Proceedings Article | 19 September 2007
Proc. SPIE. 6693, Techniques and Instrumentation for Detection of Exoplanets III
KEYWORDS: Mirrors, Phase shifts, Planets, Stars, Nulling interferometry, Telescopes, Interferometers, Photons, Manufacturing, Signal to noise ratio
Direct detection and characterization of a planet around a star by nulling interferometry, must be efficient in a large wavelength
domain in order to detect simultaneously the infrared bio-tracers CO2, O3 and H2O. This condition requires that an achromatic phase shift of π be implemented, with an accuracy sufficient for achieving a deep nulling at all considered
wavelengths. Several solutions have been presented. We present here a new concept for designing such an achromatic
phase shifter. It is based on two cellular mirrors (alternatively, transparent plates can be used) where cells have thickness
which are respectively odd and even multiples of a quarter of the central wavelength. Each cell introduces then a phase shift
of (2k + 1)π or of 2kπ, on the fraction of the wave it reflects. Each mirror is introduced in the collimated beam issued from
one or the other telescopes. Because of the odd/even distribution, a destructive interference is obviously produced on axis
for the central wavelength when recombining the two beams. The trick to obtain a quasi-achromatisation is to distribute
the thickness of the cells, so that the nulling is also efficient for a wavelength not too far from the central wavelength.
We show that if the thicknesses are distributed according to the Pascal triangle, a fair quasi-achromatism is reached. This
effect is the more efficient that the number of cells is large. For instance, with 256 × 256 cells, where phase shift range is
between -6π and +6π one shows that the nulling reaches 10-6 on the wavelength range [0.7λ0, 1.3λ0] which corresponds roughly to the DARWIN specification. In a second step, we study the optimum way to distribute the cells in the plane of the
pupil. The most important criterion is the isolation of the planet image from the residual image of the star. Several efficient
configurations are presented. Finally we consider some practical aspects on a device belonging to the real world and on the
bench we are developing. The major interest of this solution is that it allows a compact, simple and fully symmetric design,
with essentially no ajustable sub-systems ; extension to multi-telescopes interferometers with phase shift other than π can
also be envisioned.
