We present measurements of the integrated flux relative to the local background of the Large and Small Magellanic Clouds and the region 30-Doradus (the Tarantula Nebula) in the LMC in four frequency bands centered at 245, 400, 460, and 630 GHz, based on observations made with the TopHat telescope. We combine these observations with the corresponding measurements for the DIRBE bands 8, 9, and 10 to cover the frequency range 245 -3000 GHz (100 − 1220 µm) for these objects. We present spectra for all three objects and fit these spectra to a single-component greybody emission model and report best-fit dust temperatures, optical depths, and emissivity power-law indices, and we compare these results with other measurements in these regions and elsewhere. Using published dust grain opacities, we estimate the mass of the measured dust component in the three regions.
The TopHat experiment was designed to measure the anisotropy in the cosmic microwave background radiation on angular scales from 0N3 to 30 and the thermal emission from both Galactic and extragalactic dust. The balloon-borne instrument had five spectral bands spanning frequencies from 175 to 630 GHz. The telescope was a compact, 1 m, onaxis Cassegrain telescope designed to scan the sky at a fixed elevation of 78 . The radiometer used cryogenic bolometers coupled to a single feed horn via a dichroic filter system. The observing strategy was intended to efficiently cover a region 48 in diameter centered on the south polar cap with a highly cross-linked and redundant pattern with nearly uniform sky coverage. The Long Duration Balloon flight over Antarctica in 2001 January surveyed about 6% of the sky. Here we describe the design of the instrument and the achieved in-flight performance and provide a brief discussion of the data analysis.
The TopHat Long Duration Balloon (LDB) experiment, which launched on January 4, 2001, mapped 6% of the sky in a region centered about the South Celestial Pole, The five spectral bands of the instrument span from 150 to 660 GHz and are sensitive to CMBR anisotropy and thermal galactic dust emission. Analysis is in progress. The parameters of the experiment, the observing scheme, and some preliminary results are discussed.
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