ESO’s Very Large Telescope Interferometer has a history of record-breaking discoveries in astrophysics and significant advances in instrumentation. The next leap forward is its new visitor instrument, called Asgard. It comprises four natively collaborating instruments: HEIMDALLR, an instrument performing both fringe tracking and stellar interferometry simultaneously with the same optics, operating in the K band; Baldr, a Strehl optimizer in the H band; BIFROST, a spectroscopic combiner to study the formation processes and properties of stellar and planetary systems in the Y-J-H bands; and NOTT, a nulling interferometer dedicated to imaging nearby young planetary systems in the L band. The suite is in its integration phase in Europe and should be shipped to Paranal in 2025. In this article, we present details of the alignment and calibration unit, the observing modes, the integration plan, the software architecture, and the roadmap to completion of the project.
BIFROST, an upcoming instrument for the VLTI, is part of the Asgard Suite, a VLTI visitor instrument. It comprises two spectrograph arms that are optimised for wavelength range of 1- 1.75μm (fed by a fiber that is placed on-axis for fringe tracking/monitoring) and 1-1.3μm (fed by a fiber that can positioned either on-axis or off-axis to observe a faint target) wavelength range, respectively. Volume phase holographic gratings (VPHGs) are employed to achieve high spectral resolving power up to 25,000 and a throughput above 75% for all dispersing elements. In this contribution, we discuss the optical and optomechanical design of the spectrographs, as well as a new relay optics design that minimizes the thermal background, with a factor 4 reduction in thermal background compared to the non-relay optics design. We will also present the first lab results obtained with the YJH spectrograph.
NOTT (formerly Hi-5) is the L’-band (3.5-4.0μm) nulling interferometer of Asgard, an instrument suite in preparation for the VLTI visitor focus. The primary scientific objectives of NOTT include characterizing (i) young planetary systems near the snow line, a critical region for giant planet formation, and (ii) nearby mainsequence stars close to the habitable zone, with a focus on detecting exozodiacal dust that could obscure Earthlike planets. In 2023-2024, the final warm optics have been procured and assembled in a new laboratory at KU Leuven. First fringes and null measurements were obtained using a Gallium Lanthanum Sulfide (GLS) photonic chip that was also tested at cryogenic temperatures. In this paper, we present an overall update of the NOTT project with a particular focus on the cold mechanical design, the first results in the laboratory with the final NOTT warm optics, and the ongoing Asgard integration activities. We also report on other ongoing activities such as the characterization of the photonic chip (GLS, LiNbO3, SiO), the development of the exoplanet science case, the design of the dispersion control module, and the progress with the self-calibration data reduction software.
The simultaneous push to unprecedented contrast, spectral and spatial resolution at the Very Large Telescope Interferometer (VLTI), as promised by the Asgard instrument suite, requires unprecedented high Strehl ratios and phase-front stability. This will be the job of Baldr: a new J or H band Zernike wavefront sensor (ZWFS) used as a second stage adaptive optics (AO) system for the VLTI/Asgard instrument suite. ZWFS was selected for Baldr due to its optimal photon sensitivity and the need for Baldr to be extremely low latency to reduce the residuals from the first stage AO systems. Here we briefly present the design of Baldr which uses a novel architecture where all four Baldr beams for adaptive optics from each telescope are sensed with a low-latency C-RED One detector, permitting AO frame rates up to 3.5kHz. With this architecture simulations show that the Baldr design can deliver J-band Strehl ratios for the 1.8m Auxiliary Telescopes (AT’s) of over 80%, which is a significant improvement on the Strehl ratios otherwise delivered to Asgard, which would limit the scientific objectives of the instrument. Finally we present preliminary test-bed results and give an overview of progress and future work.
The Asgard instrument suite proposed for the ESO’s Very Large Telescope Interferometer (VLTI) brings with it a new generation of instruments for spectroscopy and nulling. Asgard will enable investigations such as measurement of direct stellar masses for Galactic archaeology and direct detection of giant exoplanets to probe formation models using the first nulling interferometer in the southern hemisphere. We present the design and implementation of the Astralis-built Heimdallr, the beam combiner for fringe tracking and stellar interferometry in K band, as well as Solarstein, a novel implementation of a 4-beam telescope simulator for alignment and calibration. In this update, we verify that the Heimdallr design is sufficient to perform diffraction-limited beam combination. Furthermore, we demonstrate that Solarstein presents an interface comparable to the VLTI with co-phased, equal intensity beams, enabling alignment and calibration for all Asgard instruments. In doing so, we share techniques for aligning and implementing large instruments in bulk optics.
