Astronomy is at a turning point in its history and in its relations with the Indigenous peoples who are the generational stewards of land where several of our main observatories are located. The controversy regarding the further development of astronomy facilities on Maunakea is probably the most significant and publicized conflict about the use of such land in the name of science. Thousands have stood in resistance, elders were arrested, and the community is divided. Astronomy’s access to one of its most emblematic sites is at risk. This situation challenges our professional practice, the projects we build on Indigenous lands, and our relationships with the people who live within these lands and with society in general. This paper attempts to share the perspective of the authors on the historical events, including the very recent past, through the lens of our understanding and opinions; to provide transparency, with humility, into our process of introspection and transformation; and to share our hopes and ambitions as leaders from Maunakea Observatories for the future of astronomy in Hawaiʻi, as advocated by the Astro2020 report from the U.S. National Academies of Sciences, Engineering, and Medicine; and to suggest ways for the profession to commit to this long-term vision.
MOSAIC is a multi-object spectrograph planned to be installed on the ESO-Extremely Large Telescope. The project is approved to start its phase B in September/October 2022. The main science cases addressed by MOSAIC go from the study of faint stars in the Milky Way and in the local group, to the study of dark matter, galaxy evolution and first-light objects at the epoch of reionisation. The MOSAIC instrument offers Multi-Object Spectroscopy and Integral Field Units capabilities from the visible (VIS) to the near-infrared (NIR). The Laboratoire d’Astrophysique de Marseille is responsible for the development of the near infrared spectrograph. More precisely, it is in charge of the global architecture and design of the NIR spectrograph (optical, mechanical, thermal) and the assembly, integration, tests and verification (AIT/V) activities in cryogenic environment. In this article, the main tradeoffs in terms of optical and mechanical architectures are analyzed; the main technical choices are justified according to the science requirements (from which technical requirement specifications are derived) and the level of maturity of key critical technologies. The NIR spectrograph will be described in terms of system engineering approach. The requirement flow-down strategy, from high-level requirements at the system level toward technical specifications at the module and component levels will be presented. The main interfaces and the development philosophy (with an emphasis on the AIT/V plan) will also be included.
MOSAIC, the multi-object spectrograph (MOS) for the ESO 39m European Extremely Large Telescope (ELT), will combine visible and near-infrared observations with multi-object and multi-integral field spectroscopy capabilities. It will cover a wide panel of topics, from resolved stars up to the most distant galaxies. In the frame of the NIR spectrograph unit realization led by the Laboratoire d’Astrophysique de Marseille (LAM), this paper presents the ongoing development of a cryogenic (90-130 K) NIR camera prototype tested in the 0.77-1.063 µm wavelengths (I band) detailing the opto-mechanical design and the integration and verification strategies in accordance with validation in relevant environment (ESO TRL5).
MOSAIC is the Muti-Object Spectrograph for the ESO Extremely Large Telescope. The Laboratoire d’Astrophysique de Marseille (LAM) is in charge of the instrument “Assembly, Integration, Test and Verification (AIT/V)” phases. AITV for AO instruments, in laboratory as in the telescope, always represent numerous technical challenges. We already started the preparation and planning for the instrument level AIT activities, from identification of needs, challenges, risks, to defining the optimal AIT strategy. In this paper, we present the state of this study and describe several AIT/V scenarios and a planning for AIT phases in Europe and in Chile. We also show our capacity, experience and expertise to lead the instrument MOSAIC AIT/V activities.
MOSAIC is the Multi-Object Spectrograph for the ESO Extremely Large Telescope, approved to enter Phase B beginning 2022. It is conceived as a multi- purpose instrument covering the Visible and Near Infrared bandwidth (0.45 –1.8 μm) with two observing modes: spatially resolved spectroscopy with 8 integral field units; and the simultaneous observation of 200 objects in the VIS and NIR in unresolved spectroscopy.
We present an overview of the main MOSAIC science drivers and the actual baseline design for the instrument. The prototyping and developments undertaken by the consortium to evaluate the feasibility of the project are also discussed.
The recently commissioned Dark Energy Spectroscopic Instrument (DESI) will measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 sqdeg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope delivers light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. A consortium of Aix-Marseille University (AMU) and CNRS laboratories (LAM, OHP and CPPM) together with LPNHE (CNRS, IN2P3, Sorbonne Université and Université de Paris) and the WINLIGHT Systems company based in Pertuis (France), were in charge of integrating and validating the performance requirements of the ten full spectrographs, equipped with their cryostats, shutters and other mechanisms. We present a summary of our activity which allowed an efficient validation of the systems in a short-time schedule. We detail the main results. We emphasize the benefits of our approach and also its limitations.
We present the consolidated scientific case for multi-object spectroscopy with the MOSAIC concept on the European ELT. The cases span the full range of ELT science and require either ‘high multiplex’ or ‘high definition’ observations to best exploit the excellent sensitivity and wide field-of-view of the telescope. Following scientific prioritisation by the Science Team during the recent Phase A study of the MOSAIC concept, we highlight four key surveys designed for the instrument using detailed simulations of its scientific performance. We discuss future ways to optimise the conceptual design of MOSAIC in Phase B, and illustrate its competitiveness and unique capabilities by comparison with other facilities that will be available in the 2020s.
Assembly, Integration, Test and Validation (AIT/V) phases for AO instruments, in laboratory as in the telescope, represent numerous technical challenges. The Laboratoire d’Astrophysique de Marseille (LAM) is in charge of the AIT/V preparation and planning for the MOSAIC (ELT-MOS) instrument, from identification of needs, challenges, risks, to defining the optimal AIT strategy for this highly modular and serialized instrument. In this paper, we present the status of this study and describe several AIT/V scenarios as well as a planning for AIT phases in Europe and in Chile. We also show our capabilities, experience and expertise to lead the instrument MOSAIC AIT/V activities.
