The Cassegrain U-Band Efficient Spectrograph (CUBES) is a high-efficiency spectrograph designed for observations from 305 to 400nm. It will be integrated at a Cassegrain focus of the Very Large Telescope (VLT). The image slicer technology is applied to reformat the field of view reducing the spectrograph entrance slit etendue and minimising the spectrograph volume and weight without slit losses. Two image slicers will provide CUBES with two spectral resolving powers: R≥20,000 for high resolution (HR) and R≥5,000 for low resolution (LR). Both image slicers are composed of two arrays of six spherical mirrors. For the HR mode, a rectangular field of view of 1.5arcsec by 10arcsec is reorganised into a slit of 0.19mm × 88mm; for the LR mode, a field of view of 6arcsec by 10arcsec is reformatted into a slit of 0.77mm × 88mm, with slicer mirrors of width 0.5mm and 2mm, respectively.
CUBES is currently in the Preliminary Design Phase (Phase B). This communication presents the Conceptual (Phase A) design and the main performance for the HR and LR image slicers addressing the following technological challenges: compact layout with the minimum number of optical components to optimise throughput, near diffraction limited optical quality, telecentric design with overlapped exit pupils for all slices of the field of view, distribution of the slicer mirrors to reduce shadows and selection of the best substrate for the very short wavelengths at which CUBES will operate.
HARMONI is the first light visible and near-IR integral field spectrograph for the ELT. It covers a large spectral range from 450nm to 2450nm with resolving powers from 3500 to 18000 and spatial sampling from 60mas to 4mas. It will use an image slicer to provide spectra over a single contiguous area, providing fields of view on the sky of 9.3x6.3”, 4.2x3.1”, 2.1x1.5” and 0.84x0.62” with increasing spatial resolution (i.e.- 60x30, 20x20, 10x10 and 4x4 mas2) and magnification 2, 3/6, 6/12 and 15/30 respectively. The anamorphic magnifications in 20x20, 10x10 and 4x4 scales are implemented using two toroidal mirrors in each optical path. In this paper, we present a complete tolerance analysis for the anamorphic stages and a compensation procedure to ensure the requirements of the system.
The preliminary concept development phase of the Southern African Large Telescope (SALT) mini-tracker (MT) project was completed. The addition of up to four MTs to the telescope would in effect create multiple four-to-six-meter class telescopes using SALT’s 10-m diameter primary mirror. Each MT would be able to provide spectroscopic follow up for current and future large astronomical surveys (e.g. MeerKAT, eROSITA, Gaia, LSST, SKA, etc.). This phase included development of a novel optical design for the spherical aberration corrector, preliminary mechanical design for the telescope interface and the MTs themselves, and simulation tools to calculate the effective illumination of each MT for a selected target. A detailed project management plan and documentation framework were also created, including a prototype development path, a project cost estimate, and a schedule to completion. Following a review of the project near the end of this concept development phase, the decision was taken to put the project on hold. Although the MTs were deemed to be technically feasible, a more detailed science case was required in order to proceed with the project. In addition, several personnel-intensive projects to improve the performance and reliability of the telescope, either now underway or soon to be started, would need to be completed prior to beginning a project of this magnitude and complexity. However, a number of valuable tools and results that will benefit SALT emerged from this concept development phase, and are outlined here.
HARMONI is the first light, adaptive optics assisted, integral field spectrograph for the European Southern Observatory’s Extremely Large Telescope (ELT). A work-horse instrument, it provides the ELT’s diffraction limited spectroscopic capability across the near-infrared wavelength range. HARMONI will exploit the ELT’s unique combination of exquisite spatial resolution and enormous collecting area, enabling transformational science. The design of the instrument is being finalized, and the plans for assembly, integration and testing are being detailed. We present an overview of the instrument’s capabilities from a user perspective, and provide a summary of the instrument’s design. We also include recent changes to the project, both technical and programmatic, that have resulted from red-flag actions. Finally, we outline some of the simulated HARMONI observations currently being analyzed.
KEYWORDS: Spectrographs, Stars, Chemical elements, Ultraviolet radiation, Telescopes, Galactic astronomy, Sensors, Astronomy, Signal to noise ratio, Near ultraviolet
In the era of Extremely Large Telescopes, the current generation of 8-10m facilities are likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (> 40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R >20, 000 (with a lower-resolution, sky-limited mode of R ~7, 000). With the design focusing on maximizing the instrument throughput (ensuring a Signal to Noise Ratio (SNR) ~20 per high-resolution element at 313 nm for U ~18.5 mag objects in 1h of observations), it will offer new possibilities in many fields of astrophysics, providing access to key lines of stellar spectra: a tremendous diversity of iron-peak and heavy elements, lighter elements (in particular Beryllium) and light-element molecules (CO, CN, OH), as well as Balmer lines and the Balmer jump (particularly important for young stellar objects). The UV range is also critical in extragalactic studies: the circumgalactic medium of distant galaxies, the contribution of different types of sources to the cosmic UV background, the measurement of H2 and primordial Deuterium in a regime of relatively transparent intergalactic medium, and follow-up of explosive transients. The CUBES project completed a Phase A conceptual design in June 2021 and has now entered the detailed design and construction phase. First science operations are planned for 2028.
William Brzozowski, David Robertson, Ewan Fitzsimons, Henry Ward, Jennifer Keogh, Alasdair Taylor, Maria Milanova, Michael Perreur-Lloyd, Zeshan Ali, Andrew Earle, Daniel Clarkson, Robyn Sharman, Martyn Wells, Phil Parr-Burman
This paper will present an overview of the LISA (Laser Interferometer Space Antenna) optical bench and discuss the innovative methods developed to analyse and mitigate significant engineering challenges. There are two optical benches for each of the three LISA spacecraft. The optical bench consists of numerous components which form the paths of the interferometers used to measure the displacement changes caused by gravitational waves. Given each spacecraft is separated by 2.5 million Km, a laser beam sent from one to another arrives with a significantly lower irradiance than on departure. It is in part because of this that various engineering challenges are faced by the LISA OB. This is alongside the extremely demanding nature of measuring gravitational waves at a sensitivity of pico-meters per root-Hertz.
