scholarly journals Galactic HI Mapping and Optical–IR Studies

1997 ◽  
Vol 14 (1) ◽  
pp. 118-119
Author(s):  
R. D. Davies
Keyword(s):  
Interstellar Medium ◽  
Angular Resolution ◽  
Scale Structure ◽  
Resolution Limit ◽  
Ir Studies ◽  
Scale Down

AbstractHI structure is seen at every scale down to the angular resolution limit of all survey telescopes. I present several examples of the structures at high Galactic latitudes with the 12 arcmin beam of the Loveli Telescope, the 2 arcmin resolution of the DRAO synthesis, as well as other indicators of finer scale structure in the interstellar medium (ISM).

scholarly journals Adjective distribution in Modern Mongolian

2016 ◽  
Vol 6 (2) ◽  
pp. 9-22
Author(s):  
Wenchao LI
Keyword(s):  
Scale Structure ◽  
The Other ◽  
Direct Perception ◽  
Resultative Constructions ◽  
Other Hand ◽  
Scale Down ◽  
Scalar Structure ◽  
Closed Scale

This paper discusses adjective distribution in Mongolian based upon the mereological framework: scale structure. It investigates how adjectival complements are sensitive to the scalar structure of adjectival predicates (APs) in resultative constructions as well as direct perception expressions. The findings reveal that Mongolian only tolerates inherent resultatives; derived resultatives are ruled out. The acceptability of adjectival complements in inherent resultatives runs from 'Totally open-scale/Totally closed-scale' down to 'Lower closed/Upper closed-scale'. On the other hand, adjectival complements in direct perception expressions are of no diverse acceptability, i.e. all layers of APs are licensed. Furthermore, durative verbs are likely to yield open-scale APs whilst punctual verbs seem to favour closed-scale APs.

Small-scale-structure of the interstellar medium probed through diffuse band observations

2006 ◽  
Vol 133 ◽  
pp. 403 ◽  
Author(s):  
Martin A. Cordiner ◽  
Stephen J. Fossey ◽  
Arfon M. Smith ◽  
Peter J. Sarre
Keyword(s):  
Interstellar Medium ◽  
Scale Structure ◽  
Small Scale ◽  
Diffuse Band ◽  
Small Scale Structure

scholarly journals Large Scale Structure and Kinematics of the Orion Ridge

1994 ◽  
Vol 140 ◽  
pp. 234-235
Author(s):  
J. J. Wiseman ◽  
P. T. P. Ho
Keyword(s):  
Radial Velocity ◽  
Large Scale ◽  
Angular Resolution ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Hii Region ◽  
Scale Shift

Clumps and filamentary structures have previously been observed in the extended molecular ridge of OMC-1 (see below). The region is affected by multiple outflow components, shock emission that extends 0.5 pc from the BN/KL core, and a foreground HII region expanding into the cloud. The region also displays a complex kinematical character, with a large scale shift in radial velocity along the ridge, multiple cloud velocity components (Womack et al. 1993), and fast gradients across constituent cores (Harris et al. 1983, Wiseman and Ho 1993).To clarify the structure and kinematics of the region, we have used the VLA to observe with high (0.3 km s−1) velocity resolution and high (8”) angular resolution the NH3 (1,1) and (2,2) rotation-inversion lines over 20 adjacent fields covering a 3’ by 8’ region encompassing the KL region.

Contour-crossing statistics for small scale structure on radio polarized intensity maps of the interstellar medium

2009 ◽  
Vol 53 (10) ◽  
pp. 879-885
Author(s):  
I. A. Mizeva ◽  
D. D. Sokoloff ◽  
A. Fletcher ◽  
P.G. Frick ◽  
A. Shukurov
Keyword(s):  
Interstellar Medium ◽  
Scale Structure ◽  
Small Scale ◽  
Small Scale Structure

scholarly journals Interaction of Planetary Nebulae by the Interstellar Medium

1993 ◽  
Vol 155 ◽  
pp. 307-310 ◽  
Author(s):  
K.J. Borkowski
Keyword(s):  
Interstellar Medium ◽  
Large Scale ◽  
Planetary Nebulae ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Motion Studies ◽  
Stellar Motion

Interaction of planetary nebulae (PNe) with the interstellar medium (ISM) is quite common, in accord with our understanding of the large-scale structure of the ISM. The characteristic signature of the interaction is a dipole asymmetry resulting from a distortion and compression of the nebula in the direction of stellar motion. Studies of interacting PNe provide us with information on the structure of the ISM, and on the evolution of old PNe and PN halos.

scholarly journals Galactic Plane Surveys at Low Frequencies

2002 ◽  
Vol 199 ◽  
pp. 251-258
Author(s):  
A.R. Taylor
Keyword(s):  
Interstellar Medium ◽  
Atomic Hydrogen ◽  
Angular Resolution ◽  
Spatial Scales ◽  
High Sensitivity ◽  
Hydrogen Gas ◽  
Dimensional Structure ◽  
High Angular Resolution ◽  
Wide Field ◽  
The Galaxy

Until recently, high angular resolution and high sensitivity surveys of the radio emission from the plane of our Galaxy were available only at frequencies of several GHz, where large single dish radio telescopes provide arcminute scale angular resolution. At these frequencies thermal radiation from HII regions and diffuse ionized gas comprise a major component of the Galactic emission. Advances in wide field interferometric imaging techniques now make it possible to carry out high sensitivity surveys of the Galaxy with arcminute scale angular resolution at 1.4 GHz and below. Over the past few years initial synthesis surveys have been made. More ambitious surveys that combined sensitive continuum observations with full polarimetry and images of the 3-dimensional structure of atomic hydrogen gas at pc scales are currently underway in the northern (DRAO) and southern (ATNF) hemispheres. The interstellar medium of the Galaxy contains structure on all spatial scales, and these surveys combined data from aperture synthesis telescopes and signal dish antennas to provide full spatial frequency coverage to the resolution limit. Preliminary results reveal wide-spread features and processes in the the interstellar medium that are not readily visible by other means, including, for example, unusual atomic hydrogen structures related to the vertical transfer of matter and radiation between the disk and halo of the Galaxy, Faraday rotation structures that allow study of the magnetic field and diffuse ionized component in the plane of the Galaxy, and a cold atomic phase of the neutral medium that may provide a link between global shock phenomena in the galaxy and the formation of molecular clouds.

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