Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

Figure 11.2: NAOS-CONICA image of the double star GJ 263 for which the angular distance between the two
components is only 0.030 arcsec. The raw image, as directly recorded by CONICA, is shown in the middle, with
a computer-processed (using the ONERA MISTRAL myopic deconvolution algorithm) version to the right. The
recorded Point-Spread-Function (PSF) is shown to the left. The CONICA pixel scale of 0.01325 arcsec/pixel
was used with the FeII filter (1.257 µm). The exposure time was 10 seconds. This image was obtained during
the NAOS/CONICA commissioning run in November 2003.
Following presentations of the results of our phase A study to an ESO-appointed Review Board in December
2004 and to the ESO Scientific and Technical Committee in April 2005, our proposal has been recommended for
phase B. We are currently preparing the contract for this phase B with ESO and also considering the possibility
to include members of the competing team in order to broaden the capabilities of the Planet Finder instrument.
First light of the Planet Finder is foreseen to occur by end of 2009 or beginning of 2010.
11.1.3 Instrumental Research and development activities
DEFORMABLE MICRO-MIRRORS
The LAOG R&D activities in adaptive optics are focused on the development of new deformable mirrors for the
next generation of AO systems. The goal is two-fold: i/ obtain smaller and cheaper mirrors for astronomical
applications such as AO systems for interferometry, Multi-Object Adaptive Optics (MOAO) systems, etc., or
for non astronomical applications like ophthalmology, laser beam shaping, telecommunications; ii/ manufacture
mirrors with several thousands actuators for astronomical applications in the fields of eXtreme AO, AO systems
for the Extremely Large Telescopes (ELT), etc. These innovative works lead to three patents and two technology
transfer during the 2001-2005 period (see 14.3).
Magnetic deformable mirrors This technology is particularly well adapted to the production of low order,
large stroke mirrors, therefore allowing to correct all wavefront errors without the need for the usual second tiptilt
stage. These mirrors will for instance be used for interferometry, MOAO, ophthalmology, laser beam shaping,
etc. We have already produced several 52-actuator devices (Figure 11.3), including their control electronics,
and we are now offering these devices through two commercial partners (see below and in section 14.3). Further
developments are considered in order to increase the number of actuators up to 400. The typical characteristics
of these mirrors are given below:
• the minimum actuator step is 2 mm with the current technology
• the typical best-flat surface is ∼ 5 nm RMS (mirror surface)
• typical strokes for the low order modes range from 10 to 15 µm (possibly up to 100 µm)
• the linearity remains below 2% for large strokes (below 1% for +/- 5 µm stroke)
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