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The structure and extent of the giant molecular cloud near M17
Elmegreen, B. G.; Lada, C. J.; Dickinson, D. F.
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.), AC(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.)
Astrophysical Journal, Part 1, vol. 230, June 1, 1979, p. 415, 416, 418-427. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Galactic Structure, Interstellar Gas, Milky Way Galaxy, Nebulae, Carbon Monoxide, Cloud Physics, Gas Discharges, H Ii Regions, Stellar Evolution
Bibliographic Code:


Results are reported for CO observations of the area SW of the H II region M17. It is found that: (1) molecular emission from 4 deg along the galactic plane SW of M17 consists of two prominent clouds (Regions I and III), between which is what appears to be a low-intensity bridge of clumpy CO (Region II); (2) the total observed mass is at least 320,000 solar masses; (3) Region I consists of four discrete fragments, each having a mass of about 40,000 solar masses; (4) the NE end of Region I is morphologically different from the SW end; and (5) M16, M17 along with Region I, and Region III appear to be equally spaced along the galactic plane and alternate on either side of the plane by more than their own diameters.

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