HARMONI is the adaptive optics assisted, near-infrared and visible light integral field spectrograph for the Extremely Large Telescope (ELT). A first light instrument, it provides the work-horse spectroscopic capability for the ELT. As the project approaches its Final Design Review milestone, the design of the instrument is being finalized, and the plans for assembly, integration and testing are being detailed. We present an overview of the instrument’s capabilities from a user perspective, provide a summary of the instrument’s design, including plans for operations and calibrations, and provide a brief glimpse of the predicted performance for a specific observing scenario. The paper also provides some details of the consortium composition and its evolution since the project commenced in 2015.
Precision-aligned, robust, ultra-stable optical assemblies are required in an increasing number of space-based applications such as fundamental science, metrology and geodesy. Hydroxide catalysis bonding is a proven, glue-free, technology for building such optical systems from materials such as ULE, Zerodur and fused silica. Hydroxide catalysis bonded optical systems have flown in missions such as GP-B and LISA Pathfinder achieving picometer path-length stability and microradian component stability over full mission lifetime. Component alignment and bonding was previously a largely manual process that required skilled operators and significant time. We have recently automated most of the alignment and bonding steps with the goals of improving overall precision, speed and reliability. Positioning and bonding of an optical component to within 4 microns and 10 microradians of a target position and alignment can now be reliably completed within half an hour, compared to the many hours typically taken previously. The key new features of this system are an interferometer that monitors the parallelism and separation of the surfaces to be bonded and a precision multi-axis manipulator that can optimise component alignment as it brings it down to the point of bonding. We present a description of the system and a summary of the alignment results obtained in a series of 9 test bonds. We also show how this system is being developed for integration into a precision optical manufacturing facility for assembly of large optical systems
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.
The Mid-Infrared Instrument (MIRI) on-board the James Webb Space Telescope (JWST) performs medium resolution spectroscopy in the 5 to 28.5micron wavelength range. The Medium-Resolution Spectrometer (MRS) of MIRI uses two Si:As impurity band conduction detector arrays. Coherent reflection of infrared light within the MIRI MRS detectors results in fringing; the detector layers act as efficient Fabry-Pérot etalons. In this paper we present three methods to calibrate out the fringes, as part of the MIRI data reduction pipeline. The methods are presented in the context of the investigations on the fringing seen in the MIRI flight model ground test data. The investigations show that the detector fringe transmission depends on the illumination pattern of the observed source on the detector. Optical stimuli of different spatial extents and position in the field-of-view yield different fringe patterns in their extracted spectra. An optical model of the MIRI detectors is hence proposed. By solving the Fresnel equations across the model optical layers, a source-specific fringe correction is derived.
Twinkle is a space mission designed for visible and near-IR spectroscopic observations of extrasolar planets. Twinkle’s highly stable instrument will allow the photometric and spectroscopic observation of a wide range of planetary classes around different types of stars, with a focus on bright sources close to the ecliptic. The planets will be observed through transit and eclipse photometry and spectroscopy, as well as phase curves, eclipse mapping and multiple narrow-band time-series. The targets observed by Twinkle will be composed of known exoplanets mainly discovered by existing and upcoming ground surveys in our galaxy (e.g. WASP, HATNet, NGTS and radial velocity surveys) and will also feature new discoveries by space observatories (K2, GAIA, Cheops, TESS). Twinkle is a small satellite with a payload designed to perform high-quality astrophysical observations while adapting to the design of an existing Low Earth Orbit commercial satellite platform. The SSTL-300 bus, to be launched into a low- Earth sun-synchronous polar orbit by 2019, will carry a half-meter class telescope with two instruments (visible and near-IR spectrographs - between 0.4 and 4.5μm - with resolving power R~300 at the lower end of the wavelength scale) using mostly flight proven spacecraft systems designed by Surrey Satellite Technology Ltd and a combination of high TRL instrumentation and a few lower TRL elements built by a consortium of UK institutes. The Twinkle design will enable the observation of the chemical composition and weather of at least 100 exoplanets in the Milky Way, including super-Earths (rocky planets 1-10 times the mass of Earth), Neptunes, sub-Neptunes and gas giants like Jupiter. It will also allow the follow-up photometric observations of 1000+ exoplanets in the visible and infrared, as well as observations of Solar system objects, bright stars and disks.
NASA’s James Webb Space Telescope (JWST) is a 6.5m diameter, segmented, deployable telescope for cryogenic IR space astronomy (~40K). The JWST Observatory architecture includes the Optical Telescope Element (OTE) and the Integrated Science Instrument Module (ISIM) element that contains four science instruments (SI), including a guider. OSIM is a full field, cryogenic, optical simulator of the JWST OTE. It is the “Master Tool” for verifying the cryogenic alignment and optical performance of ISIM by providing simulated point source/star images to each of the four Science Instruments in ISIM. Included in OSIM is a Pupil Imaging Module (PIM) - a large format CCD used for measuring pupil alignment. Located at a virtual stop location within OSIM, the PIM records superimposed shadow images of pupil alignment reference (PAR) targets located in the OSIM and SI pupils. The OSIM Pupil Imaging Module was described by Brent Bos, et al, at SPIE in 2011 prior to ISIM testing. We have recently completed the third and final ISIM cryogenic performance verification test before ISIM was integrated with the OTE. In this paper, we describe PIM implementation, performance, and measurement results.
