Fourier transform spectroscopy on very large telescopes

Details Fourier transform spectroscopy on very large telescopes Fourier transform spectroscopy on very large telescopes

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010spie.7735e.229r&link_type=abstract

Ground-based and Airborne Instrumentation for Astronomy III. Edited by McLean, Ian S.; Ramsay, Suzanne K.; Takami, Hideki. Pro

Astronomy and Astrophysics

Astronomy

Scientific paper

While a premier technique for laboratory spectroscopy, Fourier transform (FT) spectroscopy has fallen into disuse in astronomical applications. The speed of a FT spectroscopy is significantly less than that of a dispersive spectrograph with an array detector due to multiplex disadvantage. However, there are a number of advantages of the FT technique that can be exploited to offer spectroscopic capabilities that would otherwise not be available. For very large telescopes these include spectral resolutions significantly in excess of 100000 and 2-D spectral spatial imaging. By using postdispersers with array detectors the speed difference between cryogenic grating and FT spectrographs can be reduced. We explore the possibilities of using pre-existing FT equipment upgraded with modern detectors on next generation telescopes. For specificity, we will adopt as our model FTS at the 4-m Mayall telescope and study how it could be adapted to an ELT, and with what resulting performance.

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