  We present results from a fully relativistic investigation of matter fallback
in a supernova, assuming that the central compact star is a black hole (BH).
Our goal is to answer the following questions: can we infer from the light
curve whether a stellar black hole (BH) has formed in the aftermath of a
supernova explosion ? Did SN1897A produce a BH and, if so, when will the hole
become detectable ? We show that it should not be possible to infer the
presence of a BH in the remnant for another several hundred to a thousand
years. In the case of SN1987A, we estimate the BH luminosity to be $L\simeq
5\times 10^{34}$ erg s$^{-1}$, which is well below the present day bolometric
luminosity of the remnant ($\sim 10^{36}erg/s$; Suntzeff 1997).