Following a successful Phase A study, we introduce the delivered conceptual design of the MOSAIC1 multi-object spectrograph for the ESO Extremely Large Telescope (ELT). MOSAIC will provide R~5000 spectroscopy over the full 460-1800 nm range, with three additional high-resolution bands (R~15000) targeting features of particular interest. MOSAIC will combine three operational modes, enabling integrated-light observations of up to 200 sources on the sky (high-multiplex mode) or spectroscopy of 10 spatially-extended fields via deployable integral-field units: MOAO6 assisted high-definition (HDM) and Visible IFUs (VIFU). We will summarise key features of the sub-systems of the design, e.g. the smart tiled focal-plane for target selection and the multi-object adaptive optics used to correct for atmospheric turbulence, and present the next steps toward the construction phase.
The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 deg² will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. A consortium of Aix-Marseille University (AMU) and CNRS laboratories (LAM, OHP and CPPM) together with LPNHE (CNRS, Universities Pierre et Marie Curie and Paris-Diderot) and the WINLIGHT Systems company based in Pertuis (France), are in charge of integrating and validating the performance requirements of the full spectrographs. This includes the cryostats, shutters and other mechanisms. The first spectrograph of the series of ten has been fully tested and the performance requirements verified for the following items: focus, image quality, straylight, stability, detector properties and throughput. We present the experimental setup, the test procedures and the results.
When combined with the huge collecting area of the ELT, MOSAIC will be the most effective and flexible Multi-Object Spectrograph (MOS) facility in the world, having both a high multiplex and a multi-Integral Field Unit (Multi-IFU) capability. It will be the fastest way to spectroscopically follow-up the faintest sources, probing the reionisation epoch, as well as evaluating the evolution of the dwarf mass function over most of the age of the Universe. MOSAIC will be world-leading in generating an inventory of both the dark matter (from realistic rotation curves with MOAO fed NIR IFUs) and the cool to warm-hot gas phases in z=3.5 galactic haloes (with visible wavelenth IFUs). Galactic archaeology and the first massive black holes are additional targets for which MOSAIC will also be revolutionary. MOAO and accurate sky subtraction with fibres have now been demonstrated on sky, removing all low Technical Readiness Level (TRL) items from the instrument. A prompt implementation of MOSAIC is feasible, and indeed could increase the robustness and reduce risk on the ELT, since it does not require diffraction limited adaptive optics performance. Science programmes and survey strategies are currently being investigated by the Consortium, which is also hoping to welcome a few new partners in the next two years.
KEYWORDS: Adaptive optics, Spectrographs, Telescopes, James Webb Space Telescope, Adaptive optics, Galactic astronomy, Molybdenum, K band, Space telescopes, Near infrared, Spectral resolution
There are 8000 galaxies, including 1600 at z ≥ 1.6, which could be simultaneously observed in an E-ELT field of view of 40 arcmin2. A considerable fraction of astrophysical discoveries require large statistical samples, which can only be obtained with multi-object spectrographs (MOS). MOSAIC will provide a vast discovery space, enabled by a multiplex of 200 and spectral resolving powers of R=5000 and 20000. MOSAIC will also offer the unique capability of more than 10 `high-definition' (multi-object adaptive optics, MOAO) integral-field units, optimised to investigate the physics of the sources of reionization. The combination of these modes will make MOSAIC the world-leading MOS facility, contributing to all fields of contemporary astronomy, from extra-solar planets, to the study of the halo of the Milky Way and its satellites, and from resolved stellar populations in nearby galaxies out to observations of the earliest ‘first-light’ structures in the Universe. It will also study the distribution of the dark and ordinary matter at all scales and epochs of the Universe. Recent studies of critical technical issues such as sky-background subtraction and MOAO have demonstrated that such a MOS is feasible with state-of-the-art technology and techniques. Current studies of the MOSAIC team include further trade-offs on the wavelength coverage, a solution for compensating for the non-telecentric new design of the telescope, and tests of the saturation of skylines especially in the near-IR bands. In the 2020s the E-ELT will become the world's largest optical/IR telescope, and we argue that it has to be equipped as soon as possible with a MOS to provide the most efficient, and likely the best way to follow-up on James Webb Space Telescope (JWST) observations.
The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryon Acoustic Oscillation probe. The KPNO Mayall telescope will deliver light to 5000 fibers feeding ten broadband spectrographs. A consortium of Aix-Marseille University (AMU) and CNRS laboratories (LAM, OHP and CPPM) together with the WINLIGHT Systems company (Pertuis-France) has committed to integrate and validate the performance requirements of the full spectrographs, equipped with their cryostats, shutters and other mechanisms. An AIT plan has been defined and dedicated test equipment has been designed and implemented. This equipment simulates the fiber input illumination from the telescope, and offers a variety of continuum and line sources. Flux levels are adjustable and can illuminate one or several fibers along the test slit. It is fully remotely controlled and interfaced to the Instrument Control System. Specific analysis tools have also been developed to verify and monitor the performance and stability of the spectrographs. All these developments are described in details.
KEYWORDS: Space telescopes, Spectrographs, Spectroscopes, Telescopes, Galactic astronomy, K band, Spectral resolution, James Webb Space Telescope, Visible radiation, Sensors
Building on the comprehensive White Paper on the scientific case for multi-object spectroscopy on the European ELT, we present the top-level instrument requirements that are being used in the Phase A design study of the MOSAIC concept. The assembled cases span the full range of E-ELT science and generally require either ‘high multiplex' or 'high definition' observations to best exploit the excellent sensitivity and spatial performance of the telescope. We highlight some of the science studies that are now being used in trade-off studies to inform the capabilities of MOSAIC and its technical design.
KEYWORDS: Active optics, Mirrors, Disk lasers, Polishing, Actuators, Monochromatic aberrations, Active optics, Mirrors, Polishing, Interfaces, Chemical elements, Finite element methods, Freeform optics
We present two ways to generate or compensate for first order optical aberrations using smart warping harnesses. In these cases, we used the same methodology leading to replace a previous actuation system currently on-sky and to get a freeform mirror intended to a demonstrator. Starting from specifications, a warping harness is designed, followed by a meshing model in the finite elements software. For the two projects, two different ways of astigmatism generation are presented. The first one, on the VLT-SPHERE instrument, with a single actuator, is able to generate a nearly pure astigmatism via a rotating motorization. Two actuators are sufficient to produce the same aberration for the active freeform mirror, main part of the OPTICON-FAME project, in order to use stress-polishing method.
