Report from the
External Review Committee of the
Pueo-Nui Workshop
held on Mai 22-23, 2003 at
the
Laboratoire
d’Astrophysique - Observatoire de Grenoble.
Contributors:
Christophe
Dumas, (Christophe.Dumas@jpl.nasa.gov)
NASA/Jet
Propulsion Laboratory, Chair
Marc
Ferrari, (Marc.Ferrari@observatoire.cnrs-mrs.fr)
Observatoire
de Marseille
Pierre
Kern, (Pierre.Kern@obs.ujf-grenoble.fr)
Observatoire
de Grenoble
Norbert
Hubin, (nhubin@eso.org)
European
Southern Observatory
Guy
Perrin, (Guy.Perrin@obspm.fr)
Observatoire
de Paris-Meudon
Introduction:
Olivier
Lai and François Ménard, the main organizers of the PUEO-NUI workshop, have
requested that the External Review Committee (1) generates a review of the
discussion presented during the workshop, and (2) provides its view on the
scientific and technical cases for an upgrade of PUEO.
In
order to help in this task, the committee was asked to respond to a series of
specific points about: the science cases for the upgrade of PUEO, the
instruments that could enhance the science results obtained with Pueo-Nui, the
technological & engineering aspects of the upgrade.
The
present document captures these responses and provides a summary of the
comments and suggestions from the review board committee.
A) SCIENCE
1) Are there compelling science cases?
Several
programs, which would all benefit from the upgrade of PUEO, were presented
during the first day of the workshop. Some of them would simply return modest
improvements in regards to the results obtained with the current PUEO system.
Other programs could only be carried-out with PUEO-NUI, like the ability to
image diffuse and extended structures, or to detect faint point sources
(fainter that currently possible with PUEO), within the immediate proximity
(0.5” to a few arcseconds) of bright objects (stars, planets). Overall, the
stability and high-Strehl of the PSF produced by PUEO-NUI in the near-infrared
would return the crispiest images that can be obtained at this wavelength
range. A strong interest to work at shorter wavelengths (I band) was also
demonstrated. At these wavelengths, PUEO-NUI would allow to obtain images with
a more modest Strehl ratio while still producing diffraction limited images at
a resolution of ~40mas at R band (0.65mm). The direct competitor of PUEO-NUI at
visible wavelengths would be the Hubble Space Telescope.
- Solar
system science: PUEO-NUI would allow to search for asteroid satellites
closer-in from the primary (R-I bands), or image diffuse structures like planetary
rings or atmospheric structures at high-contrast (H-K bands).
The
inner systems (ring and satellites) of the giant planets Uranus and Neptune
could also be studied at very high contrast in the near-infrared.
- Galactic:
Near-infrared search for brown-dwarfs and debris disks at higher contrast and
closer-in from the primary (need for coronography).
- Extra-galactic:
QSO and deep-field observations (using nearby bright stars). Observations of
the galactic center (need for near-IR wavefront sensor).
2) Are the science cases compelling and numerous
enough to justify an upgrade?
A
large part of the science programs proposed for PUEO-NUI could be equally
carried-out on large 8-10m class telescopes equipped with AO. The most
compelling cases for an upgrade are those based on the ability for PUEO-NUI to
produce a very stable PSF in the near-infrared range. Such performances will
allow very high dynamic range and would therefore make possible the detection
of low contrast features/objects (atmospheric variability of Uranus and
Neptune, search for asteroid satellites, study of the inner system of the giant
planets, search for brown dwarfs and debris disks). In order to be competitive,
the modifications of current AO system should be implemented rapidly (within
the next 2-3 years), and preferably before the operation of the new generation
of AO systems on 8-10m class telescopes.
B) INSTRUMENTS
1) Is the upgrade of PUEO justified with the
current instrument only (many science cases require instruments not presently
available: e.g. Integral Field Unit for spectroscopy, long-slit spectroscopy,
coronograph)?
The
realization of a fast upgrade of PUEO under a limited budget is in
contradiction with the need for a series of new instruments (coronograph,
low-to-medium spectroscopy, etc). Because it is extremely important for CFHT to
remain at the forefront of the technology in the area of high-angular
resolution and high-contrast imaging, a limited set of improvements of the
actual system focused on the main elements (e. g. deformable mirror, wave front
sensor, real time computer) should be considered during the first phase. This
upgrade would allow better performances than HST in JHK bands (due to its
larger mirror diameter) on bright objects. At shorter wavelengths (R band),
PUEO-NUI would deliver an angular resolution equivalent to a 10-12m telescope
observing in the near-infrared. Science programs like searching for
circumstellar disks or low-mass companions to nearby young stars, or exploring the close vicinity of
main-belt asteroids to search for small (~km size) satellites, could be
successfully investigated with such an instrument.
It
would nevertheless be regretful to limit the science capabilities to direct
imaging only and future instrumentation (team/visitor as well as general public
instruments) should be investigated along with the development of PUEO-NUI.
