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Published on: August 1, 2017
SPIFI: a direct-detection imaging spectrometer for submillimeter wavelengths
C Matt Bradford1, Gordon J Stacey, Mark R Swain
1Department of Astronomy, Cornell University, Ithaca, New York 14853, USA. bradford@submm.caltech.edu
Applied Optics
|May 15, 2002
Summary
The South Pole Imaging Fabry-Perot Interferometer (SPIFI) is a novel submillimeter spectrometer offering high spectral resolution and mapping capabilities. Its sensitivity rivals heterodyne instruments, enabling deep extragalactic observations.
Area of Science:
- Astronomy and Astrophysics
- Instrument Science
- Submillimeter Spectroscopy
Background:
- The submillimeter band is crucial for studying cold dust and gas in the universe.
- Existing instruments often lack the combination of imaging and high spectral resolution.
- Ground-based observations are limited to specific atmospheric windows.
Purpose of the Study:
- To introduce the South Pole Imaging Fabry-Perot Interferometer (SPIFI), a pioneering direct-detection imaging spectrometer.
- To detail the design, motivation, and operational characteristics of SPIFI.
- To highlight SPIFI's advantages for astrophysical research, particularly extragalactic studies.
Main Methods:
- Utilizes a focal plane of 25 silicon bolometers cooled to 60 mK.
- Employs two cryogenic scanning Fabry-Perot interferometers in series with a 60-mK bandpass filter.
- Operates in the 350 and 450 micrometer atmospheric windows with selectable spectral resolving power (500-10,000).
Main Results:
- Achieves sensitivity within a factor of 1.5-3 of the photon background limit.
- Demonstrates performance comparable to the best heterodyne spectrometers.
- Offers large bandwidth and mapping capabilities for efficient sky surveys.
Conclusions:
- SPIFI represents a significant advancement in submillimeter astronomical instrumentation.
- Its unique capabilities are well-suited for deep extragalactic observations and other specialized astrophysical projects.
- The instrument's design and performance characteristics are presented for its operational use on the telescope.
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