SN 2006gy: An Extremely Luminous Supernova in the Galaxy NGC 1260
SN 2006gy: An Extremely Luminous Supernova in the Galaxy NGC 1260
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DOI：
10.1086/516749
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发表时间：
2006-12
期刊：
影响因子：
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通讯作者：
E. Ofek;P. B. Cameron;M. Kasliwal;A. Gal-yam;A. Rau;S. Kulkarni;D. Frail;P. Chandra;P. Chandra;S. Cenko;A. Soderberg;S. Immler
中科院分区：
文献类型：
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作者：
E. Ofek;P. B. Cameron;M. Kasliwal;A. Gal-yam;A. Rau;S. Kulkarni;D. Frail;P. Chandra;P. Chandra;S. Cenko;A. Soderberg;S. Immler
超新星SN 2006 gy的V波段峰值绝对星等约为-22等，可能是有史以来观测到的最亮的超新星。我们报告这个SN和它的环境的多波长观测。我们的光谱显示Hα发射线以及吸收功能，可以确定为硅II线在低膨胀速度。缓慢的增亮、峰值亮度和Hα发射线类似于在混合型IIn/Ia SNe（也称为IIa型）中观察到的，可能表明SN 2006 gy与IIa型SNe有关。主星系NGC 1260由一个具有太阳金属丰度的古老恒星群主导。然而，我们的高分辨率自适应光学图像揭示了这个星系中的尘埃带，并且在SN附近似乎有一个H II区域。异常大的峰值光度，约3 × 1044尔格·秒-1，需要一个致密的星周介质，而不管祖星星的质量。推断的质量损失率的祖先是~0.1百万分之一的一段时间内~10年前爆炸。如此高的质量损失率可能是双星星星共同包层抛射的结果。前两个月的总辐射能量约为1.1 × 1051尔格，仅比超克拉塞卡Ia型爆炸小2倍。因此，考虑到SN附近存在一个恒星形成区和高能量需求，一个合理的假设是SN 2006 gy与一颗大质量星星的死亡有关。
With an extinction-corrected V-band peak absolute magnitude of about -22, supernova SN 2006gy is probably the brightest SN ever observed. We report on multiwavelength observations of this SN and its environment. Our spectroscopy shows an Hα emission line as well as absorption features that may be identified as Si II lines at low expansion velocity. The slow brightening, the peak luminosity, and the Hα emission line resemble those observed in hybrid Type IIn/Ia SNe (also known as Type IIa) and may suggest that SN 2006gy is related to the Type IIa SNe class. The host galaxy, NGC 1260, is dominated by an old stellar population with solar metallicity. However, our high-resolution adaptive optics images reveal a dust lane in this galaxy, and there appears to be an H II region in the vicinity of the SN. The extraordinarily large peak luminosity, ~3 × 1044 ergs s-1, demands a dense circumstellar medium, regardless of the mass of the progenitor star. The inferred mass-loss rate of the progenitor is ~0.1 M☉ yr-1 over a period of ~10 yr prior to explosion. Such an high mass-loss rate may be the result of a binary star common envelope ejection. The total radiated energy in the first 2 months is about 1.1 × 1051 ergs, which is only a factor of 2 less than that available from a super-Chandrasekhar Type Ia explosion. Therefore, given the presence of a star-forming region in the vicinity of the SN and the high-energy requirements, a plausible scenario is that SN 2006gy is related to the death of a massive star.