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The high photometric quality and full-sky coverage in the COBE DIRBE datasets make possible detailed studies of the interplanetary medium. This paper presents a preliminary derivation of the infrared scattering phase function of interplanetary dust. The ultimate purpose of these investigations is to use the DIRBE observations to constrain the composition, size and structure of interplanetary dust grains.
We have found and cataloged over 100 vertical structures in H I, infrared, and radio continuum emission. These correspond to the H I worms detected by Heiles (1984). The infrared and the radio continuum properties of worms suggest that some worms have associated ionized gas. The area filling factor of superbubbles in the inner Galaxy is estimated to be greater than ~0.1.
IRAS, COBE, and ISO have demonstrated the unique importance of a cryogenic infrared telescope in space for studying diffuse infrared backgrounds and for teasing out the individual point sources which contribute to them. This importance results from the extremely high infrared sensitivity of such telescopes, particularly to diffuse radiation. The next cryogenic infrared telescope will be NASA's Space Infrared Telescope Facility (SIRTF), which is currently in the final stages of construction leading to launch in 2002. SIRTF will be the first infrared space observatory to make extensive use - both for imaging and spectroscopy - of large format infrared detector arrays. The sensitivity and spatial and spectral coverage of SIRTF's array-based instruments endow SIRTF with great power for the study of the cosmic infrared background (CIRB) and related scientific issues. This paper reviews the SIRTF mission design and measurement functionality and describes SIRTF's potential studies of the CIRB, drawing examples from the programs planned by the SIRTF Guaranteed Time Observers (GTO's). We also summarize the opportunities for community participation in SIRTF.
Early results from the SAGE-SMC (Surveying the Agents of Galaxy Evolution in the tidally-disrupted, low-metallicity Small Magellanic Cloud) Spitzer legacy program are presented. These early results concentrate on the SAGE-SMC MIPS observations of the SMC Tail region. This region is the high H i column density portion of the Magellanic Bridge adjacent to the SMC Wing. We detect infrared dust emission and measure the gas-to-dust ratio in the SMC Tail and find it similar to that of the SMC Body. In addition, we find two embedded cluster regions that are resolved into multiple sources at all MIPS wavelengths.
J. Rho, Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA, 91125, USA,
S. Van Dyk, Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA, 91125, USA,
T. Jarrett, Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA, 91125, USA,
R. M. Cutri, Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA, 91125, USA,
W. T. Reach, Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA, 91125, USA
We present near-infrared imaging of IC443, covering entire supernova remnant (50 diameter) from the Two Micron All Sky Survey (2MASS), which images are taken simultaneously in the J (1.25µm), H (1.65µm) and Ks (2.17µm) bands. Emission from IC443 was detected in all 3 bands from most of the optically bright parts of the remnant, revealing a shell-like morphology. These are the first near-infrared images that covers entire remnant. The color and structure are very different between the northeastern and southern parts. Bright J and H band emission from the northeast rim can be explained mostly by [Fe II] and the rest by hydrogen lines of Pβ and Br10. We also report ISO LWS observation of [O I] (63µm) for 11 positions in the northeast. Strong lines were detected and the strongest line is in the northeastern shell, where 2MASS image showed filamentary structure in J and H. In contrast, the southern ridge is dominated by Ks band light with knotty structure, and has weak J and H band emission. The shocked H2 line emission is well known from the sinus ridge produced by an interaction with dense molecular clouds. The large field of view and color of the 2MASS images show that the H2 emission extends to the east and the northeast. This H2 emission suggests that the interaction with the molecular clouds extends to the front side in the northeast.
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