European Southern Observatory (ESO)’s Very Large Telescope Interferometer (VLTI), Paranal, Chile, is one of the most proficient observatories in the world for high angular resolution astronomy. It has hosted several interferometric instruments operating in various bandwidths in the infrared. As a result, the VLTI has yielded countless discoveries and technological breakthroughs. We propose to ESO a new concept for a visitor instrument for the VLTI: Asgard. It is an instrumental suite comprised of four natively collaborating instruments: High-Efficiency Multiaxial Do-it ALL Recombiner (HEIMDALLR), an all-in-one instrument performing both fringe tracking and stellar interferometry with the same optics; Baldr, a Strehl optimizer; Beam-combination Instrument for studying the Formation and fundamental paRameters of Stars and planeTary systems (BIFROST), a combiner whose main science case is studying the formation processes and properties of stellar and planetary systems; and Nulling Observations of dusT and planeTs (NOTT), a nulling interferometer dedicated to imaging young nearby planetary systems in the L band. The overlap between the science cases across different spectral bands yields the idea of making the instruments complementary to deliver sensitivity and accuracy from the J to L bands. Asgard is to be set on the former AMBER optical table. Its control architecture is a hybrid between custom and ESO-compliant developments to benefit from the flexibility offered to a visitor instrument and foresee a deeper long-term integration into VLTI for an opening to the community.
The Gemini High Resolution Optical Spectrograph (GHOST) is the next generation high resolution spectrograph for the Gemini South Observatory, and this has recently been commissioned in May 2021. In a single exposure, it can obtain the full optical spectrum from blueward of 360nm to beyond 1 micron. Two modes of operation mean that either one object can be observed at R~80000, or two objects can be observed at R~55000. First light results have tested all aspects of the scientific performance of GHOST from the science user perspective, including a range of aquisition procedures and its two spectral resolution modes. On-sky observations of scientific and library targets reveal GHOST to be the most sensitive spectrograph across the full optical range of any of the 8-10m class spectrographs currently in operation. This paper presents a full discussion of the commissioning process, tests, on-sky performance and first science observations.
The Very Large Telescope Interferometer is one of the most proficient observatories in the world for high angular resolution. Since its first observations, it has hosted several interferometric instruments operating in various bandwidths in the infrared. As a result, the VLTI yields countless discoveries and technological breakthroughs. We introduce to the VLTI the new concept of Asgard: an instrumental suite including four natively collaborating instruments: BIFROST, a stellar interferometer dedicated to the study of the formation of multiple systems; Hi- 5, a nulling interferometer dedicated to imaging young nearby planetary systems in the M band; HEIMDALLR, an all-in-one instrument performing both fringe tracking and stellar interferometry with the same optics; Baldr, a fibre-injection optimiser. These instruments share common goals and technologies. Thus, the idea of this suite is to make the instruments interoperable and complementary to deliver unprecedented sensitivity and accuracy from J to M bands. The interoperability of the Asgard instruments and their integration in the VLTI are the main challenges of this project. In this paper, we introduce the overall optical design of the Asgard suite, the different modules, and the main challenges ahead.
GHOST is a high resolution spectrograph system currently being built for the Gemini South Observatory in Chile. In the Cassegrain unit, the observational targets are acquired on integral field units and guided during science exposures, feeding the fiber cable to the temperature-stabilized echelle spectrograph. The Cassegrain unit is mounted on the Gemini telescope, and consists of a main structural plate, the two object positioners and ballast frame. The image from each of the two science beams passes through a field lens and a mini-atmospheric dispersion corrector and is then captured by the integral field unit. The positioner moves each corrector-integral field unit assembly across the focal surface of the telescope. The main structural plate provides the interface for the positioner and ballast frame to the telescope structure. In this paper we describe the final design and assembly of the GHOST Cassegrain unit and report on the outcome of on-sky testing at the telescope in Chile.
