3 research outputs found
Structure in the nucleus of NGC 1068 at 10 microns
New 8 to 13 micron array camera images of the central kiloparsec of Seyfert 2 galaxy NGC 1068 resolve structure that is similar to that observed at visible and radio wavelengths. The images reveal an infrared source which is extended and asymmetric, with its long axis oriented at P.A. 33 deg. Maps of the spatial distribution of 8 to 13 micron color temperature and warm dust opacity are derived from the multiwavelength infrared images. The results suggest that there exist two pointlike luminosity sources in the central regions of NGC 1068, with the brighter source at the nucleus and the fainter one some 100 pc to the northeast. This geometry strengthens the possibility that the 10 micron emission observed from grains in the nucleus is powered by a nonthermal source. In the context of earlier visible and radio studies, these results considerably strengthen the case for jet induced star formation in NGC 1068
The 8.3 and 12.4 micron imaging of the Galactic Center source complex with the Goddard infrared array camera
A 30 x 30 arcsec field at the Galactic Center (1.5 x 1.5 parsec) was mapped at 8.3 microns and 12.41 microns with high spatial resolution and accurate relative astrometry, using the 16 x 16 Si:Bi accumulation mode charge injection device Goddard infrared array camera. The design and performance of the array camera detector electronics system and image data processing techniques are discussed. Color temperature and dust opacity distributions derived from the spatially accurate images indicate that the compact infrared sources and the large scale ridge structure are bounded by warmer, more diffuse material. None of the objects appear to be heated appreciably by internal luminosity sources. These results are consistent with the model proposing that the complex is heated externally by a strong luminosity source at the Galactic Center, which dominates the energetics of the inner few parsecs of the galaxy
Connecting the cosmic infrared background to the X-ray background
We estimate the contribution of AGNs and of their host galaxies to the
infrared background. We use the luminosity function and evolution of AGNs
recently determined by the hard X-ray surveys, and new Spectral Energy
Distributions connecting the X-ray and the infrared emission, divided in
intervals of absorption. These two ingredients allow us to determine the
contribution of AGNs to the infrared background by using mostly observed
quantities, with only minor assumptions. We obtain that AGN emission
contributes little to the infrared background (5% over most of the infrared
bands), implying that the latter is dominated by star formation. However, AGN
host galaxies may contribute significantly to the infrared background, and more
specifically 10--20% in the 1--20m range and 5% at . We also give the contribution of AGNs and of their host galaxies to the
source number counts in various infrared bands, focusing on those which will be
observed with Spitzer. We also report a significant discrepancy between the
expected contribution of AGN hosts to the submm background and bright submm
number counts with the observational constraints. We discuss the causes and
implications of this discrepancy and the possible effects on the Spitzer far-IR
bands.Comment: to appear in MNRAS, replaced with accepted version, paper shortened,
results unchange