Millimeter and Submillimeter Wavelength Telescopes

Attenuation Measurement of Very Low-Loss Dielectric Waveguides by the Cavity Resonator Method in the Millimeter/Submillimeter Wavelength Range

10.21236/ada206458 ◽

1989 ◽

Author(s):

F. I. Shimabukuko ◽

C. Yeh

Keyword(s):

Wavelength Range ◽

Cavity Resonator ◽

Dielectric Waveguides ◽

Low Loss ◽

Submillimeter Wavelength ◽

Attenuation Measurement ◽

Resonator Method

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Extension of Electric Resonance Spectroscopy to the Submillimeter Wavelength Region

1976 International Conference on Submillimeter Waves and Their Applications ◽

10.1109/icswa.1976.9350062 ◽

1976 ◽

Author(s):

J. J. Gallagher ◽

W. M. Perm

Keyword(s):

Wavelength Region ◽

Resonance Spectroscopy ◽

Electric Resonance ◽

Submillimeter Wavelength

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Obtaining precise constants of atmospheric lines in the millimeter and submillimeter wavelength ranges

Radiophysics and Quantum Electronics ◽

10.1007/s11141-008-9074-y ◽

2008 ◽

Vol 51 (9) ◽

pp. 713-717 ◽

Cited By ~ 6

Author(s):

M. Yu. Tretyakov ◽

G. Yu. Golubiatnikov ◽

V. V. Parshin ◽

M. A. Koshelev ◽

A. F. Krupnov

Keyword(s):

Submillimeter Wavelength

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Microstrip-stabilized semiconductor quantum-well generator for millimeter and submillimeter wavelength range

10.1117/12.262783 ◽

1996 ◽

Author(s):

Alexandr L. Karuzskii ◽

V. A. Dravin ◽

A. S. Ignatyev ◽

A. E. Krapivka ◽

Yu. A. Mityagin ◽

...

Keyword(s):

Quantum Well ◽

Wavelength Range ◽

Submillimeter Wavelength ◽

Semiconductor Quantum Well

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The Circumstellar Environment of Embedded Massive Stars

Highlights of Astronomy ◽

10.1017/s1539299600013083 ◽

2002 ◽

Vol 12 ◽

pp. 143-145 ◽

Cited By ~ 1

Author(s):

Lee G. Mundy ◽

Friedrich Wyrowski ◽

Sarah Watt

Keyword(s):

Massive Star ◽

Massive Stars ◽

Low Mass Stars ◽

Submillimeter Wavelength ◽

Star Forming ◽

Star Forming Regions ◽

Low Mass ◽

Circumstellar Environments ◽

Near Future

Millimeter and submillimeter wavelength images of massive star-forming regions are uncovering the natal material distribution and revealing the complexities of their circumstellar environments on size scales from parsecs to 100’s of AU. Progress in these areas has been slower than for low-mass stars because massive stars are more distant, and because they are gregarious siblings with different evolutionary stages that can co-exist even within a core. Nevertheless, observational goals for the near future include the characterization of an early evolutionary sequence for massive stars, determination if the accretion process and formation sequence for massive stars is similar to that of low-mass stars, and understanding of the role of triggering events in massive star formation.

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