SN 2005 ap：最辉煌的爆发
SN 2005ap: A Most Brilliant Explosion
摘要：
我们提出了未经过滤的光度观测与ROTSE-III和光学光谱的后续行动与HET和凯克的最明亮的超新星尚未确定，SN 2005 ap。在最大光之前约3天和之后约6天拍摄的光谱显示出窄的发射线（可能起源于矮宿主）和红移z=0.2832的吸收线，这使得峰值未过滤的幅度为-22.7 +/- 0.1绝对值。与H-α、CIII、NIII和OIII相对应的天鹅座P-Cygni的广泛特征，在光球速度约为20，000 km/s的情况下被进一步探测到。与其他高亮度超新星如2006 gy和2006 tf不同，SN 2005 ap的光变曲线显示了一个1-3周的上升到峰值，然后是相对快速的衰减。光谱也缺乏SN 2006 gy和SN 2006 tf中适度加宽（FWHM ~ 2，000 km/s）的巴耳末谱线的明显发射峰。我们简要地讨论了异常亮度的起源从强相互作用，可以预期从一对不稳定爆发或GRB类发动机包裹在一个H/He信封。
英文摘要：
We present unfiltered photometric observations with ROTSE-III and optical spectroscopic follow-up with the HET and Keck of the most luminous supernova yet identified, SN 2005ap. The spectra taken about 3 days before and 6 days after maximum light show narrow emission lines (likely originating in the dwarf host) and absorption lines at a redshift of z=0.2832, which puts the peak unfiltered magnitude at -22.7 +/- 0.1 absolute. Broad P-Cygni features corresponding to H-alpha, CIII, NIII, and OIII, are further detected with a photospheric velocity of ~20,000 km/s. Unlike other highly luminous supernovae such as 2006gy and 2006tf that show slow photometric evolution, the light curve of SN 2005ap indicates a 1-3 week rise to peak followed by a relatively rapid decay. The spectra also lack the distinct emission peaks from moderately broadened (FWHM ~ 2,000 km/s) Balmer lines seen in SN 2006gy and SN 2006tf. We briefly discuss the origin of the extraordinary luminosity from a strong interaction as may be expected from a pair instability eruption or a GRB-like engine encased in a H/He envelope.
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