.

AU - Blanchard, P. K.

AU - Czekala, I.

AU - Lunnan, R.

AU - Reynolds, M. T.

PY - 2016/10/10

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N2 - We present optical spectroscopy, ultraviolet-to-infrared imaging, and X-ray observations of the intermediate luminosity optical transient (ILOT) SN 2010da in NGC 300 (d = 1.86 Mpc) spanning from -6 to +6 years relative to the time of outburst in 2010. Based on the light-curve and multi-epoch spectral energy distributions of SN 2010da, we conclude that the progenitor of SN 2010da is a ≈10-12 M o yellow supergiant possibly transitioning into a blue-loop phase. During outburst, SN 2010da had a peak absolute magnitude of M bol ≲ -10.4 mag, dimmer than other ILOTs and supernova impostors. We detect multi-component hydrogen Balmer, Paschen, and Ca ii emission lines in our high-resolution spectra, which indicate a dusty and complex circumstellar environment. Since the 2010 eruption, the star has brightened by a factor of ≈5 and remains highly variable in the optical. Furthermore, we detect SN 2010da in archival Swift and Chandra observations as an ultraluminous X-ray source (L X ≈ 6 1039 erg s-1). We additionally attribute He ii 4686 Å and coronal Fe emission lines in addition to a steady X-ray luminosity of ≈1037 erg s-1 to the presence of a compact companion.

AB - We present optical spectroscopy, ultraviolet-to-infrared imaging, and X-ray observations of the intermediate luminosity optical transient (ILOT) SN 2010da in NGC 300 (d = 1.86 Mpc) spanning from -6 to +6 years relative to the time of outburst in 2010. Based on the light-curve and multi-epoch spectral energy distributions of SN 2010da, we conclude that the progenitor of SN 2010da is a ≈10-12 M o yellow supergiant possibly transitioning into a blue-loop phase. During outburst, SN 2010da had a peak absolute magnitude of M bol ≲ -10.4 mag, dimmer than other ILOTs and supernova impostors. We detect multi-component hydrogen Balmer, Paschen, and Ca ii emission lines in our high-resolution spectra, which indicate a dusty and complex circumstellar environment. Since the 2010 eruption, the star has brightened by a factor of ≈5 and remains highly variable in the optical. Furthermore, we detect SN 2010da in archival Swift and Chandra observations as an ultraluminous X-ray source (L X ≈ 6 1039 erg s-1). We additionally attribute He ii 4686 Å and coronal Fe emission lines in addition to a steady X-ray luminosity of ≈1037 erg s-1 to the presence of a compact companion.

KW - X-rays: binaries

KW - stars: mass-loss

KW - supernovae: individual (SN 2010da)

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THE INTERMEDIATE LUMINOSITY OPTICAL TRANSIENT SN 2010DA: The PROGENITOR, ERUPTION, and AFTERMATH of A PECULIAR SUPERGIANT HIGH-MASS X-RAY BINARY

Abstract

Funding

Keywords

ASJC Scopus subject areas

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