The Gemini High-Resolution Optical SpecTrograph (GHOST) is the newest instrument chosen for the Gemini South telescope. It is being developed by a collaboration between the Australian Astronomical Observatory (AAO), the NRC - Herzberg in Canada and the Australian National University (ANU). Using recent technological advances and several novel concepts it will deliver spectroscopy with R>50,000 for up to 2 objects simultaneously or R>75,000 for a single object. GHOST uses a fiber-image-slicer to allow use of a much smaller spectrograph than that nominally required by the resolution-slit–width product. With its fiber feed, we expect GHOST to have a sensitivity in the wavelength range between 363-950 nm that equals or exceeds that of similar directly-fed instruments on world-class facilities. GHOST has entered the build phase. We report the status of the instrument and describe the technical advances and the novel aspects, such as the lenslet-based slit reformatting. Finally, we describe the unique scientific role this instrument will have in an international context, from exoplanets through stellar elemental abundances to the distant Universe. Keywords: Gemini, spectrograph, spectroscopy, ́echelle, high resolution, radial velocity, fiber image slicer, integral field unit.
Gemini High-Resolution Optical SpecTrograph (GHOST) is a fiber-fed spectrograph being developed for the Gemini telescope. GHOST is a white pupil échelle spectrograph with high efficiency and a broad continuous wavelength coverage (363-1000nm) with R>50,000 in two-object mode and >75,000 in single-object mode. The design incorporates a novel zero-Petzval sum white pupil relay to eliminate grating aberrations at the cross-dispersers. Cameras are based on non-achromatic designs with tilted detectors to eliminate the need for exotic glasses. This paper outlines the optical design of the bench-mounted spectrograph and the predicted spectrograph resolution and efficiency for the spectrograph.
The Gemini High-resolution Optical SpecTrograph (GHOST) is a fiber fed spectrograph primarily designed for high efficiency and broad wavelength coverage (363 -1000nm), with an anticipated commissioning early in 2018. The primary scientific goal of the Precision Radial Velocity (PRV) mode will be follow-up of relatively faint (R>12) transiting exoplanet targets, especially from the TESS mission. In the PRV mode, the 1.2 arcsec diameter stellar image will be split 19 ways, combined in a single slit with a simultaneous Th/Xe reference source, dispersed at a resolving power of 80,000 and imaged onto two detectors. The spectrograph will be thermally stabilized in the Gemini pier laboratory, and modal noise will be reduced below other sources through the use of a fiber agitator. Unlike other precision high resolution spectrographs, GHOST will not be pressure controlled (although pressure will be monitored precisely), and there will be no double scrambler or shaped (e.g. octagonal) fibers. Instead, GHOST will have to rely on simultaneous two-color imaging of the slit and the simultaneous Th/Xe fiber to correct for variable fiber illumination and focal-ratio degradation. This configuration presents unique challenges in estimating a PRV error budget.
KEYWORDS: Stars, Visibility, Interferometers, Data modeling, Interferometry, Modulation, Calibration, Signal to noise ratio, Error analysis, Binary data
The conventional approach to high-precision narrow-angle astrometry using a long baseline interferometer is to directly measure the fringe packet separation of a target and a nearby reference star. This is done by means of a technique known as phase-referencing which requires a network of dual beam combiners and laser metrology systems. Using an alternative approach that does not rely on phase-referencing, the narrow-angle astrometry of several closed binary stars (with separation less than 2′′), as described in this paper, was carried out by observing the fringe packet crossing event of the binary systems. Such an event occurs twice every sidereal day when the line joining the two stars of the binary is is perpendicular to the projected baseline of the interferometer. Observation of these events is well suited for an interferometer in Antarctica. Proof of concept observations were carried out at the Sydney University Stellar Interferometer (SUSI) with targets selected according to its geographical location. Narrow-angle astrometry using this indirect approach has achieved sub-100 micro-arcsecond precision.
The Gemini High-Resolution Optical SpecTrograph (GHOST) is the newest instrument being developed for the Gemini telescopes, in a collaboration between the Australian Astronomical Observatory (AAO), the NRC - Herzberg in Canada and the Australian National University (ANU). We describe the process of design optimisation that utilizes the unique strengths of the new partner, NRC - Herzberg, the design and need for the slit viewing camera system, and we describe a simplification for the lenslet-based slit reformatting. Finally, we out- line the updated project plan, and describe the unique scientific role this instrument will have in an international context, from exoplanets through to the distant Universe.
As telescopes get larger, the size of a seeing-limited spectrograph for a given resolving power becomes larger also, and for ELTs the size will be so great that high resolution instruments of simple design will be infeasible. Solutions include adaptive optics (but not providing full correction for short wavelengths) or image slicers (which give feasible but still large instruments). Here we develop the solution proposed by Bland-Hawthorn and Horton: the use of diffraction-limited spectrographs which are compact even for high resolving power. Their use is made possible by the photonic lantern, which splits a multi-mode optical fiber into a number of single-mode fibers. We describe preliminary designs for such spectrographs, at a resolving power of R ~ 50,000. While they are small and use relatively simple optics, the challenges are to accommodate the longest possible fiber slit (hence maximum number of single-mode fibers in one spectrograph) and to accept the beam from each fiber at a focal ratio considerably faster than for most spectrograph collimators, while maintaining diffraction-limited imaging quality. It is possible to obtain excellent performance despite these challenges. We also briefly consider the number of such spectrographs required, which can be reduced by full or partial adaptive optics correction, and/or moving towards longer wavelengths.
