Despite more than 30 years of searches, the compact object in Supernova (SN) 1987A has not yet been detected. We present new limits on the compact object in SN 1987A using millimeter, near-infrared, optical, ultraviolet, and X-ray observations from ALMA, VLT, HST, and Chandra. The limits are approximately 0.1 mJy (0.1×10 −26 erg s −1 cm −2 Hz −1 ) at 213 GHz, 1 L (6×10 −29 erg s −1 cm −2 Hz −1 ) in optical if our line-of-sight is free of ejecta dust, and 10 36 erg s −1 (2 × 10 −30 erg s −1 cm −2 Hz −1 ) in 2-10 keV X-rays. Our X-ray limits are an order of magnitude less constraining than previous limits because we use a more realistic ejecta absorption model based on three-dimensional neutrino-driven SN explosion models (Alp et al. 2018). The allowed bolometric luminosity of the compact object is 22 L Corresponding author: Dennis Alp dalp@kth.se arXiv:1805.04526v2 [astro-ph.HE] 30 Jul 2018 2 Alp et al.if our line-of-sight is free of ejecta dust, or 138 L if dust-obscured. Depending on assumptions, these values limit the effective temperature of a neutron star to < 4-8 MK and do not exclude models, which typically are in the range 3-4 MK. For the simplest accretion model, the accretion rate for an efficiency η is limited to < 10 −11 η −1 M yr −1 , which excludes most predictions. For pulsar activity modeled by a rotating magnetic dipole in vacuum, the limit on the magnetic field strength (B) for a given spin period (P ) is B 10 14 P 2 G s −2 , which firmly excludes pulsars comparable to the Crab. By combining information about radiation reprocessing and geometry, it is likely that the compact object is a dustobscured thermally-emitting neutron star, which may appear as a region of higher-temperature ejecta dust emission.