Titlebook: New Extragalactic Perspectives in the New South Africa; Proceedings of the I David L. Block,J. Mayo Greenberg Conference proceedings 1996 K

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How Cold Could Galaxies Be?n inside them. Sub-millimeter detectors will soon allow us to map the coldest obscuring material directly. Ever more powerful computers permit modelling of the escape of the radiation in progressively more realistic ways. In the process some of our comfortable old ideas, such as the transparency of

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Temperature Fluctuations and Very Cold Dustdiation field. These grains cool by emission of infrared radiation at wavelengths that are out of equilibrium with thermal emission at the average grain temperature. One effect of this is the appearance of excess emission at short (∼ 3.) and middle (12 – 25.) infrared wavelengths which signals the p

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The Interstellar Medium as Observed by COBEhe early universe. It also measured emission from nearby sources such as the stars, dust, molecules, atoms, ions, and electrons in the Milky Way, and dust and comets in the Solar System. It was launched 18 November 1989 on a Delta rocket, carrying one microwave instrument and two cryogenically coole

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Molecular Gas in Spiral Galaxieserture millimeter radio telescopes in the λ2.6 mm line of the .CO molecule; an excellent example is the comprehensive FCRAO survey by Young .. (1995). The measurement actually made is the surface brightness of the .CO(1-0) line emission, diluted by the beam of the radio telescope, from which the bea

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Memorial

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Optical, IR, and HI Observations of a Large Complete Cluster Sample These difficulties can be overcome by studying the members of clusters. The objects are essentially at the same distance and all objects that meet specified selection criteria within the volume of the cluster can be included. For example, a flux threshold might be set in some spectral band and this

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The Relationship Between Near IR Extinction and CO Emission by using a radiative transfer model to match the observed optical and infrared colors at different positions in each galaxy. With assumptions of dense dust fractions and a constant dust to gas ratio, the comparision of the ratio of dust optical depth to integrated CO emission can be used to look at

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