The unusually luminous extragalactic nova SN 2010U

Ian Czekala; E. Berger; R. Chornock; A. Pastorello; G. H. Marion; R. Margutti; M. T. Botticella; P. Challis; M. Ergon; S. Smartt; J. Sollerman; J. Vinkó; J. C. Wheeler

doi:10.1088/0004-637X/765/1/57

The unusually luminous extragalactic nova SN 2010U

Ian Czekala, E. Berger, R. Chornock, A. Pastorello, G. H. Marion, R. Margutti, M. T. Botticella, P. Challis, M. Ergon, S. Smartt, J. Sollerman, J. Vinkó, J. C. Wheeler

Astronomy & Astrophysics

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Abstract

We present observations of the unusual optical transient SN 2010U, including spectra taken 1.03 days to 15.3 days after maximum light that identify it as a fast and luminous Fe II type nova. Our multi-band light curve traces the fast decline (t ₂ = 3.5 ± 0.3 days) from maximum light (M_V = -10.2 ± 0.1 mag), placing SN 2010U in the top 0.5% of the most luminous novae ever observed. We find typical ejecta velocities of ≈1100 km s^-1 and that SN 2010U shares many spectral and photometric characteristics with two other fast and luminous Fe II type novae, including Nova LMC 1991 and M31N-2007-11d. For the extreme luminosity of this nova, the maximum magnitude versus rate of decline relationship indicates a massive white dwarf (WD) progenitor with a low pre-outburst accretion rate. However, this prediction is in conflict with emerging theories of nova populations, which predict that luminous novae from massive WDs should preferentially exhibit an alternate spectral type (He/N) near maximum light.

Original language	English (US)
Article number	57
Journal	Astrophysical Journal
Volume	765
Issue number	1
DOIs	https://doi.org/10.1088/0004-637X/765/1/57
State	Published - Mar 1 2013

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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title = "The unusually luminous extragalactic nova SN 2010U",

abstract = "We present observations of the unusual optical transient SN 2010U, including spectra taken 1.03 days to 15.3 days after maximum light that identify it as a fast and luminous Fe II type nova. Our multi-band light curve traces the fast decline (t 2 = 3.5 ± 0.3 days) from maximum light (MV = -10.2 ± 0.1 mag), placing SN 2010U in the top 0.5% of the most luminous novae ever observed. We find typical ejecta velocities of ≈1100 km s-1 and that SN 2010U shares many spectral and photometric characteristics with two other fast and luminous Fe II type novae, including Nova LMC 1991 and M31N-2007-11d. For the extreme luminosity of this nova, the maximum magnitude versus rate of decline relationship indicates a massive white dwarf (WD) progenitor with a low pre-outburst accretion rate. However, this prediction is in conflict with emerging theories of nova populations, which predict that luminous novae from massive WDs should preferentially exhibit an alternate spectral type (He/N) near maximum light.",

author = "Ian Czekala and E. Berger and R. Chornock and A. Pastorello and Marion, {G. H.} and R. Margutti and Botticella, {M. T.} and P. Challis and M. Ergon and S. Smartt and J. Sollerman and J. Vink{\'o} and Wheeler, {J. C.}",

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doi = "10.1088/0004-637X/765/1/57",

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T1 - The unusually luminous extragalactic nova SN 2010U

AU - Czekala, Ian

AU - Berger, E.

AU - Chornock, R.

AU - Pastorello, A.

AU - Marion, G. H.

AU - Margutti, R.

AU - Botticella, M. T.

AU - Challis, P.

AU - Ergon, M.

AU - Smartt, S.

AU - Sollerman, J.

AU - Vinkó, J.

AU - Wheeler, J. C.

PY - 2013/3/1

Y1 - 2013/3/1

N2 - We present observations of the unusual optical transient SN 2010U, including spectra taken 1.03 days to 15.3 days after maximum light that identify it as a fast and luminous Fe II type nova. Our multi-band light curve traces the fast decline (t 2 = 3.5 ± 0.3 days) from maximum light (MV = -10.2 ± 0.1 mag), placing SN 2010U in the top 0.5% of the most luminous novae ever observed. We find typical ejecta velocities of ≈1100 km s-1 and that SN 2010U shares many spectral and photometric characteristics with two other fast and luminous Fe II type novae, including Nova LMC 1991 and M31N-2007-11d. For the extreme luminosity of this nova, the maximum magnitude versus rate of decline relationship indicates a massive white dwarf (WD) progenitor with a low pre-outburst accretion rate. However, this prediction is in conflict with emerging theories of nova populations, which predict that luminous novae from massive WDs should preferentially exhibit an alternate spectral type (He/N) near maximum light.

AB - We present observations of the unusual optical transient SN 2010U, including spectra taken 1.03 days to 15.3 days after maximum light that identify it as a fast and luminous Fe II type nova. Our multi-band light curve traces the fast decline (t 2 = 3.5 ± 0.3 days) from maximum light (MV = -10.2 ± 0.1 mag), placing SN 2010U in the top 0.5% of the most luminous novae ever observed. We find typical ejecta velocities of ≈1100 km s-1 and that SN 2010U shares many spectral and photometric characteristics with two other fast and luminous Fe II type novae, including Nova LMC 1991 and M31N-2007-11d. For the extreme luminosity of this nova, the maximum magnitude versus rate of decline relationship indicates a massive white dwarf (WD) progenitor with a low pre-outburst accretion rate. However, this prediction is in conflict with emerging theories of nova populations, which predict that luminous novae from massive WDs should preferentially exhibit an alternate spectral type (He/N) near maximum light.

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The unusually luminous extragalactic nova SN 2010U

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