Binary Stars in the Orion Trapezium Cluster Core

We have obtained high angular resolution (013 FWHM) near-infrared images of the central ~40'' × 40'' of the Trapezium cluster, using a speckle holography technique that we describe in detail. A search for close binary systems was made in K_s (2.16 μm) and H (1.65 μm) mosaic images, in which 45 and 35 stars were detected, respectively. The sensitivity limits for stellar detections are K_s ≃ 14.8 and H ≃ 14.9 over the whole mosaics and K_s ≃ 16.0 and H ≃ 15.9 for those regions of the mosaics where most data were accumulated, thus potentially including objects with substellar masses down to ~0.04 M_☉. In total, four binary systems were identified with projected linear separations in the range of 014-05 (63-225 AU). The resulting binary fraction for low-mass pre-main-sequence stars is 5.9% ± 4.0%. This fraction agrees well with the binary frequency observed for main-sequence field stars, but is lower by a factor of ~3 than the fraction found from observations of young stars in Taurus-Auriga over the same range of separations. The difference in binary frequency between the core of the Trapezium cluster and the low-mass, low stellar density dark cloud Taurus-Auriga is established at a statistical significance level of 96% and suggests that binary frequencies are affected by the local star-forming environment. We show that the massive Trapezium star θ¹ Ori A has a nearby companion separated by ~02 (~90 AU). The location of this companion is coincident, within the positional uncertainties, with a nonthermal and variable VLA radio source, which was previously associated with θ¹ Ori A itself. We give H photometry for 32 stars, K_s photometry for 43 stars, and present a color-magnitude diagram for the Trapezium core.