The Gemini High-Resolution Optical SpecTrograph (GHOST) will fill an important gap in the current suite of Gemini
instruments. We will describe the Australian Astronomical Observatory (AAO)-led concept for GHOST, which consists
of a multi-object, compact, high-efficiency, fixed-format, fiber-fed design. The spectrograph itself is a four-arm variant
of the asymmetric white-pupil echelle Kiwispec spectrograph, Kiwisped, produced by Industrial Research Ltd. This
spectrograph has an R4 grating and a 100mm pupil, and separate cross-disperser and camera optics for each of the four
arms, carefully optimized for their respective wavelength ranges. We feed this spectrograph with a miniature lensletbased
IFU that sub-samples the seeing disk of a single object into 7 hexagonal sub-images, reformatting this into a slit
with a second set of double microlenses at the spectrograph entrance with relatively little loss due to focal-ratio
degradation. This reformatting enables high spectral resolution from a compact design that fits well within the relatively
tight GHOST budget. We will describe our baseline 2-object R~50,000 design with full wavelength coverage from the
ultraviolet to the silicon cutoff, as well as the high-resolution single-object R~75,000 mode.
PIMMS IR is a prototype high resolution diraction limited spectrograph operating in the near infrared. Its
current conguration has a bandwidth of 8nm centred on 1550nm with a resolving power, λ/Δλ, of 31000 with the option to increase this to ~60000 using a dual grating system. Remarkably, this is 85% of the theoretical
limit for Gaussian illumination of a diraction grating. It is based upon the PIMMS#0 (photonic integrated
multi-mode micro-spectrograph), a design that utilises the multi-mode to single-mode conversion of the photonic
lantern. By feeding the spectrograph with the single-mode bres we are able to design and build a spectrograph
whose performance is diraction limited and independent of the input source (i.e. a telescope) it is attached to.
The spectrograph has with a throughput of ~70% (that is the light from the single-mode entrance slit that lands
on the detector). The spectrograph is also extremely compact with a footprint of just 450mm x 190mm. Here
we present the design of PIMMS IR and its performance characteristics determined from ray tracing, physical
optics simulations and experimental measurements.Δ
The Sydney University Stellar Interferometer (SUSI) is being fitted with a new beam combiner, called the
Micro-arcsecond University of Sydney Companion Astrometry instrument (MUSCA), for the purpose of high
precision astrometry of bright binary stars. Operating in the visible wavelength regime where photon-counting
and post-processing fringe tracking is possible, MUSCA will be used in tandem with SUSI’s primary beam
combiner, Precision Astronomical Visible Observations (PAVO), to record high spatial resolution fringes and
thereby measure the separation of fringe packets of binary stars. With continued monitoring of stellar separation
vectors at precisions in the tens of micro-arcseconds over timescales of years, it will be possible to search for the
presence of gravitational perturbations in the orbital motion such as those expected from planetary mass objects
in the system. This paper describes the first phase of the development, which includes the setup of the dual beam
combiner system and the methodology applied to stabilize fringes of a star by means of self-phase-referencing.
This paper presents an overview of recent progress at the Sydney University Stellar Interferometer (SUSI). Development
of the third-generation PAVO beam combiner has continued. The MUSCA beam combiner for high-precision
differential astrometry using visible light phase referencing is under active development and will be the subject of a
separate paper. Because SUSI was one of the pioneering interferometric instruments, some of its original systems are old
and have become difficult to maintain. We are undertaking a campaign of modernization of systems: (1) an upgrade of
the Optical Path Length Compensator IR laser metrology counter electronics from a custom system which uses an
obsolete single-board computer to a modern one based on an FPGA interfaced to a Linux computer - in addition to
improving maintainability, this upgrade should allow smoother motion and higher carriage speeds; (2) the replacement of
the aged single-board computer local controllers for the siderostats and the longitudinal dispersion compensator has been
completed; (3) the large beam reducing telescope has been replaced with a pair of smaller units with separate accessible
foci. Examples of scientific results are also included.
