Accession Number:

ADA172609

Title:

Structure of the Extended Emission in the Infrared Celestial Background,

Descriptive Note:

Corporate Author:

AIR FORCE GEOPHYSICS LAB HANSCOM AFB MA

Personal Author(s):

Report Date:

1986-09-30

Pagination or Media Count:

16.0

Abstract:

The extended emission in the infrared celestial background may be divided into three main components the zodiacal background, the large discrete sources in the galaxy and the interstellar dust. The zodiacal background is due to the thermal reradiation of sunlight absorbed by the dust in the solar system. An earth orbiting infrared telescope will detect the diffuse emission from this dust in all directions with maximum intensity lying roughly along the ecliptic plane where the density of dust is highest. Structure with scale lengths of 10 deg have been measured in both the visual and infrared finer structure has been detected in the infrared by the Infrared Astronomy Satellite. H II regions, areas of ionized gas mixed with and surrounded by dust, are the brightest discrete objects in the galaxy in the long wavelength infrared re-emitted in the infrared with a range of temperatures characteristic of the thermal equilibrium for the surroundings of the dust. The emission from the interstellar dust produces a filimentary structured background, the infrared cirrus. The observed far infrared color temperature of about 20-35K for the cirrus is consistent with emission form graphite and silicate grains which absorb the interstellar radiation field. The much larger LWIR color temperature is likely due to a greater abundance of sub-micron particles in the interstellar medium and, perhaps, from band emission due to polycyclic aromatic hydrocarbons. These galactic plane which has full width at half maxima of about 2 deg.

Subject Categories:

  • Astronomy
  • Infrared Detection and Detectors

Distribution Statement:

APPROVED FOR PUBLIC RELEASE