The Universe is comprised of hundreds of billions of galaxies, each populated by hundreds of billions of stars. Astrophysics aims to understand the complexity of this almost incommensurable number of stars, stellar clusters and galaxies, including their spatial distribution, formation, and current interactions with the interstellar and intergalactic media. A considerable fraction of astrophysical discoveries require large statistical samples, which can only be addressed with multi-object spectrographs (MOS). Here we introduce the MOSAIC study of an optical/near-infrared MOS for the European Extremely Large Telescope (E-ELT), which has capabilities specified by science cases ranging from stellar physics and exoplanet studies to galaxy evolution and cosmology. Recent studies of critical technical issues such as sky-background subtraction and multi-object adaptive optics (MOAO) have demonstrated that such a MOS is feasible with current technology and techniques. In the 2020s the E-ELT will become the world’s largest optical/IR telescope, and we argue that it has to be equipped as soon as possible with a MOS. MOSAIC will provide a vast discovery space, enabled by a multiplex of ∼ 200 and spectral resolving powers of R = 5 000 and 20 000. MOSAIC will also offer the unique capability of 10-to-20 ‘high-definition’ (MOAO) integral-field units, optimised to investigate the physics of the sources of reionisation, providing the most efficient follow-up of observations with the James Webb Space Telescope (JWST). The combination of these modes will enable the study of the mass-assembly history of galaxies over cosmic time, including high-redshift dwarf galaxies and studies of the distribution of the intergalactic medium. It will also provide spectroscopy of resolved stars in external galaxies at unprecedented distances, from the outskirts of the Local Group for main-sequence stars, to a significant volume of the local Universe, including nearby galaxy clusters, for luminous red supergiants.
C. Evans, M. Puech, B. Barbuy, P. Bonifacio, J.-G. Cuby, E. Guenther, F. Hammer, P. Jagourel, L. Kaper, S. Morris, J. Afonso, P. Amram, H. Aussel, A. Basden, N. Bastian, G. Battaglia, B. Biller, N. Bouché, E. Caffau, S. Charlot, Y. Clénet, F. Combes, C. Conselice, T. Contini, G. Dalton, B. Davies, K. Disseau, J. Dunlop, F. Fiore, H. Flores, T. Fusco, D. Gadotti, A. Gallazzi, E. Giallongo, T. Gonçalves, D. Gratadour, V. Hill, M. Huertas-Company, R. Ibata, S. Larsen, O. Le Fèvre, B. Lemasle, C. Maraston, S. Mei, Y. Mellier, G. Östlin, T. Paumard, R. Pello, L. Pentericci, P. Petitjean, M. Roth, D. Rouan, D. Schaerer, E. Telles, S. Trager, N. Welikala, S. Zibetti, B. Ziegler
Over the past 18 months we have revisited the science requirements for a multi-object spectrograph (MOS) for the
European Extremely Large Telescope (E-ELT). These efforts span the full range of E-ELT science and include input
from a broad cross-section of astronomers across the ESO partner countries. In this contribution we summarise the key
cases relating to studies of high-redshift galaxies, galaxy evolution, and stellar populations, with a more expansive
presentation of a new case relating to detection of exoplanets in stellar clusters. A general requirement is the need for
two observational modes to best exploit the large (≥40 arcmin2) patrol field of the E-ELT. The first mode (‘high
multiplex’) requires integrated-light (or coarsely resolved) optical/near-IR spectroscopy of >100 objects simultaneously.
The second (‘high definition’), enabled by wide-field adaptive optics, requires spatially-resolved, near-IR of >10
objects/sub-fields. Within the context of the conceptual study for an ELT-MOS called MOSAIC, we summarise the toplevel
requirements from each case and introduce the next steps in the design process.
Extreme freeform mirrors couple a non-axisymmetrical shape and an extreme asphericity, i.e. more than one millimeter
of deviation from the best fit sphere. In astronomical instrumentation, such a large asphericity allows compact
instruments, using less optical components. However, the lack of freeform mirrors manufacturing facilities is a real issue.
We present the concept and development of an innovative manufacturing process based on plasticity forming which
allow imprinting permanent deformations on mirrors, following a pre-defined mold. The aim of this activity, pursued in
the frame of the OPTICON-FAME (Freeform Active Mirrors Experiment) project, is to demonstrate the suitability of
this method for VIS/NIR/MIR applications. The process developed can operate on thin and flat polished initial
substrates. Three study cases have been highlighted by FEA (Finite Element Analysis) and the real tests associated were
performed on thin substrates in AISI420b stainless steel with 100 mm optical diameter. A comparison between FEA and
tests is performed to study the evolution of the mechanical behaviour and the optical quality. The opto-mechanical
results will allow a fine tuning of FEA parameters to optimize the residual form errors obtained through this process to
converge toward an innovative and recurrent process.
The advent of extremely large telescopes will bring unprecedented light-collecting power and spatial resolution, but it will also lead to a significant increase in the size and complexity of focal-plane instruments. The use of freeform mirrors could drastically reduce the number of components in optical systems. Currently, manufacturing issues limit the common use of freeform mirrors at short wavelengths. This article outlines the use of freeform mirrors in astronomical instruments with a description of two efficient freeform optical systems. A new manufacturing method is presented which seeks to overcome the manufacturing issues through hydroforming of thin polished substrates. A specific design of an active array is detailed, which will compensate for residual manufacturing errors, thermoelastic deformation, and gravity-induced errors during observations. The combined hydroformed mirror and the active array comprise the Freeform Active Mirror Experiment, which will produce an accurate, compact, and stable freeform optics dedicated to visible and near-infrared observations.
The EAGLE and EVE Phase A studies for instruments for the European Extremely Large Telescope (E-ELT) originated
from related top-level scientific questions, but employed different (yet complementary) methods to deliver the required
observations. We re-examine the motivations for a multi-object spectrograph (MOS) on the E-ELT and present a unified
set of requirements for a versatile instrument. Such a MOS would exploit the excellent spatial resolution in the near-infrared envisaged for EAGLE, combined with aspects of the spectral coverage and large multiplex of EVE. We briefly
discuss the top-level systems which could satisfy these requirements in a single instrument at one of the Nasmyth foci of
the E-ELT.
