The distribution of the molecular layer about the galactic plane in the outer Galaxy is determined. Between R = 10.5 and 12.5 kpc, the average CO midplane dips from z = -48 to -167 pc below the b = 0 deg plane,
We have observed the dense molecular clouds in a 150′ x40′ (1xb) region around the Galactic center with CSJ=1-0 using the 45-m telescope at Nobeyama Radio Observatory. Total mass of the clouds isM(H2= (0.6-1.4) ×108M⊙ Almost all clouds comprise of long and curved molecular filamen...
Possible signatures of the presence of molecular clouds in our galaxy are discussed. We also discuss how molecular clouds as well as MACHOs can be observed directly in the nearby M31 galaxy.De Paolis, F; Ingrosso, G; Jetzer, P; Roncadelli, Marco...
The velocity field of the gas is highly chaotic, with some clouds having large (>100 km s-1) departures from the velocity pattern expected from purely circular orbits; however, most of the gas (70%) lies in a thin sheet in the Galactic plane. The rotation curve of the gas varies from...
(2016) used 12CO CfA-Chile survey data, dividing the galactic plane into four quadrants according to the size of the longitude, and then plotted dendrograms, respectively. Where the first quadrant (13∘<l<17∘) has a rich molecular cloud structure and a more complete research history, ...
1e-9 for the SiO clouds and 1e-10 for the other molecular clouds in the GC. The characteristics (size and H2 densities) of the SiO emission in the GC are completely different from those observed in the Galactic disk, where the SiO emission arises from much smaller regions with larger ...
Insights into the collapse and expansion of molecular clouds in outflows from observable pressure gradients Article 21 July 2022 Cold gas in the Milky Way’s nuclear wind Article 19 August 2020 The nested morphology of disk winds from young stars revealed by JWST/NIRSpec observations Article...
Physical processes that have been suggested as sources of the turbulence in molecular clouds are expanding HII regions, supernova remnants, cloud–cloud collisions, galactic differential rotation, and stellar winds. Unfortunately, for all of these processes there are theoretical problems with coupling ...
Non-equilibrium H2 ortho-to-para ratio in two molecular clouds of the Galactic CenterRodriguez-FernandezN. J.Martin-PintadoJ.de VicenteP.FuenteA.HuttemeisterS.ASTRONOMY AND ASTROPHYSICS -BERLIN-
An IRAC/Spitzer Space Telescope infrared image of the center of our galaxy. The infrared penetrates much of the dust to reveal the stars of the crowded galactic center region. Older, cool stars are blue; reddish dust clouds are associated with young stars in stellar nurseries. The galactic cen...