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Spectral Features of KT Eri in its Nebular Phase

Published online by Cambridge University Press:  17 January 2013

Akira Arai ,
Mizuki Isoggai ,
Kazuyoshi Imamura ,
Yuji Ikeda ,
Takayuki Arasaki ,
Eiji Kitao  and
Gaku Taguchi
Akira Arai
Affiliation:
Koyama Astronomical Observatory, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, Japan, 603-8555 email: arai6a@cc.kyoto-su.ac.jp
Mizuki Isoggai
Affiliation:
Koyama Astronomical Observatory, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, Japan, 603-8555 email: arai6a@cc.kyoto-su.ac.jp
Kazuyoshi Imamura
Affiliation:
Department of Biosphere-Geosphere System Science, Faculty of Informatics, Okayama University of Science, 1-1 Ridai-cho, Okayama, Okayama, Japan, 700-0005
Yuji Ikeda
Affiliation:
Department of Physics, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, Japan, 603-8555
Takayuki Arasaki
Affiliation:
Department of Physics, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, Japan, 603-8555
Eiji Kitao
Affiliation:
Department of Physics, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, Japan, 603-8555
Gaku Taguchi
Affiliation:
Department of Physics, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, Japan, 603-8555
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Abstract

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Non-spherically symmetric distributions of ejected gas are often observed in classical nova remnants. However, it is unclear if these asymmetries could be produced from nova explosions. Spectra in the nebular phase can provide information on the kinematics of ejected materials. Classical nova KT Eri was discovered on November 2009. It is considered a candidate for a recurrent nova based on the high expansion velocity and rapid decline of its light curve. In order to investigate the velocity field of ejected gas in the system, we performed optical spectroscopic observations from 2010 September to 2010 December at Koyama Astronomical Observatory. We noticed the strong [O III] and He II lines in the spectra on September 1, which suggests that the nova had already entered the nebular phase. It is notable that the [O III] lines showed complex profiles with at least six peaks on September 1. Those features can be de-convolved into four velocity components (−2,000 km s−1, −1,000 km s−1, +700 km s−1, and +1,800 km s−1) of doublet [O III] λ4959 and λ5007.

Keywords

stars: novaecataclysmic variables — techniques: spectroscopic
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 119 - 120
Copyright
Copyright © International Astronomical Union 2013

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