Proposed conversion of the McMath telescope to 4.0 meter aperture for solar observations in the IR

Details Proposed conversion of the McMath telescope to 4.0 meter aperture for solar observations in the IR Proposed conversion of the McMath telescope to 4.0 meter aperture for solar observations in the IR

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991spie.1494..498l&link_type=abstract

IN: Space astronomical telescopes and instruments; Proceedings of the Meeting, Orlando, FL, Apr. 1-4, 1991 (A92-45151 19-89). Be

Astronomy and Astrophysics

Astronomy

Infrared Telescopes, Metal Surfaces, Mirrors, Optical Measuring Instruments, Solar Optical Telescope, Optical Tracking, Proposals, Tracking (Position)

Scientific paper

Located on a 2076 m summit in Arizona, the present all-reflective McMath optical system consists of a 2.0-m CERVIT flat mounted as a heliostat to follow the sun, a 1.6-m 86.4 m focal-length quartz concave positioned within an inclined underground tunnel, and a 1.5-m CERVIT flat which directs the image to different fixed instrument stations. The building is adequate to accommodate a 6.0-m tracking feed and a 4.0-m concave, resulting in an f/22 beam. A 4.0 m aperture is desirable for adequate flux and resolution at 12 microns where a number of Zeeman sensitive atomic lines are found, lines which are a diagnostic for solar magnetism. At 12 microns, the diffraction limit is 0.75 arcsec, and this resolution might be realized a significant fraction of time because of improved seeing at these IR wavelengths. Direct vector measurements of solar magnetic fields would become possible because effective Zeeman splitting is proportional to wavelength, both the linear and circular Stokes amplitudes are proportional to their vector field components, and instrumental polarization becomes negligible at 12 microns. The telescope would also be used at night by the solar/stellar community.

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