2) Which new instrument(s) would make the upgrade
very attractive?
In
order to take advantage of the full capabilities in high contrast and high
angular resolution offered by PUEO-NUI, a suite of dedicated instruments (or
upgrades) is strongly recommended. The technical study of these instruments
will have strong high-level requirements on the system (i.e. extreme quality of
the optical elements) and should therefore be identified very early during the
design phase of PUEO-NUI. The list of instruments should include, at least:
-
A
spectrograph returning low-to-medium resolution in the 0.8-2.5mic range
(cross-dispersed), but an upgrade of GRIF to obtain spectroscopic capabilities
at H and K bands would be an acceptable cost-driven compromise.
-
A new generation coronagraph (i.e. with pupil mask in addition to occulting spot).
C) ENGINEERING
1) Are there technological show-stopper? (e.g.
Deformable Mirror)
No
new technology would need to be developed to upgrade PUEO to 105 actuators. The
proposed AO system could be realized using improvements of components from
available technologies. Some recent ESO results from MACAO show the possibility
of improving the performances of PUEO within the applicable time and budget
constraints. Nevertheless, if new technology components with sufficient
performances and reliability become available in a timeframe compatible with
the design phase, the opportunity to integrate them in PUEO-NUI should be
taken. This is particularly important in order to keep the CFHT AO expertise at
the top level with respect to the next generation of AO systems (ELT or 8m
HDR).
2) Is considering the upgrade as a test-bench for
ELT or HDR 8-m compelling? If yes, is it compelling enough to justify an
upgrade?
The
engineering aspects and integration of new technology components for PUEO are
very attractive and compelling when considered as a test-bench for high
dynamics on large telescopes. The engineering validation would include analysis
of the optical quality, stiffness, data transfer speed, etc. Some new software
developments will be required. In this context, PUEO-NUI could be considered as
an intermediate instrument between the current generation of AO systems and the
future Extreme-AO systems. The realization of PUEO-NUI would address important
issues for Extreme-AO, while investigating new concepts for coronography and
related systems like double tip-tilt stage correction or phase mask position
control. PUEO-NUI would also permit exploring specific data processing products
related to second order effect on image degradation. A high order adaptive
optics system may increase the relative contribution of these second order
aberrations to the final optical quality: diffraction, parasitic light due to
optical component diffusion, remaining optical aberration corresponding to high
spatial frequencies (i.e. aberrations corresponding to modulation on smaller
scale than the inter-actuator distance).
Also,
it is important to consider that PUEO-NUI would be the first (and only?)
high-order AO curvature sensing system. Other high-order systems planned for
large telescopes like VLT or Keck are more than likely to be based on a
Shack-Hartmann concept. It is not clear how/what part of the experience
acquired from the upgrade of PUEO could easily be transferred to future
projects on large telescopes since the technology and the staff would be
different.
3) Among the *long* wish list: laser guide star,
larger wavefront sensor field-of-view, infrared wavefront sensor, higher
limiting magnitude, spectroscopy at R~200-400 and R~2000-5000, polarimeter, PSF
suppression techniques (coronagraphy, TRIDENT, etc), tip-tilt sensor (required
for laser guide star), which one are the most needed to justify an upgrade? Are
they feasible?
As
described earlier, coronographic and spectroscopic capabilities should be
considered. Additionally, fainter limiting magnitude (or laser guide star)
would come next in the priority list.
D) SUMMARY
Unique
AO expertise has been acquired at CFHT and the upgrade of PUEO should be
considered as an opportunity to secure and enrich this knowledge for the future
years. Considering the various efforts planned worldwide by other groups (ESO
8m-VLT-PF, Keck 10m-XAO, Palomar 5m-AO, etc) PUEO-NUI is most timely and should
be started as soon as possible in order to make the instruments available at
the telescope no later than 2006. The realization of the upgrade could also be
considered as an intermediate step between the current AO systems and the
future concepts of Extreme Adaptive Optics (although the transfer of knowledge
from PUEO-NUI to the new generation AO systems on large telescopes is unclear).
Some
science projects would benefit from the upgrade of PUEO, although most of the
AO programs could be equally carried-out in the near-infrared on large
telescopes currently equipped with an AO system. The programs that would
benefit the most from the upgrade of PUEO are those requiring a very stable
PSF: detection of faint and low-contrasted features such as searching for
circumstellar disks around young-nearby stars, studying the variability of
planetaary atmospheres, or studying the inner systems of the giant planets
(rings and small satellites).
It
would be regretful to limit the domain of investigation offered by PUEO-NUI to
imaging only. For this reason a minimum suite of instruments (new or upgrades)
is strongly suggested. This would include at a minimum some spectroscopic
capabilities (low-to-medium resolution) and a new generation coronograph.
Improving the limiting magnitude of the system to a lower limit should also be
considered.