CO Observations of the Molecular Cloud Encompassing Sharpless 222

1982 ◽  
pp. 343-348 ◽  
Author(s):  
R. A. Christie ◽  
W. H. McCutcheon ◽  
C. P. Chan
Keyword(s):  
Molecular Cloud ◽  
Co Observations

scholarly journals CO observations of spiral structure and the lifetime of giant molecular clouds

1979 ◽  
Vol 84 ◽  
pp. 277-283
Author(s):  
N. Z. Scoville ◽  
P. M. Solomon ◽  
D. B. Sanders
Keyword(s):  
Molecular Cloud ◽  
Mass Fraction ◽  
Molecular Clouds ◽  
Spiral Structure ◽  
Large Mass ◽  
Giant Molecular Clouds ◽  
Spiral Pattern ◽  
The Galaxy ◽  
Co Emission ◽  
Co Observations

Observations of CO emission at ℓ=0 to 70°, |b| ≤ 1° are analyzed to give a map of the molecular cloud distribution in the galaxy as viewed from the galactic pole. From the fact that this distribution shows no obvious spiral pattern we conclude that the giant molecular clouds sampled in the CO line are situated in both arm and interarm regions and they must last more than 108 years. A similar age estimate is deduced from the large mass fraction of H2 in the interstellar medium in the interior of the galaxy. An implication of this longevity is that the great masses of these clouds may be accumulated through cloud-cloud collisions of originally smaller clouds.

Evidence for the Existence of a Low-Velocity Molecular Cloud near Sgr A

1978 ◽  
Vol 3 (4) ◽  
pp. 266-269 ◽  
Author(s):  
J. B. Whiteoak ◽  
F. F. Gardner
Keyword(s):  
High Velocity ◽  
Molecular Cloud ◽  
Molecular Clouds ◽  
Galactic Centre ◽  
The Sun ◽  
Low Velocity ◽  
High Velocity Resolution ◽  
Sgr A ◽  
Galactic Longitude ◽  
Co Observations

In the wide complex profiles of OH, H2CO and CO spectra observed in directions towards the galactic centre, only the features at radial velocities near + 40 km s-1 are generally believed to originate in the molecular clouds nearest the galactic nucleus. The features at other velocities are associated with clouds or spiral features that can be traced over larger ranges of galactic longitude, implying locations which are more distant from the nucleus. In particular, the features near zero velocity have been traditionally associated with molecular clouds within 1-2 kpc of the Sun. However, H2CO observations with high velocity resolution provide evidence that one cloud with velocity near zero is probably near the galactic nucleus.

CO Observations of High-Velocity Flows in the Core of the NGC 7538 Molecular Cloud

1987 ◽  
pp. 355-356
Author(s):  
Osamu Kameya ◽  
Tatsuhiko Hasegawa ◽  
Naomi Hirano ◽  
Keiya Takakubo ◽  
Munezo Seki
Keyword(s):  
High Velocity ◽  
Molecular Cloud ◽  
The Core ◽  
Co Observations

scholarly journals A Possible Molecular Counterpart to the G359.54+0.18 Non-Thermal Filaments

1989 ◽  
Vol 136 ◽  
pp. 189-193
Author(s):  
John Bally ◽  
Farhad Yusef-Zadeh ◽  
J. M. Hollis
Keyword(s):  
Molecular Cloud ◽  
Galactic Center ◽  
Molecular Gas ◽  
Thermal Radio ◽  
Co Observations

We present new 30″ resolution J=2–1 12CO observations of the molecular gas located close to a group of non-thermal radio emitting filaments recently detected near the Galactic center (Bally and Yusef-Zadeh, 1989). The new data provide some support for the association of the non-thermal filaments G359.54+0.18 with the projected edge of a molecular cloud.

A Nearby Example of a Giant Molecular Cloud

1980 ◽  
Vol 87 ◽  
pp. 185-186
Author(s):  
J. W. Barrett ◽  
R.L. deZafra ◽  
D. B. Sanders ◽  
P. M. Solomon
Keyword(s):  
Millimeter Wave ◽  
Molecular Cloud ◽  
Open Cluster ◽  
Beam Size ◽  
University Of Texas ◽  
Intense Emission ◽  
Half Power ◽  
The University ◽  
Right Ascension ◽  
Co Observations

We have mapped an extensive molecular cloud in Perseus in the 115 GHz line of 12CO. Observations were made every 10′ in right ascension and declination over most of the cloud, and every 2′ in the regions of most intense emission, near the open cluster IC 348 and near the reflection nebula NGC 1333. We also obtained 110 GHz 13CO data every 2′ in the latter regions, as well as every 10′ in several long strips across the cloud. A total of 812 positions were observed in 12CO, and 200 in 13CO. This work was done using the 5 m antenna of the Millimeter Wave Observatory of the University of Texas. The half-power beam size was 2!6.

scholarly journals Mapping Distances across the Perseus Molecular Cloud Using CO Observations, Stellar Photometry, and Gaia DR2 Parallax Measurements

2018 ◽  
Vol 869 (1) ◽  
pp. 83 ◽  
Author(s):  
Catherine Zucker ◽  
Edward F. Schlafly ◽  
Joshua S. Speagle ◽  
Gregory M. Green ◽  
Stephen K. N. Portillo ◽  
...  
Keyword(s):  
Molecular Cloud ◽  
Stellar Photometry ◽  
Gaia Dr2 ◽  
Co Observations

CO observations of a high-latitude molecular cloud associated with NGC 7023

1978 ◽  
Vol 220 ◽  
pp. 510 ◽  
Author(s):  
D. M. Elmegreen ◽  
B. G. Elmegreen
Keyword(s):  
High Latitude ◽  
Molecular Cloud ◽  
Co Observations

scholarly journals The Molecular Cloud Content of Spiral and Dwarf Galaxies

1986 ◽  
Vol 7 ◽  
pp. 519-524
Author(s):  
L. J Rickard
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Massive Star ◽  
Spiral Structure ◽  
Dwarf Galaxies ◽  
Molecular Gas ◽  
Molecular Component ◽  
Massive Star Formation ◽  
Co Observations

AbstractThis paper concentrates on the molecular cloud component in its role as the site of current star formation – especially massive star formation. It is further restricted to the molecular component as traced by CO, the preeminent tracer of molecular gas in galaxies despite the problems discussed here. The basic topics addressed are (1) the variation of CO properties with galactic environment and type; (2) the problems involved in the inference of H2 distributions for individual galaxies from CO observations; and (3) the particular question of the presence of spiral structure in the CO component.

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