[
    {
        "id": "authors:fba02-bnp76",
        "collection": "authors",
        "collection_id": "fba02-bnp76",
        "cite_using_url": "https://authors.library.caltech.edu/records/fba02-bnp76",
        "type": "book_section",
        "title": "Results from 1.4 Millimeter Wavelength Interferometry at the Owens Valley",
        "book_title": "Submillimetre Astronomy",
        "author": [
            {
                "family_name": "Mundy",
                "given_name": "L. G.",
                "orcid": "0000-0002-8876-0690"
            },
            {
                "family_name": "Sargent",
                "given_name": "A. I.",
                "orcid": "0000-0002-4633-5098",
                "clpid": "Sargent-A-I"
            },
            {
                "family_name": "Scoville",
                "given_name": "N. Z.",
                "orcid": "0000-0002-0438-3323",
                "clpid": "Scoville-N-Z"
            },
            {
                "family_name": "Padin",
                "given_name": "S.",
                "orcid": "0009-0001-9993-4393",
                "clpid": "Padin-Stephen"
            },
            {
                "family_name": "Woody",
                "given_name": "D. P.",
                "orcid": "0000-0003-1734-2472",
                "clpid": "Woody-D-P"
            }
        ],
        "abstract": "<div class=\"c-article-section\">\n<div class=\"c-article-section__content\">\n<p>This paper summarizes the first interferometric results in the 1.4 mm band from the Owens Valley Radio Observatory (OVRO) Millimeter Wave Array. Relative to 2.7 mm, observations of thermal dust and molecular emission at 1.4 mm benefit from increased emissivity and brightness temperature sensitivity. For optically thin emir ion in the Rayleigh-Jeans limit, dust emission increases as &lambda;<sup>3</sup>&nbsp;to &lambda;<sup>-4</sup>&nbsp;assuming &lambda;<sup>-1</sup>&nbsp;to &lambda;<sup>-2</sup>&nbsp;wavelength dependence for the dust emissivity, while molecular emission increases faster than &lambda;<sup>-2</sup>&nbsp;due to the Planck function and the larger statistical weights of higher levels. In the optically thick limit, both increase as &lambda;<sup>-2</sup>. This &lambda;<sup>-2</sup> advantage can also be expressed in terms of the brightness temperature sensitivity; for a given beam size, the rms brightness temperature corresponding to a specific rms flux level is a factor of 4 lower for the 1.4 mm band than for the 2.7 mm band.</p>\n</div>\n</div>",
        "doi": "10.1007/978-94-015-6850-0_54",
        "issn": "0067-0057",
        "isbn": "978-94-015-6852-4",
        "publisher": "Springer Netherlands",
        "place_of_publication": "Dordrecht",
        "publication": "Astrophysics and Space Science Library",
        "publication_date": "1990-01-31",
        "volume": "158",
        "pages": "155-156"
    }
]