Clements, D. L.Petitpas, GlenFarrah, D.Hatziminaoglou, E.Babbedge, T.Rowan-Robinson, M.Pérez-Fournon, I.Hernán-Caballero, AntonioCastro-Rodríguez, NievesLonsdale, C.Surace, J.Franceschini, A.Wilkes, BelindaSmith, Howard2017-01-122009Clements, D. L., G. Petitpas, D. Farrah, E. Hatziminaoglou, T. Babbedge, M. Rowan-Robinson, I. Pérez-Fournon, et al. 2009. “Resolved Dust Emission in a Quasar at Z = 3.65.” The Astrophysical Journal 698 (2) (June 5): L188–L191. doi:10.1088/0004-637x/698/2/l188.0004-637Xhttp://nrs.harvard.edu/urn-3:HUL.InstRepos:29921903We present submillimeter observations of the z = 3.653 quasar SDSS 160705+533558 together with data in the optical and infrared. The object is unusually bright in the far-IR and submillimeter with an IR luminosity of ∼1014 L . We ascribe this luminosity to a combination of active galactic nucleus (AGN) and starburst emission, with the starburst forming stars at a rate of a few thousand solar masses per year. Submillimeter Array imaging observations with a resolution ∼1 show that the submillimeter (850μm) emission is extended on scales of 10–35 kpc and is offset from the optical position by ∼ 10 kpc. This morphology is dissimilar to that found in submillimeter galaxies, which are generally unresolved or marginally resolved on arcsecond scales, or submillimeter-luminous AGNs where the AGN lies at the peak of the submillimeter or molecular emission. The simplest explanation is that the object is in the early stages of a merger between a gas-rich galaxy, which hosts the starburst, and a gas-poor AGN-host galaxy, which is responsible for the quasar emission. It is also possible that jet-induced star formation might contribute to the unusual morphology.en-USGalaxies: high-redshiftGalaxies: interactionsGalaxies: starburstQuasars: individual (SDSS 160705+533558)SubmillimeterJournal Article2017-01-1210.1088/0004-637X/698/2/L188