High contrast imaging techniques such as aperture masking interferometry allow for the detection of faint companions
such as substellar companions by utilizing light from the planet itself. This allows access to study a larger population of
planetary companions as compared to the transit technique where only systems viewed edge on can be studied, for
example. However, aperture masking has several shortcomings including, low throughputs, limited Fourier coverage,
and leakage of residual atmospheric noise due to phase corrugations across each sub-apertures. These limitations can be
overcome by remapping the pupil with single-mode waveguides. We present an integrated pupil remapping
interferometer, known as Dragonfly, that aims to do just that. We discuss the progress we have made over the past year
in developing a stable and robust instrument and elucidate challenges and the innovative solutions that were applied.
Finally we discuss improvements to the instrument that will enable future scientific endeavors and outline the expected
performance limitations.
KEYWORDS: Waveguides, Interferometers, Telescopes, Spatial filters, Adaptive optics, Signal to noise ratio, Single mode fibers, Interferometry, Space telescopes, Prototyping
Interest in pupil-remapping interferometry, in which a single telescope pupil is fragmented and recombined using
fiber optic technologies, has been growing among a number of groups. As a logical extrapolation from several
highly successful aperture masking programs underway worldwide, pupil remapping offers the advantage of spatial
filtering (with single-mode fibers) and in principle can avoid the penalty of low throughput inherent to an aperture
mask. However in practice, pupil remapping presents a number of difficult technological challenges including
injection into the fibers, pathlength matching of the device, and stability and reproducibility of the results.
Here we present new approaches based on recently-available photonic technologies in which coherent threedimensional
waveguide structures can be sculpted into bulk substrate. These advances allow us to miniaturize
the photonic processing into a single, robust, thermally stable element; ideal for demanding observatory or
spacecraft environments. Ultimately, a wide range of optical functionality could be routinely fabricated into
such structures, including beam combiners and dispersive or wavelength selective elements, bringing us closer to
the vision of an interferometer on a chip.
The Sydney University Stellar Interferometer (SUSI) has been enhanced by installation of the PAVO beam combiner,
which uses an electron-multiplying CCD detector giving a fast, low-noise 2D readout. This allows PAVO to provide
wide-band wavelength dispersed beam combination, which improves sensitivity and scientific productivity. PAVO also
provides pupil segmentation which improves the instrumental fringe visibility. A remote operations facility has been
established, which allows SUSI to be operated from Sydney or elsewhere. A new control system for the longitudinal
dispersion corrector and siderostats is under development. Installation has commenced of a high precision differential
astrometry system (MUSCA) which aims to detect planets in binary star systems.
ERASMUS-F is a pathfinder study for a possible E-ELT 3D-instrumentation, funded by the German Ministry for
Education and Research (BMBF). The study investigates the feasibility to combine a broadband optical spectrograph
with a new generation of multi-object deployable fibre bundles. The baseline approach is to modify the spectrograph of
the Multi-Unit Spectroscopic Explorer (MUSE), which is a VLT integral-field instrument using slicers, with a fibre-fed
input. Taking advantage of recent developments in astrophotonics, it is planed to equip such an instrument with fused
fibre bundles (hexabundles) that offer larger filling factors than dense-packed classical fibres.
The overall project involves an optical and mechanical design study, the specifications of a software package for 3Dspectrophotometry,
based upon the experiences with the P3d Data Reduction Software and an investigation of the
science case for such an instrument. As a proof-of-concept, the study also involves a pathfinder instrument for the VLT,
called the FIREBALL project.
We demonstrate for the first time an imaging fibre bundle ("hexabundle") that is suitable for low-light applications in
astronomy. The most successful survey instruments at optical-infrared wavelengths today have obtained data on up to a
million celestial sources using hundreds of multimode fibres at a time fed to multiple spectrographs. But a large fraction
of these sources are spatially extended on the celestial sphere such that a hexabundle would be able to provide
spectroscopic information at many distinct locations across the source. Our goal is to upgrade single-fibre survey
instruments with multimode hexabundles in place of the multimode fibres. We discuss two varieties of hexabundles: (i)
closely packed circular cores allowing the covering fraction to approach the theoretical maximum of 91%; (ii) fused noncircular
cores where the interstitial holes have been removed and the covering fraction approaches 100%. In both cases,
we find that the cladding can be reduced to ~2μm over the short fuse length, well below the conventional ~10λ thickness
employed more generally. We discuss the relative merits of fused/unfused hexabundles in terms of manufacture and
deployment, and present our first on-sky observations.
