High‐Resolution Observations of the Molecular Clouds in the NGC 1333 IRAS 4 Region

2001 ◽  
Vol 553 (1) ◽  
pp. 219-226 ◽  
Author(s):  
Minho Choi
Keyword(s):  
High Resolution ◽  
Molecular Clouds

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.

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 Molecular Superclouds in M51

1994 ◽  
Vol 140 ◽  
pp. 353-354 ◽  
Author(s):  
T. Tosaki ◽  
R. Kawabe ◽  
Y. Taniguchi
Keyword(s):  
High Resolution ◽  
Molecular Clouds ◽  
Spiral Galaxies ◽  
Molecular Gas ◽  
Giant Molecular Clouds

Recently, it has been shown that some of nearby spiral galaxies have very massive (107-8Mʘ) and large (several 100 pc - ~ 1 kpc) molecular gas clouds (M51: Rand & Kulkarni 1990; NGC1068: Planesas et al. 1991). Since these clouds are significantly more massive and larger than those of so-called Giant Molecular Clouds (GMCs) found in our Galaxy, they are called Molecular Super-clouds (Rand & Kulkarni 1990; hereafter MSCs). In order to study observational properties of MSCs, we present the results of high-resolution (4”) 12CO(J=1-0) mosaic mapping of central 2.’5 region of the Sbc galaxy M51 using the Nobeyama Millimeter Array (NMA). Our main results are summarized in the followings (Tosaki, Kawabe & Taniguchi 1992).

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

High-resolution maps of 6 centimeter formaldehyde - Clumping in molecular clouds

1985 ◽  
Vol 299 ◽  
pp. 386 ◽  
Author(s):  
J. Martin-Pintado ◽  
T. L. Wilson ◽  
C. Henkel ◽  
K. J. Johnston
Keyword(s):  
High Resolution ◽  
Molecular Clouds

scholarly journals Small-Scale Structure of the Mon R2 Cloud Core

1994 ◽  
Vol 140 ◽  
pp. 266-267
Author(s):  
TH. Henning ◽  
R. Chini ◽  
W. Pfau
Keyword(s):  
Star Formation ◽  
High Resolution ◽  
Formation Process ◽  
Molecular Clouds ◽  
Scale Structure ◽  
Small Scale ◽  
Small Scale Structure ◽  
Ir Sources ◽  
Cloud Core

High-resolution mm continuum observations are especially well suited to detect clumpy structures in molecular clouds. In this paper we concentrate on the Mon R2 cloud core which is associated with a cluster of IR sources. Walker et al. (1990) made a 1.3 mm map with 30″ resolution. They found an unresolved and elongated structure extending from NE to SW. Here, we discuss high-resolution continuum maps at 870 and 1300 µm showing a rich clumpy structure on the scale of several 10 arcsec. The clumps are probably intimately linked to the star formation process in Mon R2.

scholarly journals 4.14. Molecular shell formation by supernova remnants in the Galactic center—what we learn from the case of W44

1998 ◽  
Vol 184 ◽  
pp. 195-196
Author(s):  
Masumichi Seta ◽  
Gisbert Winnewisser ◽  
Tetsuo Hasegawa ◽  
Glenn J. White ◽  
Tomoharu Oka
Keyword(s):  
High Resolution ◽  
Molecular Clouds ◽  
Supernova Remnants ◽  
Galactic Center ◽  
Shell Structures ◽  
Shell Formation ◽  
Considerable Fraction ◽  
Good Place

Recent high resolution CO images of the Galactic center (GC) molecular clouds reveal many arc and/or shell structures (Oka et al. 1997). A considerable fraction of them may most probably be formed by an interaction between supernova remnants (SNRs) and molecular clouds. Studies of such cases in less confused areas are needed to clarify this picture. The SNR W44 is a good place for examining the SNR induced shell formation scenario.

scholarly journals High Resolution Studies of Star-Forming Molecular Clouds

1987 ◽  
pp. 329-330
Author(s):  
A. I. Sargent ◽  
N. Z. Scoville ◽  
C. R. Masson ◽  
K. Y. Lo ◽  
T. G. Phillips
Keyword(s):  
High Resolution ◽  
Molecular Clouds ◽  
Star Forming
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