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Synthesis imaging of the DR 21(OH) cluster. I - Dust continuum and C(O-18) emission

Jeffrey G. Mangum, Alwyn Wootten, Lee G. Mundy

Open publisher page 44 citations

Abstract

This study presents maps at 7-arcsec resolution of 2.7-mm continuum and J = 1 to 0 C(O-18) emission that were made of the DR 21(OH) molecular cloud core. Three compact regions were detected. Two components, each measuring about 12,000 AU, containing about 400-500 solar masses of material, and encompassing H2O masers, were found to dominate the most compact, luminous, and massive region. Even though these two components are separated by only about 8 arcsec on the sky and 3.5 km/s in velocity, they are quite different, possibly representing different phases of early stellar formation. The other two compact regions, mapped in molecular emission, are located to the south of the OH source. They measure about 30,000 AU, comprise about 500 solar masses of material, and have no associated maser or known mid-infrared sources. These latter regions are warm (not less than 20 K) gas condensations.

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What this paper is about

This study presents maps at 7-arcsec resolution of 2.7-mm continuum and J = 1 to 0 C(O-18) emission that were made of the DR 21(OH) molecular cloud core. Three compact regions were detected. Two components, each measuring about 12,000 AU, containing about 400-500 solar masses of material, and encompassing H2O masers, were found to dominate the most compact, luminous, and massive region. Even though these two components are separated by only about 8 arcsec on the sky and 3.5 km/s in velocity, they are quite different, possibly representing different phases of early stellar formation. The other two compact regions, mapped in molecular emission, are located to the south of the OH source. They measure about 30,000 AU, comprise about 500 solar masses of material, and have no associated maser or known mid-infrared sources. These latter regions are warm (not less than 20 K) gas condensations.

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Available abstract

This study presents maps at 7-arcsec resolution of 2.7-mm continuum and J = 1 to 0 C(O-18) emission that were made of the DR 21(OH) molecular cloud core. Three compact regions were detected. Two components, each measuring about 12,000 AU, containing about 400-500 solar masses of material, and encompassing H2O masers, were found to dominate the most compact, luminous, and massive region. Even though these two components are separated by only about 8 arcsec on the sky and 3.5 km/s in velocity, they are quite different, possibly representing different phases of early stellar formation. The other two compact regions, mapped in molecular emission, are located to the south of the OH source. They measure about 30,000 AU, comprise about 500 solar masses of material, and have no associated maser or known mid-infrared sources. These latter regions are warm (not less than 20 K) gas condensations.

Key concepts: Physics, Astrophysics, Maser, Astronomy, Molecular cloud, Interstellar medium, Star formation, Infrared

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