The 229 GHz (lambda 1.3 mm) radio emission from Orion-KL was mapped with up to 0".4 angular resolution with CARMA, allowing measurements of the flux densities of Source I ("SrcI") and the Becklin-Neugebauer Object (BN), the two most massive stars in this region. We find integrated flux densities of 310 + or - 45 mJy for SrcI and 240 + or - 35 mJy for BN. SrcI is optically thick even at 229 GHz. No trace of the H30 alpha recombination line is seen in its spectrum, although the nu sub(2) = 1, 5(5,0)-6(4,3) transition of H sub(2)O, 3450 K above the ground state, is prominent. SrcI is elongated at position angle 140degrees, as in 43 GHz images. These results are most easily reconciled with models in which the radio emission from SrcI arises via the H- free-free opacity in a T < 4500 K disk, as considered by Reid et al. By contrast, the radio spectrum of BN is consistent with p super(+)/e super(-) free-free emission from a dense (ne ~ 5 x 10 super(7) cm super(-3)), but otherwise conventional, hypercompact H II region. The source is becoming optically thin at 229 GHz, and the H30 alpha recombination line, at V sub(LSR) = 23.2 + or - 0.5 km s super(-1), is prominent in its spectrum. A Lyman continuum flux of 5 x 10 super(45) photons s super(-1), consistent with that expected from a B star, is required to maintain the ionization. Supplementary 90 GHz observations were made to measure the H41 alpha and H42 alpha recombination lines toward BN. Published 43 and 86 GHz data suggest that SrcI brightened with respect to BN over the 15 year period from 1994 to 2009.