Twinkle is a small satellite mission to observe the atmospheres of exoplanets in the visible to near infrared. This paper
describes the design of the infrared (1.3 to 4.5 micron) spectrometer which works at the diffraction limit of the 450mm
diameter telescope and at a resolving power of 300 (1.3-2.4 microns) and, in order to achieve the required SNR, R=30
for 2.4-4.5 microns. The planetary spectrum is obtained by taking differences between the spectra of star + planet at
different phases of the planet’s orbit so there is an emphasis of spectral and radiometric stability. The design incorporates
a number of features to enhance this stability
- compact all aluminium structure and mirror substrates to reduce alignment offsets when cooled to the operating
temperature of ~100K
- pupil imaging in the across dispersion direction to minimise changes due to sub-pixel variations in sensitivity and
reduce the number of illuminated pixels for background measurements
Image slicing integral field units were developed to provide spatially resolved spectroscopy over a two dimensional field of view. Spectral slicing applies similar design principles to provide an alternative to cross-dispersion. Key benefits include more efficient use of detector space and greater flexibility in selecting the wavelength ranges within each band. We will describe the design of a deployable spectral slicing mode as part of the METIS LM-band high resolution spectrometer.
The tropospheric distribution of greenhouse gases (GHGs) depends on surface flux variations, atmospheric chemistry and transport processes over a range of spatial and temporal scales. Accurate and precise atmospheric concentration observations of GHGs can be used to infer surface flux estimates, though their interpretation relies on unbiased atmospheric transport models. GHOST is a novel, compact shortwave infrared spectrometer which will observe tropospheric columns of CO2, CO, CH4 and H2O (along with the HDO/H2O ratio) during deployment on board the NASA Global Hawk unmanned aerial vehicle. The primary science objectives of GHOST are to: 1) test atmospheric transport models; 2) evaluate satellite observations of GHG column observations over oceans; and 3) complement in-situ tropopause transition layer observations from other Global Hawk instruments. GHOST comprises a target acquisition module (TAM), a fibre slicer and feed system, and a multiple order spectrograph. The TAM is programmed to direct solar radiation reflected by the ocean surface into a fibre optic bundle. Incoming light is then split into four spectral bands, selected to optimise remote observations of GHGs. The design uses a single grating and detector for all four spectral bands. We summarise the GHOST concept and its objectives, and describe the instrument design and proposed deployment aboard the Global Hawk platform.
KEYWORDS: Lawrencium, Silicon, Optical alignment, Virtual colonoscopy, James Webb Space Telescope, Metrology, Space telescopes, Telescopes, Finite element methods, Mirrors
While efforts within the optics community focus on the development of high-quality systems and data products, comparatively little attention is paid to their use. Our standards for verification and validation are high; but in some user domains, standards are either lax or do not exist at all. In forensic imagery analysis, for example, standards exist to judge image quality, but do not exist to judge the quality of an analysis. In litigation, a high quality analysis is by default the one performed by the victorious attorney’s expert. This paper argues for the need to extend quality standards into the domain of imagery analysis, which is expected to increase in national visibility and significance with the increasing deployment of unmanned aerial vehicle—UAV, or “drone”—sensors in the continental U. S.. It argues that like a good radiometric calibration, made as independent of the calibrated instrument as possible, a good analysis should be subject to standards the most basic of which is the separation of issues of scientific fact from analysis results.
The current instrumentation plan for the E-ELT foresees a High Resolution Spectrograph conventionally indicated as
HIRES. Shaped on the study of extra-solar planet atmospheres, Pop-III stars and fundamental physical constants, HIRES
is intended to embed observing modes at high-resolution (up to R=150000) and large spectral range (from the blue limit to the K band) useful for a large suite of science cases that can exclusively be tackled by the E-ELT. We present in this
paper the solution for HIRES envisaged by the "HIRES initiative", the international collaboration established in 2013 to
pursue a HIRES on E-ELT.
MOONS is a new Multi-Object Optical and Near-infrared Spectrograph selected by ESO as a third generation
instrument for the Very Large Telescope (VLT). The grasp of the large collecting area offered by the VLT (8.2m
diameter), combined with the large multiplex and wavelength coverage (optical to near-IR: 0.8μm - 1.8μm) of MOONS
will provide the European astronomical community with a powerful, unique instrument able to pioneer a wide range of
Galactic, Extragalactic and Cosmological studies and provide crucial follow-up for major facilities such as Gaia,
VISTA, Euclid and LSST. MOONS has the observational power needed to unveil galaxy formation and evolution over
the entire history of the Universe, from stars in our Milky Way, through the redshift desert, and up to the epoch of very
first galaxies and re-ionization of the Universe at redshift z>8-9, just few million years after the Big Bang. On a
timescale of 5 years of observations, MOONS will provide high quality spectra for >3M stars in our Galaxy and the
local group, and for 1-2M galaxies at z>1 (SDSS-like survey), promising to revolutionise our understanding of the
Universe.
The baseline design consists of ~1000 fibers deployable over a field of view of ~500 square arcmin, the largest patrol
field offered by the Nasmyth focus at the VLT. The total wavelength coverage is 0.8μm-1.8μm and two resolution
modes: medium resolution and high resolution. In the medium resolution mode (R~4,000-6,000) the entire wavelength
range 0.8μm-1.8μm is observed simultaneously, while the high resolution mode covers simultaneously three selected
spectral regions: one around the CaII triplet (at R~8,000) to measure radial velocities, and two regions at R~20,000 one
in the J-band and one in the H-band, for detailed measurements of chemical abundances.
The Mid-Infrared Instrument (MIRI) is one of four scientific instruments on the James Webb Space Telescope (JWST)
observatory, scheduled for launch in 2018. It will provide unique capabilities to probe the distant or deeply dust-enshrouded
regions of the Universe, investigating the history of star and planet formation from the earliest universe to
the present day. To enable this the instrument optical module must be cooled below 7K, presenting specific challenges
for the environmental testing and calibration activities.
The assembly, integration and verification (AIV) activities for the proto-flight model (pFM) instrument ran from March
2010 to May 2012 at RAL where the instrument has been put through a full suite of environmental and performance tests
with a non-conventional single cryo-test approach.
