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- W4246558280 abstract "In 1968 NH 3 molecules were discovered in gas clouds near the center of our Galaxy. The NH 3 molecules showed emission lines in transitions arising from metastable J = K rotational states. NH 3 has many transitions at about 1.25 cm; hence, a great deal can be learned about the gas clouds. In particular, 1-1, 2-2, 3-3, 4-4 have excitation temperatures of 24K, 65K, 125K, 203K respectively. Thus, one can determine temperatures very accurately by comparing line strengths to statistical theory. NH 3 is particularly useful as an interstellar thermometer since all of these lines can be detected by a single radio telescope with essentially the same beam size. Generally, a telescope measures the antenna temperature T A of an object which is related to the brightness temperature T B of an object by T A =Ω s /Ω A T Bj ; Ω s /Ω A ≤1 . T A = T B when Ω s ≥Ω A where Ω A is the solid angle of the antenna pattern and Ω s , is the solid angle of the source as seen from the antenna. If measurements can be made with the same telescope, T B for different spectral lines will be simply related to the T A for the lines and one does not have the complication of source size and geometry." @default.
- W4246558280 created "2022-05-12" @default.
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- W4246558280 date "1971-01-01" @default.
- W4246558280 modified "2023-09-28" @default.
- W4246558280 title "NH<sub>3</sub> and H<sub>2</sub>O Emission in our Galaxy" @default.
- W4246558280 doi "https://doi.org/10.1017/s1539299600000356" @default.
- W4246558280 hasPublicationYear "1971" @default.
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