 |
 |
 |
 |
 |
 |
|
|
|
|
|
|
Kutner, M.L., K.D. Tucker, G. Chin, and P. Thaddeus, 1977: The molecular complexes in Orion. Astrophys. J., 215, 521-528, doi:10.1086/155384.
Line emission from CO at 2.6 mm is observed over an area of 28 square degrees in the Orion region. Most of the emission comes from two giant molecular complexes, roughly associated with Ori B and Ori A. The latter provides the best example of a giant molecular complex at the end of a sequence of OB association subgroups of decreasing age. This complex is apparently rotating with an angular velocity 4.5×10-15 /s, but in a direction opposed to the Galactic rotation. The apparently denser parts of the cloud are rotating at a somewhat greater angular velocity. The total mass of the molecular gas derived from the observations is 2×105 M☉, implying that roughly half the matter in this region is in the form of molecular hydrogen.
|
|
|