In this paper we present an overview of the testing conducted on the MIRI pFM including ambient alignment testing,
vibration testing, gravity release testing, cryogenic performance and calibration testing, functional testing at ambient and
operational temperatures, thermal balance tests, and Electro-Magnetic Compatibility (EMC) testing. We discuss how
tests were planned and managed to ensure that the whole AIV process remained on schedule and give an insight into the
lessons learned from this process. We also show how the process of requirement verification for this complex system
was managed and documented. We describe how the risks associated with a single long duration test at operating
temperature were controlled so that the complete suite of environmental tests could be used to build up a full picture of
instrument compliance.
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.
MOONS is a new conceptual design for a Multi-Object Optical and Near-infrared Spectrograph for the Very Large
Telescope (VLT), selected by ESO for a Phase A study. The baseline design consists of ~1000 fibers deployable over a
field of view of ~500 square arcmin, the largest patrol field offered by the Nasmyth focus at the VLT. The total
wavelength coverage is 0.8μm-1.8μm and two resolution modes: medium resolution and high resolution. In the medium
resolution mode (R~4,000-6,000) the entire wavelength range 0.8μm-1.8μm is observed simultaneously, while the high
resolution mode covers simultaneously three selected spectral regions: one around the CaII triplet (at R~8,000) to
measure radial velocities, and two regions at R~20,000 one in the J-band and one in the H-band, for detailed
measurements of chemical abundances.
The grasp of the 8.2m Very Large Telescope (VLT) combined with the large multiplex and wavelength coverage of
MOONS – extending into the near-IR – will provide the observational power necessary to study galaxy formation and
evolution over the entire history of the Universe, from our Milky Way, through the redshift desert and up to the epoch
of re-ionization at z<8-9. At the same time, the high spectral resolution mode will allow astronomers to study chemical
abundances of stars in our Galaxy, in particular in the highly obscured regions of the Bulge, and provide the necessary
follow-up of the Gaia mission. Such characteristics and versatility make MOONS the long-awaited workhorse near-IR
MOS for the VLT, which will perfectly complement optical spectroscopy performed by FLAMES and VIMOS.
KEYWORDS: Fermium, Frequency modulation, Optical alignment, Mirrors, James Webb Space Telescope, Temperature metrology, Interferometry, Optical simulations, Data modeling, Sensors
We report on the alignment verification activities using optical visible techniques, and performed at ambient temperature
before and after environmental and qualification tests, on the Mid InfraRed Instrument (MIRI), one of the scientific
instruments on-board the James Webb Space Telescope (JWST). More specifically, the method developed to measure
some of the instrument key parameters, such as pupil shear and focus offset, is explained in details. We describe the
chosen approach, the associated common hardware, the initial set-up and alignment, then discuss the measurements
themselves and finally the data analysis, before concluding on the successful application of such approach to the optical
characterization of the MIRI flight model.
The Mid Infrared Instrument of the James Webb Space Telescope is equipped with an integral field unit (IFU)
spectrometer. The optical distortion in the image slicing and dispersive optics leads to non-uniform sampling
and a catenation of the spatial and spectral information on the detector plane. To enable the translation of
detector data to the three-dimensional data cube representing the two spatial and the spectral sky dimension,
we have built two software tools: The first is miri cube, an image reconstruction programme which translates
the detector data back into the sky cube. The second is an extended version of SpecSim, an IFU simulator which
simulates the image slicing and dispersion based on optical models of the instrument. With these tools we are
able to determine and implement the correct strategy for the end-to-end calibration of spectroscopy data during
the on-ground cryogenic test campaign.
The Verification Model (VM) of MIRI has recently completed an extensive programme of cryogenic testing, with the
Flight Model (FM) now being assembled and made ready to begin performance testing in the next few months. By
combining those VM test results which relate to MIRI's scientific performance with measurements made on FM
components and sub-assemblies, we have been able to refine and develop the existing model of the instrument's
throughput and sensitivity.
We present the main components of the model, its correlation with the existing test results and its predictions for
MIRI's performance on orbit.
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.
The ISS (Integral-field Spectrograph System) has been designed as part of the EAGLE Phase A Instrument Study for the
E-ELT. It consists of two input channels of 1.65x1.65 arcsec field-of-view, each reconfigured spatially by an imageslicing
integral-field unit to feed a single near-IR spectrograph using cryogenic volume-phase-holographic gratings to
disperse the image spectrally. A 4k x 4k array detector array records the dispersed images. The optical design employs
anamorphic magnification, image slicing, VPH gratings scanned with a novel cryo-mechanism and a three-lens camera.
The mechanical implementation features IFU optics in Zerodur, a modular bench structure and a number of highprecision
cryo-mechanisms.
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.
KEYWORDS: Mirrors, Telescopes, Monochromatic aberrations, Image quality, Cameras, Simulation of CCA and DLA aggregates, Image segmentation, Wavefront sensors, Wavefronts, Interfaces
Construction of the Southern African Large Telescope (SALT) was largely completed by the end of 2005 and since then
it has been in intensive commissioning. This has now almost been completed except for the telescope's image quality
which shows optical aberrations, chiefly a focus gradient across the focal plane, along with astigmatism and other less
significant aberrations. This paper describes the optical systems engineering investigation that has been conducted since
early 2006 to diagnose the problem. A rigorous approach has been followed which has entailed breaking down the
system into the major sub-systems and subjecting them to testing on an individual basis. Significant progress has been
achieved with many components of the optical system shown to be operating correctly. The fault has been isolated to a
major optical sub-system. We present the results obtained so far, and discuss what remains to be done.
KEYWORDS: James Webb Space Telescope, Systems engineering, Interfaces, Thermography, Calibration, Spectroscopy, Document management, Optical filters, Scanning tunneling microscopy, Imaging systems
This paper elaborates the system engineering methods that are being successfully employed within the European
Consortium (EC) to deliver the Optical System of the Mid Infa-Red Instrument (MIRI) to the James Webb Space
Telescope (JWST).
