SN 2005ap: A MOST BRILLIANT EXPLOSION

摘要

We present unfiltered photometric observations with ROTSE-Ⅲ and optical spectroscopic follow-up with HET and the Keck telescope 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 Hα, C Ⅲ, N Ⅲ, and O Ⅲ are further detected with aphotospheric velocity of ～20,000 km s~(-1). 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 ～2000 km s~(-1)) 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.