Far-infrared continuum emission from the nucleus, starburst, and extended spiral arms of NGC 1068

Journal Article · Thu Oct 01 04:00:00 EDT 1987 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/165668· OSTI ID:5605310

Lester, D F; Joy, M; Harvey, P M; Ellis, Jr, H B; Parmar, P S

Far-infrared slit scans across NGC 1068 are used to better define the contribution of the active nucleus, starburst disk, and extended spiral arms in the luminous output of this bright Seyfert 2 galaxy. The decomposition of the emission from the bright, inner 3 kpc of this galaxy suggests that at 50 microns, about half the emission is from star formation in a starburst disk and half from the compact, centrally heated circumnuclear cloud. The 100-micron profile of the starburst disk is asymmetric with respect to the nucleus. This appears to be the result of an extraordinary star-forming complex about a kiloparsec away from the center. With the application of maximum entropy deconvolution to the scans, evidence is found for 100-micron emission from the extended spiral arms of the galaxy. The far-infrared emission from the starburst region is distinguished from that of the extended spiral arms. In terms of both total luminosity and surface brightness, the extended spiral arms of NGC 1068 are at the bright end of the range of far-infrared emission from quiescent, noninteracting spirals. 17 references.

• Research Organization: McDonald Observatory, Austin, TX
• OSTI ID: 5605310
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 321; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
CONFIGURATION
ELECTROMAGNETIC RADIATION
ENTROPY
FAR INFRARED RADIATION
GALAXIES
GALAXY NUCLEI
INFRARED RADIATION
INFRARED SPECTRA
LUMINOSITY
NEAR INFRARED RADIATION
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
RADIATIONS
SEYFERT GALAXIES
SPECTRA
SPIRAL CONFIGURATION
STAR EVOLUTION
THERMODYNAMIC PROPERTIES