The EC is a Consortium of 21 institutes located in 10 European countries and, at instrument level, it works in a 50/50
partnership with JPL who are providing the instrument cooler, software and detector systems.
The paper will describe how the system engineering approach has been based upon proven principles used in the space
industry but applied in a tailored way that best accommodates the differences in international practices and standards
with a primary aim of ensuring a cost-effective solution which supports all science requirements for the mission.
The paper will recall how the system engineering has been managed from the definition of the system requirements in
early phase B, through the successful Critical Design Review at the end of phase C and up to the test and flight build
activities that are presently in progress. Communication and coordination approaches will also be discussed.
The James Webb Space Telescope (JWST) is a space-based, infrared observatory designed to study the early stages of
galaxy formation in the Universe. It is currently scheduled to be launched in 2013 and will go into orbit about the
second Lagrange point of the Sun-Earth system and passively cooled to 30-50 K to enable astronomical observations
from 0.6 to 28 μm. The JWST observatory consists of three primary elements: the spacecraft, the optical telescope
element (OTE) and the integrated science instrument module (ISIM). The ISIM Element primarily consists of a
mechanical metering structure, three science instruments and a fine guidance sensor with significant scientific capability.
One of the critical opto-mechanical alignments for mission success is the co-registration of the OTE exit pupil with the
entrance pupils of the ISIM instruments. To verify that the ISIM Element will be properly aligned with the nominal
OTE exit pupil when the two elements come together, we have developed a cryogenic pupil measurement test
architecture to measure three of the most critical pupil degrees-of-freedom during optical testing of the ISIM Element.
The pupil measurement scheme makes use of: specularly reflective pupil alignment references located inside of the
JWST instruments; ground support equipment that contains a pupil imaging module; an OTE simulator; and pupil
viewing channels in two of the JWST flight instruments. Current modeling and analysis activities indicate this
measurement approach will be able to verify pupil shear to an accuracy of 0.5-1%.
The Mid-Infrared Instrument (MIRI) is one of the three scientific instruments to fly on the James Webb Space
Telescope (JWST), which is due for launch in 2013. MIRI contains two sub-instruments, an imager, which has low
resolution spectroscopy and coronagraphic capabilities in addition to imaging, and a medium resolution IFU
spectrometer. A verification model of MIRI was assembled in 2007 and a cold test campaign was conducted between
November 2007 and February 2008. This model was the first scientifically representative model, allowing a first
assessment to be made of the performance. This paper describes the test facility and testing done. It also reports on the
first results from this test campaign.
Segmented primary mirrors dominate the current generation of 10m class telescopes as well as the designs for the next
generation of Extremely Large Telescopes (ELT's). The complex nature of these telescopes is demonstrated by the long
time periods associated with their commissioning and the difficulty of performing high precision optical alignments.
However, additional tools to provide in situ measurements of their optical alignment can be provided by making use of
the individual mirrors of a segmented primary; with the ability to move in six degrees of freedom, the individual mirrors
can be deployed to trace multiple optical paths through the telescope. In this paper we describe how it is possible to use
the segments themselves to create a number of Hartmann masks that allow focus and other aberrations to be measured
using a standard imaging camera rather than a dedicated wavefront sensor. The Southern African Large Telescope
(SALT), with a primary mirror composed of 91 1m segments, is used as an example. The segments were arranged to
create eight Hartmann masks to measure the optical alignment. Through imaging data obtained at the telescope, the
sensitivity of this method to changes in focus along with aberrations inherent in the system is demonstrated through
Zernike polynomial fits to the observed patterns. Finally, we present simulations of possible patterns for use on future
ELT's.
This paper summarizes the different optical concepts developed for the EAGLE Phase A design. EAGLE will be an
MOAO (Multi-object AO) IFU spectrometer operating between 0.8 and 2.5μm. The EAGLE consortium have
developed different concepts for the challenging problem of acquiring more than twenty objects in the patrol field of
view (FOV), correcting the wavefront along the line of sight to each of the objects and analyzing each object spatially
and spectrally with an Integral Field Spectrograph. The target selection FOV will be ≥20 square arcmin and the
individual target FOV can be selected to be either 1.65×1.65arcsec or 1.65×3.3arcsec. They will be sampled spatially at
75mas and with spectral resolutions of 4000 and 10000. Optical designs for target acquisition systems, integral-field
unit, and spectrographs have been developed. These will be compared and the expected performance will be described
in terms of the number of targets, overall patrol field of view, individual field of view, throughput, spectral resolving
power and image quality.
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.
We present designs for compact near-IR spectrometers with mid to high resolving powers. They use an innovative
combination of integral-field units and immersed gratings, both with and without cross-dispersion. The advent of ELTs
with scientific requirements for multi-channel instruments (e.g. EAGLE) with high resolving powers has led to designs
for spectrometers which are made more compact by using immersed gratings and are capable of high spectral resolving
power by including cross dispersion and an arrangement of the IFU output that provides the requisite short slit.
Recent advances in the design of all reflective integral field units have led engineers to look for new techniques to manufacture monolithic mirror arrays for use in such instruments. One such design is being developed at the UKATC for use on the Mid-Infrared Instrument (MIRI) on the James Webb Space telescope. The MIRI instrument will contain four integral field units with image slicer and re-imaging mirror arrays manufactured at Cranfield University. The mirror arrays have been designed with particular attention to the requirements of precision machining and subsequent metrology. The philosophy of "design for manufacture" has led to the production of mirror arrays with unrivalled levels of accuracy. Initially, this paper will describe the opto-mechanical design of the mirror arrays. The paper will then discuss the diamond turning manufacturing technique specially developed to machine these complex components. The paper will also describe the precision metrology capability developed specifically for the MIRI project that is used to accurately measure mirror locations and surface form errors. Finally, the paper will present the results obtained so far for the mirror arrays being prepared for the IFU verification model and prototype.
