High resolution J = 2 - 1 and J = 1 - 0 carbon monoxide self-reversed line profiles toward molecular clouds

1981 ◽  
Vol 245 ◽  
pp. 495 ◽  
Author(s):  
R. B. Loren ◽  
R. L. Plambeck ◽  
J. H. Davis ◽  
R. L. Snell
Keyword(s):  
Carbon Monoxide ◽  
High Resolution ◽  
Molecular Clouds ◽  
Line Profiles ◽  
Reversed Line

scholarly journals Molecular Outflows

1989 ◽  
Vol 120 ◽  
pp. 231-243
Author(s):  
Ronald L. Snell
Keyword(s):  
Carbon Monoxide ◽  
Sound Speed ◽  
Molecular Clouds ◽  
Molecular Form ◽  
Line Profiles ◽  
Internal Dynamics ◽  
Molecular Outflows ◽  
Submillimeter Spectroscopy ◽  
Line Widths ◽  
Co Emission

The development of millimeter and submillimeter spectroscopy has allowed astronomers to probe the cold, dense component of the interstellar medium. This medium, primarily composed of gas in molecular form, is gravitationally bound into relatively distinct clouds that are sites of star formation within our Galaxy. The most ubiquitous tracers of these molecular clouds are the rotational transitions of carbon monoxide. Observations of CO emission have been commonly used to estimate the size, temperature, mass, and density of molecular clouds; in addition, the spectral line profiles can be used to study the internal dynamics of these clouds. Although the sound speed within molecular clouds is only about 0.2 km s−1, observed CO line widths are more typically 1 to 5 km s−1. Thus, the internal dynamics of molecular clouds are characterized by supersonic gas motions whose nature is poorly understood.

scholarly journals Molecules in the Magellanic Clouds

1991 ◽  
Vol 148 ◽  
pp. 415-420 ◽  
Author(s):  
R. S. Booth ◽  
Th. De Graauw
Keyword(s):  
High Resolution ◽  
Molecular Clouds ◽  
Short Review ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Giant Molecular Clouds ◽  
Interstellar Molecules ◽  
First Time ◽  
Excitation Conditions

In this short review we describe recent new observations of millimetre transitions of molecules in selected regions of the Magellanic Clouds. The observations were made using the Swedish-ESO Submillimetre Telescope, SEST, (Booth et al. 1989), the relatively high resolution of which facilitates, for the first time, observations of individual giant molecular clouds in the Magellanic Clouds. We have mapped the distribution of the emission from the two lowest rotational transitions of 12CO and 13CO and hence have derived excitation conditions for the molecule. In addition, we have observed several well-known interstellar molecules in the same regions, thus doubling the number of known molecules in the Large Magellanic Cloud (LMC). The fact that all the observations have been made under controlled conditions with the same telescope enables a reasonable intercomparison of the molecular column densities. In particular, we are able to observe the relative abundances among the different isotopically substituted species of CO.

Electron impact studies. VI. Mass spectra of esters and thioesters. Skeletal rearrangement on electron impact

1967 ◽  
Vol 20 (4) ◽  
pp. 689 ◽  
Author(s):  
JH Bowie ◽  
RG Cooks ◽  
P Jakobsen ◽  
S Lawesson ◽  
G Schroll
Keyword(s):  
Carbon Dioxide ◽  
Carbon Monoxide ◽  
High Resolution ◽  
Electron Impact ◽  
Mass Spectra ◽  
Skeletal Rearrangement ◽  
Unsaturated Esters ◽  
Impact Studies ◽  
Unsaturated Alcohols ◽  
Metastable Ions

The mass spectra of representative series of simple alkyl acetoacetates, alkyl acetothioacetates, and some unsaturated esters derived from unsaturated alcohols or phenols are reported and discussed. The fragmentation schemes have been established by high resolution measurements, appropriate metastable ions, and by deuterium and 18O labelling. Many of the spectra show significant skeletal rearrangement fragments arising from either loss of carbon monoxide or carbon dioxide.

HIGH-RESOLUTION OSCILLATOR STRENGTH MEASUREMENTS OF THEv′ = 0,1 BANDS OF THEB-X,C-X, ANDE-XSYSTEMS IN FIVE ISOTOPOLOGUES OF CARBON MONOXIDE

2014 ◽  
Vol 788 (1) ◽  
pp. 67 ◽  
Author(s):  
G. Stark ◽  
A. N. Heays ◽  
J. R. Lyons ◽  
P. L. Smith ◽  
M. Eidelsberg ◽  
...  
Keyword(s):  
Carbon Monoxide ◽  
High Resolution ◽  
Oscillator Strength

scholarly journals Giant Molecular Clouds in M33. II. High‐Resolution Observations

2003 ◽  
Vol 599 (1) ◽  
pp. 258-274 ◽  
Author(s):  
E. Rosolowsky ◽  
G. Engargiola ◽  
R. Plambeck ◽  
L. Blitz
Keyword(s):  
High Resolution ◽  
Molecular Clouds ◽  
Giant Molecular Clouds

scholarly journals High resolution spectroscopy of RY Tauri: variability of the Na D line profiles

1990 ◽  
Vol 137 ◽  
pp. 219-220
Author(s):  
P.P. Petrov
Keyword(s):  
High Resolution ◽  
Large Scale ◽  
Young Stars ◽  
High Resolution Spectroscopy ◽  
Line Profiles

Ejection and accretion of gas clouds in the vicinity of RY Tau were discovered. The existense of large scale “stellar prominences” around young stars is suggested.

scholarly journals New Progress in Mode Detection and Identification in δ Scuti Stars by the Analysis of Line Profile Variations

2000 ◽  
Vol 176 ◽  
pp. 463-464
Author(s):  
L. Mantegazza ◽  
E. Poretti ◽  
M. Bossi ◽  
N. S. Nuñez ◽  
A. Sacchi ◽  
...  
Keyword(s):  
High Resolution ◽  
Line Profile ◽  
High Resolution Spectroscopy ◽  
Line Profiles ◽  
Powerful Technique ◽  
Mode Detection ◽  
Detection And Identification ◽  
Scuti Stars ◽  
Δ Scuti Stars ◽  
Nonradial Pulsation

Abstractδ Sct stars are among the most promising targets to perform ground-based asteroseismology. High resolution spectroscopy offers us a powerful technique to identify radial and nonradial pulsation modes, since we can easily detect oscillations and travelling features in the line profiles.

scholarly journals Kinematic Structure and Chemical Composition of the Double Shell PN NGC 3242

1989 ◽  
Vol 131 ◽  
pp. 200-200
Author(s):  
K. C. Sahu ◽  
S. R. Pottasch ◽  
B. G. Anandarao ◽  
J. N. Desai
Keyword(s):  
Chemical Composition ◽  
High Resolution ◽  
Outer Shell ◽  
Expansion Velocity ◽  
Kinematic Structure ◽  
Line Profiles ◽  
Kinematic Study ◽  
Fabry Perot

Kinematic study of the multiple shell PN NGC 3242 was carried out by obtaining Hα and [O III] line profiles at 9 positions of the nebula using a high-resolution (R ≅ 50,000) Fabry-Pérot spectrometer. The positions cover both the bright inner shell and the faint outer shell. It is shown here that the two apparently continuous shells are kinematically separate: the faint outer shell was ejected ∼ 5000 years earlier and has less expansion velocity than the bright inner shell.

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