We present the current status of the development of the SPICA Coronagraph Instrument (SCI). SPICA is a next-generation
3-meter class infrared telescope, which will be launched in 2022. SCI is high-contrast imaging, spectroscopic
instrument mainly for direct detection and spectroscopy of extra-solar planets in the near-to-mid infrared wavelengths to
characterize their atmospheres, physical parameters and evolutionary scenarios. SCI is now under the international
review process. In this paper, we present a science case of SCI. The main targets of SCI, not only for direct imaging but
also for spectroscopy, are young to matured giant planets. We will also show that some of known exoplanets by ground-based
direct detection are good targets for SCI, and a number of direct detection planets that are suitable for SCI will be
significantly increased in the next decade. Second, a general design of SCI and a key technology including a new high-throughput
binary mask coronagraph, will be presented. Furthermore, we will show that SCI is potentially capable of
achieving 10 -6 contrast by a PSF subtraction method, even with a telescope pointing error. This contrast enhancement
will be important to characterize low-mass and cool planets.

SPICA coronagraph instrument: characterization of atmospheres and physical parameters of giant planets by direct imaging and spectroscopy

We describe the principles and potential of Color-Differential Astrometry (CDA), a high-resolution technique easily
implementable on the Science Coronographic Instrument (SCI) of the SPICA satellite, and aimed here at the direct
detection and spectroscopy of giant Extrasolar Planets (ESP). By measuring the photocentre of the source diffraction
pattern relatively between dispersed spectral channels, CDA gives access to flux ratio and angular information well
beyond the telescope resolution limit. Applied to known ESPs, it can yield the inclination (thus the mass) and spectrum
of the planet. Our estimates show that low-resolution spectroscopy of Jupiter-radius ESP can be measured within a few
hours for planets at orbital distances ranging from 0.05 AU to a few AUs, thus complementing the detection range
expected using the coronographic measurements. More generally, it may also apply to any unresolved source with some
wavelength-dependent asymmetry.
In addition to the ESP cases considered for the scientific signal and to their associated fundamental noises, we also
present the instrumental effects and a dedicated optical testbench. The combined effects of several instrumental noise
sources can be introduced into our numerical model (pointing errors, beam tip-tilt, optical aberations, variations of the
detector gain table), and then confronted to measurements from the experimental testbench.

High-resolution and high-precision color-differential astrometry for direct spectroscopy of extrasolar planets onboard SPICA: science and validation experiment

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High-resolution and high-precision color-differential astrometry for direct spectroscopy of extrasolar planets onboard SPICA: science and validation experiment