The MIRI Medium Resolution Spectrometer (MIRI-MRS) will increase the sensitivity of astronomical spectroscopy at thermal infrared wavelengths (from 5 to 28 microns), by a factor of 1000 over the best that can be achieved by existing ground-based instruments. This leap in performance is further enhanced by the first use at these wavelengths of all reflective Integral Field Units (image slicers) to provide the spectrometer with a rectangular field of view with a shortest dimension of 3.5 arcseconds.
We describe the optical design of the MRS and present predictions for its delivered image quality.
KEYWORDS: Telescopes, Sensors, Spectroscopy, James Webb Space Telescope, Imaging systems, Diffraction, Mid-IR, Space telescopes, Point spread functions, Optical filters
Modelling the scientific performance of infrared instruments during the design and definition phase of a project is an essential part of the system design optimisation for both the instrument and the observatory. This is particularly so in the case of space observatories where the opportunities for correcting design errors or omissions following launch are limited. We describe the approach taken to the estimation of the sensitivity of the Mid Infrared Instrument (MIRI) operating from 5 to 28 microns on the NASA/ESA James Webb Space Telescope (JWST) due for launch in 2011. We show how the sensitivity is estimated both for the photometric imager and the integral field spectrometer using a model that includes the effects of background radiation from the telescope and its surroundings; diffraction effects and detector performance and operations.
The spectrometer sub-system of the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) contains four channels which spectrally multiplex the incoming radiation. This incident radiation, spanning a wavelength range from 4.8 to 28.8μm is spectrally divided between the channels using sets of three dichroics combined in series along the optical trains. The four channels, with overlapping wavelengths 4.8-7.8, 7.4-11.9, 11.4-18.3 and 18.3-28.8μm, are in-turn each split into three wavelength ranges to provide the required resolving power with the available detector pixels. This splitting of the wavelengths within each channel is achieved using three separate sets of dichroics and diffraction gratings, mounted on two wheels.
This paper describes the design of the dichroics together with a spectral performance model developed to simulate the system spectral throughput for each of the four channels of the MIRI instrument. Details of the spectral design, manufacture, testing and mounting of the dichroics are presented together with the opto-mechanical layout of the instrument.
The James Webb Space Telescope (JWST) Observatory, the follow-on mission to the Hubble Space Telescope and to the Spitzer Space Facility, will yield astounding breakthroughs in the realms of infrared space science. The science instrument suite for this Observatory will consist of a Near-Infrared Camera, a Near-Infrared Spectrograph, a Mid-Infrared Instrument with imager, coronagraph and integral field spectroscopy modes, and a Fine Guider System Instrument with both a Guider module and a Tunable Filter Module. In this paper we present an overview of the optical designs of the telescope and instruments.
We present the results of a design study for the spectrograph module for KMOS - a cryogenic near-infrared multi-object spectrograph being developed as a second generation instrument for the VLT by a consortium of UK and German institutes. KMOS will consist of 24 deployable integral field units feeding three identical spectrograph units via image slicers. The spectrographs are designed to provide a resolving power greater than 3000, so as to provide adequate OH avoidance, whilst covering one of the J, H or K bands within a single exposure. We present the opto-mechanical layout of the spectrographs, together with an analysis of the impact of the image quality (and PSF uniformity) on the accuracy of sky background subtraction within each IFU's field of view.
A prototype cryogenic 'pick-off' arm for selecting a small field from the focal plane of a large telescope has been built and tested against a set of scientific requirements representative of those for proposed multi-integral-field spectrographs. In this paper, we present the design of the arm and the results of the cryogenic testing. Since the proposed instruments will require tens of arms, perhaps hundreds, we have also considered the industrialisation of the manufacture and assembly of the arms. We briefly discuss this aspect of the design and the possibilities for future instrumentation on Extremely Large Telescopes.
This paper describes our approach to the design of reflective, image-slicing Integral-Field Units. The first IFU built at the UK ATC (Ramsay-Howat et al 2004) has been successfully commissioned and is in routine use on the UKIRT. This IFU uses all diamond-turned optics and close attention was paid in the design to the manufacturability of the individual components, their alignment into groups and the overall alignment and integration of the IFU into the spectrometer. Building on this experience we are designing and making four IFUs for the MIRI on JWST where constraints on mass and launch survivability have led us to use monolithic arrays of slicing and re-imaging mirrors. This paper describes the ways in which the optical design and the manufacturing methods have each been adapted to: (a) achieve image quality, pupil alignment and mass requirements (b) ensure components can be reliably manufactured to the tolerances needed so that the IFUs can be aligned without adjustment and (c) ensure that performance is maintained after launch and cooling to 7 K. We also show that, although designed specifically for a space instrument, such a compact and reproducible IFU is well suited to instruments where multiple IFUs are required.
We present the results of a detailed technical study of the use of image slicers for multiple integral field spectroscopy at infrared wavelengths. Our solution uses independently controlled robotic arms to relay selected portions of the focal plane to fixed positions where they are dissected using a set of advanced image slicers. We discuss the technical requirements of this approach and describe a feasibility study to examine the risks and technical challenges.
MIRI, the mid-IR instrument for NGST is being provided by a collaboration between a consortium of European institutes, ESA, NASA, JPL and US scientists, with the Europeans responsible for the optics module. The instrument will provide diffraction limited imaging and spectroscopic capability over the 5-28μm region with unprecedented sensitivity. In this paper we describe the current optical design of the medium resolution spectroscopy channel (MIRI-S). This uses a novel arrangement of dichroics, image slicers and spectrometers to optimise the division of a limited number of detector pixels between spatial and spectral information whilst working within the tight mass and volume constraints imposed by a space mission. We also present our design for reflective image slicers that are adapted properly for diffraction limited performance to provide a high throughput over the full wavelength range of the instrument.
