Resolved Dust Emission in a Quasar at Z = 3.65

DSpace/Manakin Repository

Resolved Dust Emission in a Quasar at Z = 3.65

Citable link to this page


Title: Resolved Dust Emission in a Quasar at Z = 3.65
Author: Clements, D. L.; Petitpas, Glen Raymond; Farrah, D.; Hatziminaoglou, E.; Babbedge, T.; Rowan-Robinson, M.; Pérez-Fournon, I.; Hernán-Caballero, Antonio; Castro-Rodríguez, Nieves; Lonsdale, C.; Surace, J.; Franceschini, A.; Wilkes, Belinda Jane; Smith, Howard A.

Note: Order does not necessarily reflect citation order of authors.

Citation: Clements, 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.
Full Text & Related Files:
Abstract: We 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.
Published Version: doi:10.1088/0004-637X/698/2/L188
Other Sources:
Terms of Use: This article is made available under the terms and conditions applicable to Other Posted Material, as set forth at
Citable link to this page:
Downloads of this work:

Show full Dublin Core record

This item appears in the following Collection(s)


Search DASH

Advanced Search