The XRT will provide 2-arcsecond resolution images of the highest temperature solar coronal material, from 1,000,000 to 10,000,000 Kelvin.
The EIS will measure ultraviolet spectral lines in two wavelength ranges, spanning plasma temperatures from 100,000 to 20,000,000 Kelvin. These observations will provide measurements of flow velocities (as low as 3 kilometers per second), electron temperatures, and densities from the transition region to the corona.
The 50 cm OTA and the Focal Plane Package (FPP) will make continuous measurements of the photosphere at visible wavelengths. FPP instruments, combined with polarizing optics, will measure photospheric vector magnetic fields with an angular resolution of 0.2 arcseconds (140 km).
The Broadband Filter Imager (BFI) will measure horizontal flows of the photosphere and reveal locations of strong magnetic fields. With its CA II H-line and CN band filters, it will reveal magnetic field structure in the chromosphere.
The Narrowband Filter Imager (NFI) will measure very narrow spectral bands in teh photosphere and chromosphere to derive line-of-sight velocities of solar plasma. Polarizing optics will allow measurement of the magnetic field over a wide field-of-view.
The Spectro-Polarimeter (SP) will record the polarization states of spectral lines, yielding measurements of the three-dimensional magnetic field vector in the photosphere.