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Mid-infrared Lines as Astrophysical Diagnostics: Two Decades of Problems and Promise

  • Sara C. Beck
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Abstract

I arrived in Berkeley in August 1976 with an introduction to Charles Townes from my undergraduate advisor, 70 dollars, and the idea that 0.9 μm was pretty far into the infrared. Forty-eight hours later I was at Lick Observatory with John Lacy and Fred Baas and a large and unwieldy spectrometer, looking for an ionic species ([NeII]) I had never heard of, at a wavelength (12.8 μm) that seemed unimaginably long. And in complete disregard for all my preconceptions the [Nell] came booming in so strongly from every HII region we looked at that we could see it on the voltmeter. That first venture into the middle-infrared convinced me that it was the spectral region of the future, and although there have been ups and downs in the last two decades I still think so.

Keywords

Planetary Nebula Metal Abundance Infrared Space Observatory Very Large Array Stellar Temperature 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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References

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    S. C. Beck, in The Nearest Active Galaxies, Beckman, Colina, and Netzer (eds.), CSIC Madrid, pl69(1993).Google Scholar
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    S. C. Beck, and R. S. Sutherland, submitted to AJ (1995).Google Scholar
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  4. D. K. Aitken, P. F. Roche, M. C. Allen, and M. M. Phillips, MNRAS 199, 31p (1982).Google Scholar
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    S. C. Beck, J. T. Turner, P. T. P. Ho, J. H. Lacy, and D. M. Kelly, submitted to ApJ (1995).Google Scholar

Copyright information

© Springer-Verlag New York, Inc. 1996

Authors and Affiliations

  • Sara C. Beck

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