Their argument was based primarily on the fact that the inferred ejecta mass (3.2 [+ or -] 0.5 [M.sub.[dot encircle]]), determined via fitting the Arnett model  to their constructed bolometric LC, was too low for the amount of nickel needed to explain the observed bolometric luminosity (1.0 [+ or -] 0.1 [M.sub.[dot encircle]]).
At late times the decay rate of model (1) provides a much better fit than the [t.sup.-2] decay, which grossly overpredicts the bolometric luminosity at times later than 400 d.
Here [[PHI].sub.bol](L, z) is a bolometric luminosity function (defined for the luminosity L integrated over all wavelengths) and [bar.[eta]] represents an averaged radiation efficiency that is assumed not to depend on z or L in this formula.
(12) The bolometric luminosity function of all AGNs (including Comptonthin and Compton-thick AGNs) is derived from the hard XLF by assuming luminosity-dependent bolometric correction factors and their scatter.