SODISM II plate-scale for different wavelengths.
|Wavelength [nm]||Optical thickness [mm]||TPS||ACPS||SRPS||SRPS–ACPS|
|393.37||12.328||1.060818||1.061076||1.061102||2.63 × 10-5|
|535.7 (a)||12.297||1.060792||1.061057||1.061060||2.75 × 10-6|
|535.7 (b)||12.303||1.060796||1.061061||1.061064||2.92 × 10-6|
|607.1||12.225||1.060757||1.061016||1.061025||9.42 × 10-6|
|782.2||12.341||1.060781||1.061083||1.061049||− 3.40 × 10-5|
|1025.0||12.080||1.060679||1.060931||1.060947||1.54 × 10-5|
Notes.The optical thickness column corresponds to a characterization of the different filters. SODISM II interference filters do not have the same optical thickness (index, thickness of optical elements used, etc.). Thus, each wavelength has its own plate-scale correction factor. Theoretical plate-scales (TPS in arcsec pixel-1) are obtained from an optical model using the appropriate optical configuration. Angular calibration plate-scales (ACPS in arcsec pixel-1) are obtained during specific campaigns on star doublets. SODISM reference plate-scales (SRPS in arcsec pixel-1) are obtained from the knowledge of the solar radius measured by SODISM at 607.1 nm during the Venus transit. Six digits of the TPS, ACPS, and SRPS entries are significant.
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