Notes. ^(a)Object names from MBS07. ^(b)Coordinates corrected using Spitzer images overlaid with SMA contours and ellipses defined by FWHMa from MBS07. ^(c)Heliocentric distances and uncertainties are from Rygl et al. (2012) and references therein unless otherwise noted. ^(d)Projected from Cyg OB2 calculated using D_⊙. ^(e)Number of core components visible in SMA images (868 μm, 0′′.7 resolution). A plus (+) indicates that weak and/or filamentary emission suggest there may be additional fragments. ^(f)Maximum 868 μm flux density among all core fragments. (^*Peak flux density of N54 measured from image centred on N54.) ^(g)Rygl et al. (2012) did not explicitly measure the parallaxes at the locations of these sources, so we adopted the average and uncertainty over Cygnus X. ^(h)SEDs could not be reconstructed for these sources. See text for details. ⁽ⁱ⁾The distance to S8 is poorly constrained; the given uncertainties reflect the full range of distance estimates in the literature (see review by Varricatt et al. 2010, appendix A37), and the smallest possible projected distance can by calculated by assuming both S8 and Cyg OB2 are at the latter’s minimum distance from us (~ 1.3 kpc). ^(j)The projected distance between S26 and Cyg OB2 is negligible compared to their line-of-sight separation, ≳ 1.57 kpc.