Proceedings Article | 14 November 2014
Jean-François Sauvage, Thierry Fusco, Cyril Petit, David Mouillet, Kjetil Dohlen, Anne Costille, Jean-Luc Beuzit, Andrea Baruffolo, Markus Kasper, Marcos Suarez Valles, Mark Downing, Philippe Feautrier, Laurent Mugnier, Pierre Baudoz
KEYWORDS: Optical spheres, Turbulence, Sensors, Spatial filters, Stars, Adaptive optics, Coronagraphy, Point spread functions, Exoplanets, Spatial frequencies
SPHERE instrument [1] (Spectro-Polarimetry High-contrast Exoplanet Research) is a second generation ESO
instrument dedicated to high contrast imaging, and exoplanet direct detection and characterisation. The
overall performance of XAO system of SPHERE, as well as the optimal control law for turbulence correction,
are presented in dedicated papers [5,6]. The global performance of the instrument and of all observing modes
of SPHERE is done in [4].
The strategy of Wave-front Sensing [WFS] in SPHERE relies on two faces, and is thoroughly discussed in
this paper.
Firstly, extreme adaptive optics (XAO) is required for both turbulence and quasi-static pattern compensation.
Particularly, the high frame rate and large subaperture numbers of the Shack-Hartmann WFS allows SAXO to
optimally measure and compensate for atmospherical turbulence. Moreover, the spatial filtering [7,8] allows
one to deepen the contrast curve, and is automatically adjusted on turbulence level to provide the best
performance. Finally, a dedicated calibration procedure based on focal-plane wave-front sensing is optimized
for NCPA compensation on the coronagraphic device, ensuring the best compensation of quasi-static speckle.
Secondly, a high robustness to faint magnitude guide star allows SAXO to address a large panel of targets for
exoplanet detection and characterization. This is only made possible by the joint use of a dedicated Wave-
Front Sensing for turbulence, EMCCD detector capability, and adaptation of the system to the star magnitude.
The noise propagation has been carefully monitored and optimized. The weighted center of gravity gives an
optimal trade-off between performance with respect to noise, and complexity of implementation. The use of
an EMCCD detector allows a powerful noise reduction on the wave-front sensor detector. And finaly, 5
SAXO observing modes are defined in order to cover all star magnitudes up to 16, with systematic optimal
performance. During the whole assembly integrations and test period, choices have been done to optimise the
trade-off between performance, robustness, and simplicity of use. The self-adaptation and auto-calibration of
the instrument has been a strong investment, as well as developing a great simplicity of use. We describe here
the actions taken to reach this level of operation for SPHERE. Finally, perspective are withdrawn for
improving the strategy of WFS in the framework of future XAO instrumentations in E-ELT.