The EAGLE instrument is a Multi-Object Adaptive Optics (MOAO) fed, multiple Integral Field Spectrograph (IFS),
working in the Near Infra-Red (NIR), on the European Extremely Large Telescope (E-ELT). A Phase A design study
was delivered to the European Southern Observatory (ESO) leading to a successful review in October 2009. Since that
time there have been a number of developments, which we summarize here. Some of these developments are also
described in more detail in other submissions at this meeting.
The science case for the instrument, while broad, highlighted in particular: understanding the stellar populations of
galaxies in the nearby universe, the observation of the evolution of galaxies during the period of rapid stellar build-up
between redshifts of 2-5, and the search for 'first light' in the universe at redshifts beyond 7. In the last 2 years substantial
progress has been made in these areas, and we have updated our science case to show that EAGLE is still an essential
facility for the E-ELT. This in turn allowed us to revisit the science requirements for the instrument, confirming most of
the original decisions, but with one modification.
The original location considered for the instrument (a gravity invariant focal station) is no longer in the E-ELT
Construction Proposal, and so we have performed some preliminary analyses to show that the instrument can be simply
adapted to work at the E-ELT Nasmyth platform.
Since the delivery of the Phase A documentation, MOAO has been demonstrated on-sky by the CANARY experiment at
the William Herschel Telescope.
We present the SVOM mission that the Chinese National Space Agency and the French Space Agency have decided to jointly implement. SVOM has been designed to detect, characterise and quickly localise gamma-ray bursts (GRBs) and other types of high-energy transients. For this task the spacecraft will carry two widefield high-energy instruments: ECLAIRs, a hard X-ray imager, and the Gamma-Ray Monitor, a broadband spectrometer. Upon localising a transient, SVOM will quickly slew towards the source and start deep followup observations with two narrow-field telescopes: the Micro-channel X-ray Telescope in X-rays and the Visible Telescope in the visible. The nearly anti-solar pointing of SVOM combined with the fast transmission of GRB positions to the ground in less than 1 minute, will facilitate the observations of SVOM transients by the largest ground based telescopes.
Freeform optics offer additional degrees of freedom that can lead to a simplification of instrument optical designs with
compact solutions. In this context, we propose a new mathematical description of freeform surfaces. This new
mathematical formalism, based on the "eigen-modes" of Bernstein polynomials was developed for off-axis highly
aspherical surfaces modelling. It allows to take into account different kinds of deformations of the optical surface with
local influence capabilities. We present the mathematical formalism developed and then we focus on the optical analysis
of an innovative instrument design. The advantages provided by this new modelling are examined.
The next generation of focal-plane astronomical instruments requires technological breakthroughs to reduce their system
complexity while increasing their scientific performances. Applied to the optical systems, recent studies show that the
use of freeform reflective optics allows competitive compact systems with less optical components. In this context, our
challenge is to supply an active freeform mirror system, using a combination of different active optics techniques. The
optical shape will be provided during the fabrication using the mechanical property of metals to plasticize and will be
coupled with a specific actuator system to compensate for the residual form errors, during the instrument operation
phase. We present in this article the development of an innovative manufacturing process based on cold hydro-forming
method, with the aim to adapt it for VIS/NIR requirements in terms of optical surface quality. It can operate on thin and
flat polished initial substrates. The realization of a first prototype for a 100 mm optical diameter mirror is in progress, to
compare the mechanical behaviours obtained by tests and by Finite Element Analysis (FEA), for different materials.
Then, the formed samples will be characterized optically. The opto-mechanical results will allow a fine tuning of FEA
parameters to optimize the residual form errors obtained through this process. It concerns the microstructure
considerations, the springback effects and the work hardening evolutions of the samples, depending on the initial
substrate properties and the boundary conditions applied. Modeling and tests have started with axi-symmetric spherical
and aspherical shapes and will continue with highly aspherics and freeforms.
The future generation of Extremely Large Telescopes will require a complex combination of technologies for adaptive
optics (AO) systems assisted by laser guide stars (LGS). In this context, the distance from the LGS spot to the telescope
pupil ranges from about 80 to 200 km, depending on the Sodium layer altitude and the elevation of the telescope. This
variation leads to a defocusing effect on the LGS wave-front sensor which needs to be compensated. We propose an
active mirror able to compensate for this variation, based on an original optical design including this active optics
component. This LGS Variable Curvature Mirror (LGS-VCM) is a 120 mm spherical active mirror able to achieve 820
μm deflection sag with an optical quality better than 150 nm RMS, allowing the radius of curvature variation from F/12
to F/2. Based on elasticity theory, the deformation of the metallic mirror is provided by an air pressure applied on a thin
meniscus with a variable thickness distribution. In this article, we detail the analytical development leading to the
specific geometry of the active component, the results of finite element analysis and the expected performances in terms
of surface error versus the range of refocalisation. Three prototypes have been manufactured to compare the real
behavior of the mirror and the simulations data. Results obtained on the prototypes are detailed, showing that the
deformation of the VCM is very close to the simulation, and leads to a realistic active concept.
The evolution of astrophysical needs in the era of extremely large telescopes calls more and more complex instrumental systems and sub-systems. A promising solution would be to propose compact reflective optical systems, with less optical
surfaces than classical optical designs. This is made possible if the designs are not limited by the use of known conics or
symmetrical optical surfaces. Recent studies have shown that the use of highly aspherics could strongly reduce the number of optical surfaces and also the size of instruments, while improving the global system performances. The aim of
this article is to study the feasibility of the design and manufacturing of highly aspheric optical mirrors, toward freeform
mirrors, thanks to the combination of different active optics techniques: stress deformations up to plasticization
phenomenon to provide the optical shape during the manufacturing and actuator corrections to compensate for residual errors during the operation phase of the instrument. A first step consists in structural mechanics analysis to understand as
possible the non-linear behaviors of materials and its particular effects which depend on the material chosen, the global dimensions and the boundary conditions parameterized for the manufacturing process.
We developed a new mathematical formalism to model highly aspherical optical surfaces opening the possibility to
explore innovative optical designs. This formalism is based on Bernstein polynomials allowing to describe from low to
high order deformations of the optical surface. It has been implemented into Zemax making use of the User-Defined
Surface (UDS-DLL) Zemax capability. In this case, the mathematical definition of the surface is imported into Zemax
then allowing to apply classical optimization and analysis functionalities. This paper presents the UDS-DLL tool based
on Bernstein polynomials together with an initial optical analysis performed to evaluate the gain obtained in using such a
new formalism.