NAOMI (Nasmyth Adaptive Optics for Multi-purpose Instrumentation) is a recently completed and commissioned astronomical facility on the 4.2m William Herschel Telescope. The system is designed to work initially with Natural Guide Stars and also to be upgradeable for use with a single laser guide star. It has been designed to work with both near infrared and optical instrumentation (both imagers and spectrographs). The system uses a linearised segmented adaptive mirror and dual-CCD Shack-Hartmann wavefront sensor together with a multiple-DSP real-time processing system. Control system parameters can be updated on-the-fly by monitoring processes and the system can self-optimize its base optical figure to compensate for the optical characteristics of attached scientific instrumentation. The scientific motivation, consequent specification and implementation of NAOMI are described, together with example performance data and information on future upgrades and instrumentation.
VISTA is the Visible and Infrared Survey Telescope for Astronomy that has been designed by the UK ATC. The design incorporates two cameras covering the visible and near-IR wavelengths. An important concern in designing the telescope and cameras is the level of stray, scattered and background light. In the IR camera, K-band (approx. 2.0-2.3 microns) thermal emission from the telescope structure contributes ~50% of the sky background. Therefore a cold baffle is necessary. Due to the large field-of-view, and size of the required optics, a cold stop is precluded. Therefore baffling is provided by a long cryostat and a system of cold baffles with a coating that must absorb in-band light but reflect thermal radiation from the cryostat window, thus reducing the thermal load on the cryostat. In addition, the temporally and spatially variable OH airglow from the atmosphere is obscured by a warm (and hence non-absorbing) annular baffle around the secondary mirror. We report here on the modelling of the scattered and background light for VISTA. The model includes accurate models for the geometry of baffles and optical surface properties of all surfaces in the system. The optical specification is taken from a ZEMAX model and imported into TracePro to generate a fully three-dimensional telescope model, with a simple dome. For both cameras the analysis has been done for the case of scattered light from a full moon at various incident angles from 0 degrees (on axis) to 65 degrees. It is shown that a reflective baffle around the secondary mirror does not significantly impair the performance of the visible camera. Ghosting from bright stars in the field has also been calculated for both cameras. Results indicate that the level of scattered and ghosts is below the limits specified for VISTA.
We present here details of the manufacture of a deployable image
slicing IFU for UIST (a new imager spectrometer for UKIRT). We also
present the alignment methods developed and used to achieve optimal
transmission and give results for laboratory testing of the IFU at
cryogenic temperatures in its operational configuration in UIST.
These tests covered transmission, scattered light, alignment of exit pupils and the spatial and spectral PSFs. The calibration and
automatic data reduction methods which produce spectra (in the form
of an x, y, λ data-cube) aligned in wavelength and the two spatial dimensions for all the observed pixels will be described.
Gemini have funded a design study to investigate the technologies needed in a versatile multi-object spectrograph for IR astronomy. We report on our investigations into wide- field spectroscopy using multiple integral-field units (MIFUs) to match particular areas of interest to the available detector(s). Such technologies enable integral field spectroscopy of several targets over a much wider field than can be covered with a single IFU. A brief overview of the scientific rationale for a multipel0IFU capability matched to multi-conjugate adaptive optics, and with its wider uncorrected field, on Gemini is given. A proposed method of deploying MIFUs is then described along with the optical consequences of the method.
We present results on the integration and testing of an imaging spectrometer for the 1-5micrometers wavelength band. UIST offers high angular resolution imaging and spectroscopy and has been designed to exploit the best performance of the UK IR Telescope. In addition to imaging with 0.24arcsec and 0.12arcsec resolution, long-slit and cross-dispersed spectroscopy, UIST has an integral field mode using a reflective image slicer. An image rotator allows the slits and the rectangular field of view of the IFU to be oriented at any position angle on the sky. The UIST optical design relies on refractive optics with the spectroscopy provided by both replicated and direct-ruled grisms. The lenses are mounted in mechanical modules which also contain the mechanisms, such as the filter and slit wheels. The integration of the opto-mechanical system will be discussed. The high tolerances on positioning the optical components to be used under cryogenic conditions are achieved by mechanical alignment on an optical bench which is an integral part of the instrument. Initial tests of the cryogenic performance of the optics will be presented. The UIST detector is an 1024 by 1024 InSb 'ALADDIN' array from the Raytheon IR Center of Excellence. The array controller is modified from 'EDICT', a VME processor based system which was developed at the UK ATC to control the mid-IR arrays used in the MICHELLE spectrometer. Progress on the integration of the UIST detector and controller will be discussed.
We present her the opto-mechanical design of an image slicer with reference to designs for a deployable IFU for UIST and two mid-IR IFUs for NGST. Particular attention is paid to how the design achieves a number of goals required of an IFU working in an astronomical IR instrument.
The design of any modern astronomical telescope requires close interaction between the science requirements, the optical and mechanical design of the telescope and its instrumentation. In addition new, large aperture, telescopes will need to have adaptive optics as an integral part of the concept. This paper discusses optical concepts for the telescope and instruments, highlighting technology challenges.
We present the design of a mid-IR (5 - 28 micrometers ) integral field spectrometer for NGST. Details of the opto-mechanical design are given with particular attention being paid to those aspects influenced by the cryogenic, low background space environment in which the instrument needs to work. The instrument consists of three subsections: fore-optics and image slicing integral field units (IFU's), a 5 - 10 micrometers spectrograph and 10 - 28 micrometers spectrograph. Two co-aligned fields of view are separated into two wavelength channels (5 - 10 and 10 - 28 micrometers ) by a dichroic mirror in the fore- optics which also re-image the telescope focal plane onto the slicing mirrors of two IFU's.
Previous work has shown that atmospheric distortions are predictable. We present preliminary results which show that introducing predictors into the control loop of an adaptive optics system with a zero hysteresis segmented mirror improves systems performance.
