Ultraluminous infrared galaxies and the origin of quasars

Journal Article · Mon Feb 01 04:00:00 EST 1988 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/165983· OSTI ID:7129036

Sanders, D B; Soifer, B T; Elias, J H; Matthews, K; Madore, B F

An evolutionary connection between ultraluminous infrared galaxies and quasars is deduced from observations of all 10 infrared galaxies with luminosities L(8-1000 microns) of 10 to the 12th solar luminosities and greater. The observations show that all the galaxies are strongly interacting, with most appearing to be advanced mergers of two spiral disks. Nine of the 10 have dominant nonthermal optical emission lines, and the near-infrared colors show a mixture of starburst and AGN energy sources. All appear to be extremely rich in molecular gas. These observations are interpreted to imply that the ultraluminous infrared objects are dust-enshrouded quasars. A model is presented for the formation of ultraluminous infrared galaxies through the strong interaction or merger of two molecular gas-rich spirals. 76 references.

• Research Organization: Palomar Observatory, Pasadena, CA (USA); David Dunlap Observatory, Richmond Hill (Canada)
• OSTI ID: 7129036
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 325; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BASIC INTERACTIONS
CARBON COMPOUNDS
CARBON MONOXIDE
CARBON OXIDES
CHALCOGENIDES
CONFIGURATION
COSMIC GASES
COSMIC RADIO SOURCES
ELECTROMAGNETIC RADIATION
EMISSION SPECTRA
FLUIDS
GALACTIC EVOLUTION
GALAXIES
GALAXY NUCLEI
GASES
GRAVITATIONAL INTERACTIONS
INFRARED RADIATION
INTERACTIONS
LUMINOSITY
MATHEMATICAL MODELS
OPTICAL PROPERTIES
ORIGIN
OXIDES
OXYGEN COMPOUNDS
PHYSICAL PROPERTIES
QUASARS
RADIATIONS
SPECTRA
SPIRAL CONFIGURATION
STAR EVOLUTION
VISIBLE SPECTRA