EAGLE is the multi-object spatially-resolved near-IR spectrograph instrument concept for the E-ELT, relying
on a distributed Adaptive Optics, so-called Multi Object Adaptive Optics. This paper presents the results of
a phase A study. Using 84×84 actuator deformable mirrors, the performed analysis demonstrates that 6 laser
guide stars (on an outer ring of 7.2' diameter) and up to 5 natural guide stars of magnitude R < 17, picked-up in
a 7.3' diameter patrol field of view, allow us to obtain an overall performance in terms of Ensquared Energy of
35% in a 75×75mas2 resolution element at H band whatever the target direction in the centred 5' science field
for median seeing conditions. In terms of sky coverage, the probability to find the 5 natural guide stars is close
to 90% at galactic latitudes |b| ~ 60 deg. Several MOAO demonstration activities are also on-going.
We designed, developed, and tested a Variable Curvature Mirror (VCM) as an active refocusing system for the Laser
Guide Star (LGS) Wave Front Sensor (WFS) of the E-ELT EAGLE instrument [1]. This paper is the second of two from
our team on this R&D activity: Hugot et al. this conf. [2] presented the mirror design and performance simulations. Here,
we report on the fabrication integration, testing and performance of the VCM system. During this activity, we developed
all necessary parts for the VCM system: a metallic mirror, its housing and mounts, a computer-controlled pressure
system, an internal metrology, a testbench etc. The functional testing of the VCM system is successful: we can control
the internal pressure to less than 1 mBar, and measure the mirror displacement with a 100 nm accuracy. The mirror
displacement is a near-linear and well-simulated function of internal pressure for the desired range of focus. The intrinsic
optical quality of the mirror meniscus is well within the specifications. Once mounted in its housing, we observe
additional mechanical constraints for the current design that generate optical aberrations. We measured the amplitude of
the Zernike modes, and we showed that the axisymetric terms display a variation trend very similar to simulations, with
amplitude close to simulations. All these results are very promising for a design of focus compensation without any
moving part.
KEYWORDS: Mirrors, Finite element methods, Telescopes, Spherical lenses, Sodium, Space telescopes, Disk lasers, Optical design, Active optics, Monochromatic aberrations
In the frame of the E-ELT-EAGLE instrument phase A studies, we designed a convex VCM able to compensate
for the focus variation on the Laser Guide Star (LGS) wavefront sensor, due to the elevation of the telescope
and the fixed sodium layer altitude. We present an original optical design including this active convex mirror,
providing a large sag variation on a spherical surface with a 120mm clear aperture, with an optical quality
better than lambda/5 RMS up to 820μm of sag and better than lambda/4 RMS up to 1000μm of sag. Finite
element analysis (FEA) allowed an optimisation of the mirror's variable thickness distribution to compensate
for geometrical and material non linearity. Preliminary study of the pre-stressing has also been performed by
FEA, showing that a permanent deformation remains after removal of the loads. Results and comparison with
the FEA are presented in the article of F.Madec et al (AS10-7736-119, this conference), with an emphasis on
the system approach.
EAGLE is a Phase A study of a multi-IFU, near-IR spectrometer for the European Extremely Large Telescope (E-ELT).
The design employs wide-field adaptive optics to deliver excellent image quality across a large (38.5 arcmin2) field.
When combined with the light grasp of the E-ELT, EAGLE will be a unique and efficient facility for spatially-resolved,
spectroscopic surveys of high-redshift galaxies and resolved stellar populations. Following a brief overview of the
science case, here we summarise the functional and performance requirements that flow-down from it, provide
illustrative performances from simulated observations, and highlight the strong synergies with the James Webb Space
Telescope (JWST) and the Atacama Large Millimeter Array (ALMA).
EAGLE is an instrument under consideration for the European Extremely Large Telescope (E-ELT). EAGLE will be
installed at the Gravity Invariant Focal Station of the E-ELT. The baseline design consists of 20 IFUs deployable over a
patrol field of ~40 arcmin2. Each IFU has an individual field of view of ~ 1.65" x 1.65". While EAGLE can operate with
the Adaptive Optics correction delivered by the telescope, its full and unrivaled scientific power will be reached with the
added value of its embedded Multi-Object Adaptive Optics System (MOAO). EAGLE will be a unique and efficient
facility for spatially-resolved, spectroscopic surveys of high-redshift galaxies and resolved stellar populations. We detail
the three main science drivers that have been used to specify the top level science requirements. We then present the
baseline design of the instrument at the end of Phase A, and in particular its Adaptive Optics System. We show that the
instrument has a readiness level that allows us to proceed directly into phase B, and we indicate how the instrument
development is planned.
EAGLE is an instrument for the European Extremely Large Telescope (E-ELT). EAGLE will be installed at the Gravity
Invariant Focal Station of the E-ELT, covering a field of view of 50 square arcminutes. Its main scientific drivers are the
physics and evolution of high-redshift galaxies, the detection and characterization of first-light objects and the physics of
galaxy evolution from stellar archaeology. These key science programs, generic to all ELT projects and highly
complementary to JWST, require 3D spectroscopy on a limited (~20) number of targets, full near IR coverage up to 2.4
micron and an image quality significantly sharper than the atmospheric seeing. The EAGLE design achieves these
requirements with innovative, yet simple, solutions and technologies already available or under the final stages of
development. EAGLE relies on Multi-Object Adaptive Optics (MOAO) which is being demonstrated in the laboratory
and on sky. This paper provides a summary of the phase A study instrument design.
EAGLE is a wide FoV (5 arcmin diameter), multi-objects (at least 20) integral-field spectrograph (R>4000) for the E-ELT.
The top level requirements are to concentrate 30 to 40 % of the photons collected by the E-ELT in a focal area of
75x75 mas2 in H band. This leads to the selection of the Multi Object Adaptive Optics in order to deliver such a
performance in a so-large FoV. In this paper, we present a detailed analysis of the error budget for an MOAO system in
EAGLE. It is based on numerical simulation results. The budget is splitted in LGS and NGS contributions. The analysis
leads to share the specifications between low spatial frequencies and high spatial frequencies in the wave-front errors.
