Imaging Vector Magnetograph
Papers
The Imaging Vector Magnetograph was on the spar at Mees Solar Observatory
from 1992 - 2010, during which time it obtained many thousands of
polarimetric data sets. In brief, observations in Zeeman-sensitive lines
were made using a 28 cm aperture telescope, a polarizing modulator, and a
tunable Fabry Perot filter. The spectral resolution is approximately
7pm, the spatial resolution approximately 1 arcsec over a field of view
4.7arcmin^2, with a polarimetric precision of at least 0.1%. Two beams are
recorded simultaneously for purposes of registration and (spatial, spectral)
distortion correction post-facto.
Below are links to the IVM instrument papers where full descriptions can
be found.
The IVM is described in the paper:
The Imaging Vector Magnetograph at Haleakala, by
D. L. Mickey, R. C. Canfield, B. J. LaBonte,
K. D. Leka, M. F. Waterson, and H. M. Weber, in
Solar Physics, Volume 168, p. 229, 1996.
An analysis of the IVM system and the correction of the raw
data to form Stokes spectra is given in the paper:
The Imaging Vector Magnetograph at Haleakala II: Reconstruction of Stokes Spectra,
by B. J. LaBonte, D. L. Mickey, and K. D. Leka in Solar Physics,
Volume 189, p. 1, 1999.
Detailed analysis of the IVM characteristics are given by:
Alignment of Fabry-Perot Interferometer Plates in a Solar Vector Magnetograph at Haleakala, by D. L. Mickey in
Solar Physics, Volume 220, pp. 21-27, 2004.
and
The Imaging Vector Magnetograph at Haleakala III:
Effects of Instrumental Scattered Light on Stokes Spectra
by B. J. LaBonte in Solar Physics, Volume 221, pp. 191-207, 2004.
and
The Imaging Vector Magnetograph at Haleakala IV: Stokes Polarization Spectra in the Sodium D1 589.6 nm Spectral Line,
by K. D. Leka, D. L. Mickey, H. Uitenbroek, E. L. Wagner, and T. R. Metcalf,
in Solar Physics, Volume 278, pp. 471-485, 2012.
Last modified: Tue Jun 19 16:35:24 MDT 2012