A modified Baker-Nunn camera was used to conduct a wide-field survey of 1428 deg ^ { 2 } of sky near the ecliptic in search of bright Kuiper Belt objects and Centaurs .
This area is an order of magnitude larger than any previously published CCD survey for Centaurs and Kuiper Belt Objects .
No new objects brighter than red magnitude m _ { R } = 18.8 and moving at a rate 1 \arcsec hr ^ { -1 } to 20 \arcsec hr ^ { -1 } were discovered , although one previously discovered Centaur 1997 CU26 Chariklo was serendipitously detected .
The parameters of the survey were characterized using both visual and automated techniques .
From this survey the empirical projected surface density of Centaurs was found to be \Sigma _ { C } ( m _ { R } \leq 18.8 ) = 7.8 ( ^ { +16.0 } _ { -6.6 } ) \times 10 ^ { -4 } \mbox { deg } ^ { -2 } and we found a projected surface density 3 \sigma upper confidence limit for Kuiper Belt objects of \Sigma _ { K } ( m _ { R } \leq 18.8 ) < 4.1 \times 10 ^ { -3 } \mbox { deg } ^ { -2 } .
We discuss the current state of the cumulative luminosity functions of both Centaurs and Kuiper Belt objects .
Through a Monte Carlo simulation we show that the size distribution of Centaurs is consistent with a q \sim 4 differential power law , similar to the size distribution of the parent Kuiper Belt Objects .
The Centaur population is of order 1 \times 10 ^ { 7 } ( radius \geq 1 km ) assuming a geometric albedo of 0.04 .
About 100 Centaurs are larger than 50 km in radius , of which only 4 are presently known .
The current total mass of the Centaurs is 10 ^ { -4 } M _ { \oplus } .
No dust clouds were detected resulting from Kuiper Belt object collisions , placing a 3 \sigma upper limit < 600 collisionally produced clouds of m _ { R } < 18.8 per year .