Finally a preliminary conceptual design of the MOAO system is deduced including 9 LGS for tomography and a 9000
actuator deformable mirror per channel.
The reliability of active optic for telescopes and instrumentation is now good enough to make them available for day to
day use in working observatories. Future telescopes and their associated instruments will benefit from this technology to
offer innovative concepts, optimal performance and improved reliability.
An optical design of the multi-objects spectrograph EAGLE using, active surfaces, is detailed in this article. The first
active component is a steering mirror, included in the target acquisition system, able to compensate for large astigmatism
variations due to the variable off-axis design. This innovative design also includes two variable curvature mirrors
authorising focus compensation and adding a zoom facility. A complete description of these active mirrors mechanical
principle is presented, from elasticity theory to opto-mechanical design. The prototypes of these active mirrors with their
complete test bench are detailed.
We present an overview of the EAGLE science case, which spans spatially resolved spectroscopy of targets from five
key science areas - ranging from studies of heavily obscured Galactic star clusters, right out to the first galaxies at the
highest redshifts. Here we summarise the requirements adopted for the study and also evaluate the availability of natural
guide stars in example fields, which will impact on the adaptive optics performance and architecture.
EAGLE is an instrument under conceptual study for the European Extremely Large Telescope (E-ELT). EAGLE will be
installed at the Gravity Invariant Focal Station of the E-ELT, covering a field of view between 5 and 10 arcminutes. Its
main scientific drivers are the physics and evolution of high-redshift galaxies, the detection and characterization of first-light
objects and the physics of galaxy evolution from stellar archaeology. The top level requirements of the instrument
call for 20 spectroscopic channels in the near infrared, assisted by Adaptive Optics. Several concepts of the Target
Acquisition sub-system have been studied and are briefly presented. Multi-Conjugate Adaptive Optics (MCAO) over a
segmented 5' field has been evaluated and compared to Multi-Object Adaptive Optics (MOAO). The latter has higher
performance and is easier to implement, and is therefore chosen as the baseline for EAGLE. The paper provides a status
report of the conceptual study, and indicates how the future steps will address the instrument development plan due to be
completed within a year.
A particular flavor of multi-object spectrographs uses pick-off and steering mirrors. These mirrors perform target selection by relaying the optical beams from variable positions in the focal plane to fixed optics in the instrument. Examples of instrument conceptual designs based on this system are presented and illustrated. Particular emphasis is given to the beam steering mirror (BSM) environment which requires the following mechanical motions: translation, rotations and possibly active deformation of the optical surface. A BSM design featuring translation, tip-tilt and a toroidal deformable surface is presented. First results from a prototype development are also presented. A metrology system including wavefront sensing allows to measure and control the position of the optical beam. This system, required for system tests, integration, calibration and operation, is presented. This work is part of the Laboratoire d'Astrophysique de Marseille (LAM) contribution to the beam manipulation work package of the OPTICON smart focal plane.
We report on the science case high level specifications for a wide field spectrograph instrument for an Extremely Large
Telescope (ELT) and present possible concepts. Preliminary designs are presented which resort to different instrument
concepts: monolithic integral field (IFU), multi-IFU, and a smart tunable filter. This work is part of the activities performed
in the work package 'Instrumentation' of the 'ELT Design Study', a programme supported by the European Community,
Framework Programme 6.
We discuss the possibility of improving the optical efficiency of ELT instruments by reducing the number of optical surfaces with highly aspheric optics generated by deformable mirrors (DMs). Preliminary analysis shows that a 2 aspheric mirror design could in principle replace a traditional optical design with a complex series of ~ 10 lenses, providing a potential gain in efficiency of ~ 20% as well as a significant gain in compactness. New OH suppression systems based on technologies from the photonics world become available that may ultimately allow to reduce the near IR sky brightness by 2 to 4 magnitudes, depending on wavelength. The potential performance of an ELT with OH suppression is similar in imaging and significantly higher in spectroscopy than JWST.
We report on the development of instrument concepts for a European ELT, expanding on studies carried out as part of the ESO OWL concept. A range of instruments were chosen to demonstrate how an ELT could meet or approach the goals generated by the OPTICON science team, and used to push the specifications and requirements of telescope and adaptive optics systems. Preliminary conclusions are presented, along with a plan for further more detailed instrument design and technology developments. This activity is supported by the European Community (Framework Programme 6, ELT Design Study, contract number 011863).
MIDI (MID-infrared Interferometric instrument) gave its first N-band (8 to 13 micron) stellar interference fringes on the VLTI (Very Large Telescope Interferometer) at Cerro Paranal Observatory (Chile) in December 2002. An lot of work had to be done to transform it, from a successful physics experiment, into a premium science instrument which is offered to the worldwide community of astronomers since September 2003. The process of "paranalization", carried out by the European Southern Observatory (ESO) in collaboration with the MIDI consortium, has aimed to make MIDI simpler to use, more reliable, and more efficient. We describe in this paper these different aspects of paranalization (detailing the improvement brought to the observation software) and the lessons we have learnt. Some general rules, for bringing an interferometric instrument into routine operation in an observatory, can be drawn from the experience with MIDI. We also report our experience of the first "service mode" run of an interferometer (VLTI + MIDI) that took place in April 2004.
KEYWORDS: James Webb Space Telescope, Mirrors, Spectrographs, Prototyping, Space telescopes, Optics manufacturing, Optical design, Spectral resolution, Optical components, Near infrared
We propose to implement an Integral-Field Unit (IFU) mode in the near-infrared spectrograph NIRSpec of the future James Webb Space Telescope (JWST), instrument under the responsibility of the European Space Agency (ESA). The IFU mode will provide unique additional scientific capabilities, complementary to those of the main multi-object mode of NIRSpec. It would cover a 3"x3" field of view with a 0.075" sampling and make use of the R=3000 spectral configurations of NIRSpec, covering the complete 1.0-5.0 microns range in three shots. First performance simulations yield a limiting AB magnitude of 24 for a point-like source. On the technical side, the IFU is based on the advanced image slicer concept and would include a stack of forty 900 μm thick, slicing mirrors. We are currently conducting a prototyping work funded by ESA, aiming at demonstrating a TRL6 readiness level for this technology (see presentation by F. Laurent). We present the optical design of the IFU, the strategy used during its definition (minimum impact on NIRSpec), as well as the proposed implementation within the NIRSpec instrument. We will stress that, this currently optional mode is a unique opportunity to provide JWST with a powerful integral field mode at marginal costs.
