Aperture synthesis observations of CO emission from the W3 molecular cloud core

Molecular Cloud Core and CS Outflow Associated with Haro 4-255 FIR

International Astronomical Union Colloquium ◽

10.1017/s0252921100019540 ◽

1994 ◽

Vol 140 ◽

pp. 228-229

Author(s):

K. Tatematsu ◽

T. Umemoto ◽

Y. Murata ◽

H. Chen ◽

N. Hirano ◽

...

Keyword(s):

Molecular Cloud ◽

Aperture Synthesis ◽

Cloud Core

AbstractThe region containing Haro 4-255 FIR is studied in CS (1-0) with the 45 m telescope and the Nobeyama Millimeter Array. We have detected intense CS outflow. The CS abundance is found to be enhanced in the outflow lobe. The aperture synthesis data show two groups of emission, one of which is likely to impede the blueshifted CS lobe.

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13CO(J = 1-0) Observations of the Orion Molecular Cloud

Symposium - International Astronomical Union ◽

10.1017/s007418090009519x ◽

1987 ◽

Vol 115 ◽

pp. 149-150

Author(s):

K. Sugitani ◽

Y. Fukui

Keyword(s):

Millimeter Wave ◽

High Velocity ◽

Molecular Cloud ◽

High Velocity Resolution ◽

H Ii Region ◽

Co Emission

We present new 13CO(J = 1-0) measurements of the Orion molecular cloud. The data were taken with the 4-m millimeter-wave telescope of Nagoya University with a beamwidth of 2.7′. The high velocity resolution of 0.1 km s−1 employed has revealed significant details of the 13CO emission toward the H II region.

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Infrared Space ObservatoryLong Wavelength Spectrometer Observations of a Cold Giant Molecular Cloud Core near the Galactic Center

The Astrophysical Journal ◽

10.1086/306366 ◽

1998 ◽

Vol 507 (2) ◽

pp. 794-804 ◽

Cited By ~ 50

Author(s):

D. C. Lis ◽

Karl M. Menten

Keyword(s):

Molecular Cloud ◽

Galactic Center ◽

Giant Molecular Cloud ◽

Cloud Core

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Density and kinematics of the W49A cloud core

Symposium - International Astronomical Union ◽

10.1017/s0074180900199528 ◽

1991 ◽

Vol 147 ◽

pp. 494-495

Author(s):

E. Serabyn ◽

R. Güsten

Keyword(s):

Molecular Cloud ◽

Temperature Scale ◽

Dense Core ◽

Density Structure ◽

Cloud Core

The dense core of the W49A molecular cloud (Miyawaki et al. 1986, Schloerb et al. 1987) has been mapped in 5 different transitions of CS and C34S, in order to determine its density structure. The three lower frequency transitions (CS J=3-2, CS J=5-4 and C34S J=5-4) were observed with the IRAM 30m telescope, and the two highest frequency transitions (CS J=7-6 and C34S J=7-6) with the Caltech Submillimeter Observatory. The beamsizes were in the range 12″ to 20″. As a calibration check, the CS J=7-6 line was observed with both telescopes, and was found to give a consistent temperature scale. The spectra at the peak of the emission are shown in Fig. 1.

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Density and kinematics of the W49A cloud core

Symposium - International Astronomical Union ◽

10.1017/s007418090024014x ◽

1991 ◽

Vol 147 ◽

pp. 494-495

Author(s):

E. Serabyn ◽

R. Güsten

Keyword(s):

Molecular Cloud ◽

Temperature Scale ◽

Dense Core ◽

Density Structure ◽

Cloud Core

The dense core of the W49A molecular cloud (Miyawaki et al. 1986, Schloerb et al. 1987) has been mapped in 5 different transitions of CS and C34S, in order to determine its density structure. The three lower frequency transitions (CS J=3-2, CS J=5-4 and C34S J=5-4) were observed with the IRAM 30m telescope, and the two highest frequency transitions (CS J=7-6 and C34S J=7-6) with the Caltech Submillimeter Observatory. The beamsizes were in the range 12″ to 20″. As a calibration check, the CS J=7-6 line was observed with both telescopes, and was found to give a consistent temperature scale. The spectra at the peak of the emission are shown in Fig. 1.

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Observations of Orion Molecular Cloud with NMA

International Astronomical Union Colloquium ◽

10.1017/s0252921100019448 ◽

1994 ◽

Vol 140 ◽

pp. 185-189

Author(s):

Y. Murata ◽

R. Kawabe ◽

M. Ishiguro ◽

K.-I. Morita ◽

T. Hasegawa ◽

...

Keyword(s):

Magnetic Field ◽

Molecular Cloud ◽

Gas Flow ◽

Position Angle ◽

Aperture Synthesis ◽

Width Ratio ◽

Length Width ◽

The Magnetic Field

AbstractWe have made aperture synthesis multifield observations of Orion Molecular Cloud-1 (OMC-1) in the CS (J=1-0) line using the Nobeyama Millimeter Array (NMA), and obtained 9” resolution maps over 10’ length. The OMC-1 ridge shows a wiggled structure. The position angle of whole the ridge is ~ 0° - 10°, but ~ 20° - 30°around the clumps. It is possible to make this structure by the magnetic field with a position angle of ~ 150°. We also found filamentary structures in the northwest of Orion-KL, with a length-width ratio of more than 25, which are made by the gas flow from Orion-KL.

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