Optical Performance of the Solar Optical Telescope aboard HINODE

Details Optical Performance of the Solar Optical Telescope aboard HINODE Optical Performance of the Solar Optical Telescope aboard HINODE

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9402s&link_type=abstract

American Astronomical Society Meeting 210, #94.02; Bulletin of the American Astronomical Society, Vol. 39, p.217

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The Solar Optical Telescope (SOT) carried by HINODE was designed to perform a high-precision polarimetric observation of the Sun in visible light spectra with a spatial resolution of 0.2 - 0.3 arcseconds. The SOT is a sophistcated instrument and consists of two separate optical parts; the Optical Telescope Assembly (OTA) which is 50 cm aperture Gregorian telescope feeding the light into following observing instruments which is called the focal plane package (FPP) made of two filtergraphs and a spectro-polarimeter. The performance of the OTA is important because a spatial resolution and its temporal stability is mainly determined by this component. To keep the OTA in moderate temperature and optical thermal deformation small, it equipped newly designed components such as a heat dump and a secondary field stop aluminum mirror with high reflectivity silver coating and a temperature low-sensitive apochromatic collimataing lens unit with a UV/IR cut coating on the first surface. In addition, the SOT has an active image stabilization system consisting of correlation tracker, tip-tilt mirror and its controller against satellite pointing jitter. It was confirmed that this system freezes residual motion to the 0.01 arcsecond level on orbit. The image of sub-arcsecond G-band (430.5 nm) bright points clearly indicates that the SOT achieves the diffraction-limit on orbit; this is also confirmed using a phase diversity method. In this paper, we describe details of the design and on-orbit performance of the OTA.

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