High-z galaxies beyond redshift ~ 4 are essentially detected from ground based observations through their Lyα emission. The anticipated Lyα flux of galaxies at redshifts ~ 6 and beyond is a few times 0.1 10-17 ergs.s-1.cm-2 and its detection requires observations in low background conditions, when the observing wavelength is pushed into the near IR domain. We have carried out observations on 4-8 m telescopes to search for high z galaxies at 920 nm, 1060 and 1187 nm, resorting to various techniques: Narrow Band (NB) imaging and multi-slit windows. Observations, data reduction and preliminary results are described.
This paper presents miscellaneous activities related to instrumentation taking place at Paranal Observatory. The number of instruments and / or facilities that will eventually equip the Observatory (VLT, VLTI, VST, VISTA)is about 20. An adequate organization (human and technical)is required to ensure configuration control and efficient preventive and corrective maintenance (hardware and software). Monitoring instrument performance is a key feature to guarantee success of operations and minimize technical downtime. Some observational projects are carried out with the aim of characterizing the Paranal sky conditions in the visible and the IR, in emission and absorption. Efforts are being developed to monitor, characterize and archive the transparency conditions at night.
ISAAC is an IR imager and spectrometer installed at the first Unit Telescope of the ESO-VLT. ISAAC started science operations in April 99. We present the instrument characteristics, its performance and operation.
The VIRMOS consortium of French and Italian Institutes is manufacturing 2 wide field imaging multi-object spectrographs for the European Southern Observatory Very Large Telescope, with emphasis on the ability to carry over spectroscopic surveys of large numbers of sources. The Visible Multi-Object Spectrograph, VIMOS, is covering the 0.37 to 1 micron wavelength domain, with a full field of view of 4 by 7 by 8 arcmin2 in imaging and MOS mode. The Near IR Multi-Object Spectrograph, NIRMOS, is covering the 0.9 to 1.8 microns wavelength range, with afield of view 4 by 6 by 8 arcmin2 in MOS mode. The spectral resolution for both instrument scan reach up to R equals 5000 for a 0.5 arcsec wide slit. Multi-slit masks are produced by a dedicated Mask Manufacturing Machine cutting through thin Invar sheets and capable of producing 4 slit masks approximately 300 by 300 mm each with approximately slits 5.7 mm long in less than one hour. Integral field spectroscopy is made possible in VIMOS by switching in the beam specially build masks fed by 6400 fibers coming form a 54 by 54 arcsec2 integral field head with a 80 by 80 array of silica micro-lenses. NIRMOS has a similar IFS unit with a field of 30 by 30 arcmin2. These instruments are designed to offer very large multiplexing capabilities. In MOS mode, about 1000 objects can be observed simultaneously with VIMOS, with a S/N equals 10 obtained on galaxies with I equals 24 in one hour, and approximately 200 objects can be observed simultaneously with NIRMOS, with a S/N equals 10 obtained don galaxies with J equals 22, H equals 20.6 in 1h at Req equals 200. We present here the status of VIMOS, currently under final integration, with expected first light in the summer 2000, together with the final design of NIRMOS presented at the Final Design Review. The VLT-VIRMOS deep redshift survey of more with the final design of NIRMOS presented at the Final Design Review. The VLT-VIRMOS deep redshift survey of more than 150000 galaxies over the redshift range 0 < z < 5 will be undertaken based on 120 guaranteed nights awarded to the project.
ISAAC is an IR imager and array camera operating from 0.9 to 5 micrometers . This paper illustrates some preliminary scientific results which have been obtained during its first year of science operations. In Low Resolution Spectroscopy, we present results obtained on one Centaur, on TMR1-C and the detection of a methane brown dwarf. In Medium Resolution Spectroscopy, we present results obtained on kinematics studies in the central kpc of AGNs, and of emission line detections of distant galaxies at various redshift, from 0.6 to 3.
The IR Spectrometer and Array Camera (ISAAC) at the VLT has ben used for follow-up spectroscopy of 11 candidate H(alpha) emitting galaxies at z approximately equals 2.2 detected in a preparatory, IR narrow band filter imaging survey. This survey was conducted with Son of ISAAC at the ESO NTT and covered an area of 100 sq. arcmin including the WFPC2 and STIS fields in the HDFS. Line emission within the wavelength range of the 2.1 micrometers narrow band filters is confirmed in 6 of the candidates and in all but one of the 6 detected at >= 4 (sigma) in the survey. Although only a single emission line is observed its identification with H(alpha) is relatively secure and the absence of (NII) (6548,6584 Angstrom) is consistent with high ionization and/or low metallicity systems. Velocity dispersions and one H(alpha) rotation curve imply masses of up to approximately 1010M. Star formation rates of the individual galaxies derived from the H(alpha) fluxes are 20-35 M yr-1 and the total star formation rate density is 0.12 M Mpc-3. This is the same as found at z approximately equals 1.3 from H(alpha) observations with NICMOS on HST$_1) and close to that at z equals 3-4.5 derived from the extinction corrected UV continuum fluxes of Lyman Break galaxies2.
We investigate the use of non-cryogenic instrumentation for near IR spectroscopy. With this technique, it is possible to apply in the J and H bands some instrument concepts and observing techniques used in the visible. We present observations of the thermal background in H. We derive some instrument requirements for minimizing and handling it. We recommend the use of short wavelength cutoff wavelengths or linear filters in H. We present observations of the sky emission, and do confirm previous upper limits of the continuum emission between the OH lines. We discuss some applications of non-cooled near IR spectroscopy.
The atmospheric refraction affects the position of objects in the sky in two ways: a chromatic effect and a field differential effect. The former is about the same in the field and can be, in principle, corrected using an Atmospheric Dispersion Compensator (ADC). The latter is dependent of the field size and cannot be corrected. For spectroscopy in wide fields, both effects have to be carefully considered because they affect the spectrophotometry in terms of signal to noise ratio and spectral distortions. The present study aims to evaluate the atmospheric effects in the case of the VIMOS instrument for the ESO VLT. It is shown that provided a careful operational mode the distortion of spectra can be kept at a level less than 15% with reasonable constraints.