We present the first integrated multimode photonic spectrograph, a device we call PIMMS #1. The device comprises
a set of multimode fibres that convert to single-mode propagation using a matching set of photonic lanterns. These
feed to a stack of cyclic array waveguides (AWGs) that illuminate a common detector. Such a device greatly reduces
the size of an astronomical instrument at a fixed spectroscopic resolution. Remarkably, the PIMMS concept is
largely independent of the telescope diameter, input focal ratio and entrance aperture - i.e. one size fits all! The
instrument architecture can also exploit recent advances in astrophotonics (e.g. OH suppression fibres). We present a
movie of the instrument's operation and discuss the advantages and disadvantages of this approach.
The Sydney University Stellar Interferometer (SUSI) has now been operating with a significanly more sensitive beam
combiner system (the Red Table) for several years. A number of novel results from the realms of single, binary and
pulsating star astrophysics are presented. Simultaneous dual beam-combiner operation with the Red Table and an
upgraded Blue Table has been demonstrated, enabling a high spectral dispersion oberving mode for stellar studies. Plans
for a major upgrade are briefly described. One component of this will be remote operation of the array for routine
observational data taking, with first steps on this path reported here with the inception of the Sydney Remote Operations
Center. The backbone of future plans with SUSI center around the installation of the southern of the twin PAVO
instruments. PAVO is also discussed in more detail in Ireland et al, this proceedings.
Dragonfly is designed to overcome the blurring effects of the Earth's atmosphere and achieve high dynamic range
observations of bright objects close to the diffraction limit of a large ground-based telescope. Injection of the sub-pupil
images into single-mode fibres will provide both spatial filtering and reformatting of the redundant pupil array into a
non-redundant output suitable for interferometry. We describe the optical system which includes (i) interface with an
Adaptive Optics system (ii) pupil fragmentation and injection into 36 single-mode fibres (iii) fibre path-length matching
(iv) a beam combiner with spectral dispersion and output to a Low Light Level CCD detector.
The Sydney University Stellar Interferometer is a long baseline optical interferometer located in northern New South Wales, Australia. It has a North-South array of eleven fixed input siderostat stations giving a range of baselines from 5 to 640 m. Currently ten baselines from 5 to 160 m are fully operational and beam-combination and detection systems for the spectral ranges 430-520nm and 550-950nm are available. Dichroic beam-splitters have been introduced to allow simultaneous observations with both spectral systems. The original blue beam-combination system has been upgraded to improve sensitivity and to allow rapid wavelength switching. A software scheduler has been developed to automate much of the observational procedure including the acquisition of a star, fringe search and acquisition, recording of fringe scans, and the taking of photometric scans. A data pipeline for processing the observational data has been further developed to include seeing corrections and this has improved the calibration of the observational data. Preliminary results of scientific observations with both blue and red
systems, including observations of single stars, binary stars and Cepheid variables are described.
The Sydney University Stellar Interferometer (SUSI) is a long-baseline optical interferometer operating at an observatory near Narrabri in Australia. SUSI features a 640 m long North-South array with 11 fixed siderostat stations. New science from the Blue (400-500 nm) and from the recently commissioned Red (500-950 nm) fringe detectors will be presented. Recent technological developments, mainly associated with the new Red detection system, encompassing wavefront correction, fringe encoding, wavelength switching and data analysis strategies, are described.
We present visibility measurements of the nearby Mira-like star R Doradus taken over a wide range of wavelengths (650 - 990 nm). The observations were made using MAPPIT (Masked APerture-Plane Interference Telescope), an interferometer operating at the 3.9-m Anglo-Australian Telescope. We used a slit to mask the telescope aperture and prism to disperse the interference pattern in wavelength. We observed in R Dor strong decreases in visibility within the TiO absorption bands. The results are in general agreement with theory but differ in detail, suggesting that further work is needed to refine the theoretical models.
We are proposing a new spectrograph (ATLAS) which would revolutionize intermediate-dispersion observations at the AAT. Based on the new technology of volume phase holographic gratings, and using transmission optics, ATLAS offers high throughput and a wide field. It will be ideally situated to extensive surveys of faint objects. It has been designed with a collimated beam diameter of 150 mm, giving resolution (lambda) /(delta) (lambda) up to nearly 10,000 with a 1.5 arcsecond slit and good efficiency. It will be a dual-beam instrument, to maximize observing speed and allow optimized optical coatings to be used. The project is working towards its concept design review which will occur during 2000.
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