Small-Scale Structure of the Mon R2 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.

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The Relationship Between Gas and Cirrus Dust Filaments at the Edge of the Expanding Shell in Eridanus

Symposium - International Astronomical Union ◽

10.1017/s0074180900240771 ◽

1990 ◽

Vol 139 ◽

pp. 235-236

Author(s):

G. L. Verschuur ◽

F. Verter ◽

L. J. Rickard ◽

D. T. Leisawitz

Keyword(s):

High Resolution ◽

Surface Brightness ◽

Neutral Hydrogen ◽

Scale Structure ◽

Small Scale ◽

Molecular Gas ◽

Small Scale Structure ◽

Point To Point ◽

The Relationship ◽

Co Observations

At the boundary of a large expanding shell in Eridanus around l = 187°, b = −50° the morphology observed in the HI emission is well mimicked by the 100 μm surface brightness but with associated structures offset by as much as 0.°5. A point-to-point comparison between I100μm and NHI in filaments of neutral hydrogen and dust (IR cirrus) produces only a weak dependence. However, when I100μm at a cirrus dust peak is compared with NHI at the associated H i peak, a relationship closer to that reported by other workers is found. Preliminary CO observations have set low limits on the molecular gas in these filaments. Since the H i and dust in our region are associated with a large expanding shell (or superbubble), shocks may be responsible for separation of gas and dust. The existence of small-scale structure in both the HI and IR is noted. We conclude that attempts to correlate HI and IR must invoke high-resolution area surveys.

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Small-scale structure of the Taurus molecular clouds Turbulence in Heiles' Cloud 2

The Astrophysical Journal ◽

10.1086/164930 ◽

1987 ◽

Vol 312 ◽

pp. 837 ◽

Cited By ~ 26

Author(s):

S. C. Kleiner ◽

R. L. Dickman

Keyword(s):

Molecular Clouds ◽

Scale Structure ◽

Small Scale ◽

Small Scale Structure

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Chemistry and small-scale structure of diffuse and translucent clouds

Symposium - International Astronomical Union ◽

10.1017/s0074180900239478 ◽

1991 ◽

Vol 147 ◽

pp. 139-150

Author(s):

John H. Black ◽

Ewine F. van Dishoeck

Keyword(s):

Molecular Clouds ◽

Column Density ◽

Scale Structure ◽

Small Scale ◽

Interstellar Chemistry ◽

Small Scale Structure ◽

Chemical Stratification

The small, thin diffuse and translucent molecular clouds are excellent laboratories for studying the ways in which small—scale structure and interstellar chemistry affect each other. Variations of density or column density and chemical stratification can be found on scales as small as 0.01 pc. The origin of such structures and the evolutionary states of small clouds remain elusive.

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