We present the current design of the VIsible Multi-Object Spectrograph (VIMOS) and the Near InfraRed Multi-Object Spectrograph (NIRMOS) for the European Southern Observatory Very Large Telescope. The basic scientific requirement is to conduct very deep redshift surveys of large quantities of objects, in a minimum number of nights. The technical specifications are to allow for a large multiplex gain over a wide field, and a high efficiency of the optical train, over the 0.37 to 1.8 micrometer domain. The baseline technical concept is built around 4 channels, covering 4 X 7 X 8 arcmin2 for VIMOS and 4 X 7 X 7 arcmin2 for NIRMOS. Each channel is an imaging spectrograph with a large field adaptation lens, a collimator, grisms or filters, and a F/1.8 camera, coupled to a 2048 X 4096 pixels CCD for VIMOS, and a 20482 HgCdTe Rockwell array for NIRMOS. The unique multiplex gain allows to obtain spectra of up to 840 object simultaneously with VIMOS, and up to 170 with NIRMOS (10 arcsec slits). An integral field spectroscopy mode with more than 6400 fibers coupled to micro-lenses will be available for VIMOS, covering a 1 X 1 arcmin2 field. The VLT-VIRMOS survey of more than 150,000 galaxies is planned down to magnitudes IAB equals 24, coupled to an ultra deep probe to IAB equals 26.
Paul Felenbok, Jean Gabriel Cuby, Jean-Pierre Lemonnier, Jacques Baudrand, Martin Casse, Michel Andre, Jean Czarny, J. Daban, M. Marteaud, Jean-Pierre Vola
'FUEGOS' (Fibre Unit for European General Optical Spectroscopy) is one of the foreseen focal instruments for the future ESO VLT (very large telescope). The goal is to provide the european community with first class equipment allowing high and low resolution spectroscopy for stellar and extragalactic observations in a large field. This large field of view, 30 arcmin provided by the VLT, is quite unique on 8 m class telescopes. The instrument is made of two parts: a fibre positioner attached to the Nasmyth rotator and a spectrograph sitting on the Nasmyth platform. The two assemblies are linked together with optical fibres. The instrument will include two different modes: the MEDUSA mode for the multi-object spectroscopy and the ARGUS mode for the 2D spectroscopy for extended objects. The multi-object positioner is of the robot type, based on a design using two gripper heads travelling simultaneously on a X-Y carriage. It locks magnetically 80 independent optical fibre bundles at object coordinates on a metallic focal surface. 2D spectroscopy is provided through a fibre anamorphoser in three different fields and spatial samplings. The spectrograph is of the 'white pupil' type, based on a catadioptric design with spherical optics throughout. It gives access to spectral resolutions ranging from 1500 to 30000. The detector is a 2048 x 2048 CCD located inside the camera optics.
Sky subtraction with fibres is known to be more difficult than with slits. The scientific objectives relevant to carry out with multifibre instruments, even in the new age of 8-10 m telescopes, mainly deal with objects of magnitude <EQ 22. The requirement in beam switching methods to reach the ultimate performances is controversial. In this paper, we present the results of sky subtraction tests that have been performed on the 3.6 m ESO telescope. The two basic points we wanted to address were the ability of fibres to allow sky subtraction up to the 22nd magnitude, and whether or not beam switching is required. We detail the data reduction steps we have employed. We define all the possible techniques that can be used for sky subtraction and give the corresponding expressions for spectrum extraction. Last, we present the results we have obtained, and conclude that sky subtraction with fibres is quite feasible, even on 4 m telescopes, up to b(subscript $japproximately equals 22 without resorting to beam switching techniques.
The scientific objectives of multi-object fiber instruments on 8 m class telescopes may significantly depart from those carried out on 4 m class telescopes. Crude anticipation of future programs on these instruments allows to predict that targets will be mainly point sources or of low extension, with magnitudes up to approximately 22. With these characteristics, some observational aspects are investigated: (1) The (blind) positioning error budget constrains the astrometry to within 0.2' rms to keep photon losses at an acceptable level; (2) All-sky atlases from Schmidt plate scans, when available, will provide the relevant information for most programs; (3) Cross- identification or special observing procedures may be required for guide stars if they have a different origin than targets; (4) Atmospheric effects are investigated. Chromatic dispersion is shown impossible to calibrate out. The observation wavelength must be properly related to the acquisition and guiding wavelengths, constraining the use of filters; (5) Other observational constraints like sky subtraction or high spectral stability can lead to specific observational procedures. General observing modes are briefly reviewed. The impacts on the performances, described in terms of `Realizable Multiplex Advantage' (RMA) is described. At best, the RMA can reach one third of the number of fibers.
Wavefront sensing is a very powerful technique whose capability in the field of diffraction- limited imaging through turbulence has been demonstrated. The ultimate performance of a Hartmann-Shack wavefront sensor is analyzed and used to define a detector choice strategy.
This paper is a presentation of the Come-On-Plus adaptive optics system, based on the Come-On
prototype. Come-On-PIus will be set up in 1992 on the ESO 3.6 m telescope in La Silla (Chile). It is an
upgrade of the Come-On instrument, with a 52 actuator deformable mirror, and 30 Hz correction
bandwidth. But the main improvement concerns the wavefront sensing, designed in this instrument for
astronomical applications, with a high detectivity wavefront sensor and a specific mirror control
algorithm. This system is planned for routine astronomical observing as well as providing design
parameters for the adaptive optics system of the ESO Very Large Telescope (VLT).
The aim of this paper is to show the relevance of the electron bombardment technique of photon counting for astronomical applications, using results obtained both in the laboratory and on the sky with a prototype tube. The potential astronomical applications discussed are in techniques requiring high time resolution, either in an analog or a photon counting mode (wavefront analysis, speckle interferometry, multitelescope interferometry, etc.) and observation of rapidly varying objects. Current prototypes will be used to achieve wavefront analysis in the near future. The first priority in further technical development must obviously be to develop a larger and faster CCD.
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