An imaging spectrometer is being designed to take advantage of recent improvements in the image quality achieved at the UK Infrared Telescope. The realization of near-diffraction limited imaging at two microns brings with it the possibility of significant improvements in sensitivity to IR observations. UIST will provide a versatile facility for high spatial resolution imaging and spectroscopy in the 1-5 micrometers wavelength range. We will present the opto-mechanical design of this new instrument, highlighting the innovative features. These include provision of multiple pixel scales within the camera and polarimetry via a Wollaston prism. One of the most challenging areas of the design is the inclusion of a cryogenic integral field unit for area spectroscopy over a 5 inch field. The spectroscopic modes include cross- dispersed spectroscopy over the complete 1-2.5 micrometers wavelength ranges and moderate resolution long slit or area spectroscopy over the complete 1-5 micrometers range. A higher resolution mode will also the included. This will allow USTI to take advantage of the very low backgrounds to be found between OH sky lines. The instruments will incorporate a 1024 X 1024 Indium Antimonide array from SBRC. The development of the IR array controller for UIST will also be discussed.
A conceptual design for the WHT Natural Guide Star Adaptive Optics system, now called NAOMI (Nasmyth Adaptive Optics for Multi-purpose Instrumentation) was presented at the 1995 SPIE meeting1. Although the general principle of using off-axis paraboloidal mirrors (OAP) as a collimator- camera combination, with a deformable mirror located between them in the collimated beam, remains the same many features of the design have been improved.
The United Kingdom is funding a program of astronomical adaptive optics (AO), the primary purpose of which is to equip two 4-meter telescopes with common-user (facility) natural guide star AO systems: the 4.2 m William Herschel Telescope on La Palma in the Canary Islands and the 3.8 m United Kingdom Infrared Telescope on Mauna Kea, Hawaii. The program also supports related developments in the following fields: site evaluation (on La Palma and Mauna Kea), IR instrumentation, adaptive secondary mirror design, partial AO, and laser beacons (for La Palma). The structure, purposes, and timescales of the overall program are described. In general, the goal is to deliver AO systems which have wide astronomical application and provide well-optimized performance in a wide range of environmental conditions. The ways in which this goal has conditioned the program are outlined.
The UK Adaptive Optics program is funded to provide common user adaptive optics facilities for UK telescopes. One phase of this program aims to provide an adaptive optical system for the 4.2 m William Herschel Telescope (WHT), sited on La Palma in the Canary Islands. The WHT natural guide star (NGS) adaptive optics system is specified to have optimum correction at 2.2 micrometer in typical to good site seeing conditions. The initial detector system is an infrared camera with a 256 multiplied by 256 InSb array detector. The system will be mounted at the Nasmyth focus on the GHRIL (General High Resolution Imaging Laboratory) optical bench. The AO system optical design currently uses a conventional pupil imaged deformable mirror and an 8 multiplied by 8 Shack Hartmann wavefront sensor (WFS). A CCD camera is intended as the wavefront sensor detector, based on a 64 multiplied by 64 or 80 multiplied by 80 pixel detector array. Modes for turbulent layer conjugation are currently being investigated. It is intended that the system should be a common-user facility. Therefore functions of system configuration, alignment, and operation are being designed to be operated by non-specialists, so that the facility can be used in the same way as one of the standard suite of instruments available for the telescope. This paper describes the current conceptual design of the system.
A novel form of Shack-Hartmann wavefront sensor is described which can be used in existing infrared and visible cameras with only minimal disturbance to their optics. Such a device has been installed in IRCAM3, the common-user IR camera on UKIRT (United Kingdom Infrared Telescope). The camera's fast readout electronics and a purpose built data storage system allows the wavefront slopes to be measured in 25 sub-apertures at frame rates of between 30 and 100 per second. The first spatially and temporally resolved IR wavefront measurements are presented and an outline is given of the use of this wavefront sensor for long term monitoring on both Mauna Kea, Hawaii and La Palma, Canary Islands.
This paper reports the results of some experiments on wavefront sensing at La Palma, Canary Is., using a Shack-Hartmann sensor. From the Shack-Hartmann data, we derive estimates of the seeing parameter r0 and compare different methods of wavefront reconstruction: a new method of wave front reconstruction based on Bayes' theorem is presented. The design of a Shack-Hartmann sensor for operation at 2 micrometers on UKIRT is described.
The Infrared Space Observatory (ISO) photometer is one of four instruments on board the European Space Agency ISO satellite scheduled for launch in September 1995. It covers the wavelength range 2.5 to 240 μm with wide and narrow spectral bands. Diffraction-limited observations as well as wide-beam measurements of faint extended sources are possible. Polarimetric observations can be made over the whole wavelength range. The minimal detectable flux is ~10 mJy. The astronomical areas to be addressed range from solar system objects to cosmology.
ISOPHOT is one of four instruments onboard the ESA Infrared Space Observatory scheduled for launch in September 1995. It covers the wavelength range 2.5 micrometers to 240 micrometers with wide and marrow spectral bands. Diffraction limited observations as well as wide beam measurements of faint extended sources are possible. Polarimetric observation can be made over the whole wavelength range. The minimal detectable flux is approximately 10 mJy. The astronomical areas to be addressed range from solar system objects to cosmology.
The optical design of Isophot-S, the low-resolution NIR spectrophotometer for the IR Space Observatory (ISO), is described and illustrated with drawings and graphs of test data. The ISO is to be launched in 1993 as a successor to IRAS for astronomical surveys at 2.5-200 microns. Isophot-S has an aperture of 24 arcsec sq, and the two 64-pixel Si:Ga detector arrays have noise-equivalent power of about 5 x 10 to the -17th W/sq rt Hz at 15 microns, corresponding to 1-sigma 1-sec detection sensitivity 400 mJy for a point source at 12 microns or surface brightness 0.8 mJy/sq arcsec for an extended source. The system comprises two grating spectrometers, one operating at 2.5-5 microns with resolution 40 nm and one operating at 6-12 microns with resolution 90 nm.
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