OVRO image created by averaging ﹩10^{\prime \prime }\times 10^{\prime \prime }﹩ images toward the positions of known low‐mass K‐band cluster members in NGC 2024. The bright sources listed in Table 1 were removed using CLEAN before shifting and co‐adding the images. The contour increment is given by the standard deviation of the mean for the flux distribution (0.06 mJy; § 4). Negative contours are represented by dotted lines, and positive contours are represented by solid lines. The FWHM of the emission, as well as the negative features, are consistent with the OVRO beam shown in Fig. 3c. We also note that the emission is centered at (0, 0), corresponding to the mean position of K‐band sources. None of the individual stars used to create this image were detected at the ≥3 σ level, although the sources are detected in the mean at the ~5 σ level. Assuming this compact emission originates from circumstellar disks, the average disk mass for the ensemble of K‐band sources is ~0.005 M_⊙.