Molecular gas kinematics and high-mass star formation in the spiral arms of the Milky Way

Details Molecular gas kinematics and high-mass star formation in the spiral arms of the Milky Way Molecular gas kinematics and high-mass star formation in the spiral arms of the Milky Way

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004rmxac..21..143l&link_type=abstract

The Environment and Evolution of Double and Multiple Stars, Proceedings of IAU Colloquium 191, held 3-7 February, 2002 in Merida

Astronomy and Astrophysics

Astronomy

1

Binaries: Close, Galaxy: Kinematics And Dynamics, Ism: Molecules

Scientific paper

We study the kinematic of the molecular gas using observations of the rotational line 12CO(J=1 to 0), and also the star formation traced by Ultra-Compact HII regions in the IV galactic quadrant (270 o ≤ l ≤ 360°). Our results show that there is a connection between 1) high-mass star formation in the spiral arms of the Milky Way, 2) molecular gas of high column density, and 3) the large-scale rigid-body-like motion of the gas. The large-scale rigid-body-like motions observed in the arms imply that there is less angular momentum to dissipate in the formation processes of stellar systems. We show a multiple stellar system under study, embedded in its parent molecular cloud in the Carina arm region.

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