The Haleakala Imaging Vector Magnetograph

Details The Haleakala Imaging Vector Magnetograph The Haleakala Imaging Vector Magnetograph

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.4005m&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #40.05; Bulletin of the American Astronomical Society, Vol. 24, p.793

Astronomy and Astrophysics

Astronomy

Scientific paper

The Imaging Vector Magnetograph, now in daily use at Mees Solar Observatory, Haleakala, Hawaii, extends our capabilities in the measurement of solar vector magnetic fields by providing high spatial and temporal resolution, together with extended area coverage. The instrument is based on a fast-readout CCD camera as its primary detector, a tunable air-spaced Fabry-Perot filter for spectral selection, and variable nematic liquid-crystal retarders for polarization selection. A 28 cm aperture reflecting telescope provides an image the size of a large active region; it is coupled to the magnetograph in a configuration compact enough to mount on the Observatory's 3.6 m equatorial spar. The assembly can be pointed independently of the spar to select a region of interest, so the telescope is always used on-axis. A tip-tilt image stabilizer corrects for image displacement due to spar shake or large-scale atmospheric turbulence. A workstation-based computer control system, incorporating separate processors for user interface, process management and device control, permits accurate process timing along with a flexible user interface. The latter is implemented in an X-windows framework, so that in fact we have found it quite reasonable to operate the instrument from an X terminal at a remote location. The raw data images are stored on 8mm tape for off-line processing, or can be reduced in a few minutes using the instrument's built-in array processor to provide near-real-time magnetograms. Instrument operational parameters can be adjusted in several ways to favor spatial resolution, spatial field, temporal resolution or magnetic sensitivity, but typically we have a 4.5 x 4.5 arcminute field, 1 arcsecond spatial sampling, and an observation interval of five minutes. Initial solar observations showing current capabilities will be presented.

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