Polarization calibration of the Tandem Etalon Magnetograph of the Solar Magnetic Activity Research Telescope at Hida Observatory
arXiv:2208.10696 · doi:10.1093/pasj/psac072
Abstract
The Tandem Etalon Magnetograph (TEM) is one of the instruments of the Solar Magnetic Activity Research Telescope of Hida Observatory. The TEM is a partial disk (320" x240") filter magnetograph which scans the wavelength around a Fe I line at 6303 angstrom and achieves polarimetric sensitivity of < 5x10^-4 for each wavelength. To obtain the polarimeter response matrix of the instrument, we have carried out end-to-end polarization calibrations of the instrument. We have also measured the polarization characteristics of the polarization beam splitter (PBS), which is a crucial component of the instrument. As a result of end-to-end calibration, we found significant spatial variation in the response matrix across the field of view. From a laboratory test, we found that 1% of the magnitude of a circular diattenuation of the PBS was due to the retardation caused by the stress in the cube and the linear diattenuation of the film. Although the spatial variation across the field of view is more than ten times larger, to achieve the polarimetric sensitivity of < 5x10^-4, this can be well explained by the polarization characteristic of the PBS and corrected by using the response matrix obtained in the end-to-end calibration. In addition, we also obtained the daily variation of the polarization property of the TEM. We found that the crosstalk from Stokes Q to V changes an amount comparable to the tolerance through a day. In the present configuration, we require a pixel-by-pixel calibration every 100 minutes to meet the accuracy requirement.
arXiv comment19 pages, 11 figures. Accepted for the Publications of the Astronomical Society of Japan
References in corpus (19)
- The Solar Optical Telescope for the Hinode Mission: An Overview
- Torus instability
- Magnetic Field Structures Triggering Solar Flares and Coronal Mass Ejections
- Global Forces in Eruptive Solar Flares: The Lorentz force Acting on the Solar Atmosphere and the Solar Interior
- Solar magnetic fields as revealed by Stokes polarimetry
- Study on Triggering Process of Solar Flares Based on Hinode/SOT Observations
- Magnetic fields of an active region filament from full Stokes analysis of Si I 1082.7 nm and He I 1083.0 nm
- Double arc instability in the solar corona
- High-resolution, high-sensitivity, ground-based solar spectropolarimetry with a new fast imaging polarimeter
- Triggering Process of the X1.0 Three-ribbon Flare in the Great Active Region NOAA 12192
- Statistical Study of the Magnetic Field Orientation in Solar Filaments
- An MHD Modeling of Successive X2.2 and X9.3 Solar Flares of 2017 September 6
- A Study of Magnetic Field Characteristics of Flaring Active Region Based on Nonlinear Force-free Field Extrapolation
- Non-potential field formation in the X-shaped quadrupole magnetic field configuration
- Increase in the amplitude of line-of-sight velocities of the small-scale motions in a solar filament before eruption
- Evolution of the Non-potential Magnetic Field in the Solar Active Region 12673 Based on a Nonlinear Force-free Modeling
- Onset Mechanism of M6.5 Solar Flare Observed in Active Region 12371
- Small-scale motions in solar filaments as the precursors of eruptions
- Extrapolation of Three-dimensional Magnetic Field Structure in Flare-productive Active Regions with Different Initial Conditions