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MOSAIC is the Multi-Object Spectrograph (MOS) for the 39m Extremely Large Telescope (ELT) of the European Southern Observatory (ESO), with unique capabilities in terms of multiplex, wavelength coverage and spectral resolution. It is a versatile multi-object spectrograph working in both the Visible and NIR domains, designed to cover the largest possible area (∼40 arcmin2) on the focal plane, and optimized to achieve the best possible signal-to-noise ratio on the faintest sources, from stars in our Galaxy to galaxies at the epoch of the reionization. In this paper we describe the main characteristics of the instrument, including its expected performance in the different observing modes. The status of the project will be briefly presented, together with the positioning of the instrument in the landscape of the ELT instrumentation. We also review the main expected scientific contributions of MOSAIC, focusing on the synergies between this instrument and other major ground-based and space facilities.
WST – Widefield Spectroscopic Telescope: We summarise the design challenges of instrumentation for a proposed 12m class Telescope that aims to provide a large (>2.5 square degree) field of view and enable simultaneous Multi-object (> 20,000 objects) and Integral Field spectroscopy (inner 3x3 arcminutes field of view), initially at visible wavelengths. For the MOS mode, instrumentation includes the fiber positioning units, fiber runs and the high (R~40,000) and low (R~3,000 - 4,000) resolution spectrographs. For the MUSE like Integral Field Spectrograph, this includes the relay from the Telescope Focal Plane, the multi-stage splitting and slicing and almost 150 identical spectrographs. We highlight the challenge of mass production at a credible cost and the issues of maintenance and sustainable operation.
BlueMUSE is a blue-optimised, medium spectral resolution, panoramic integral eld spectrograph under development for the Very Large Telescope (VLT). With an optimised transmission down to 350 nm, spectral resolution of R~3500 on average across the wavelength range, and a large FoV (1 arcmin2), BlueMUSE will open up a new range of galactic and extragalactic science cases facilitated by its specific capabilities. The BlueMUSE consortium includes 9 institutes located in 7 countries and is led by the Centre de Recherche Astrophysique de Lyon (CRAL). The BlueMUSE project development is currently in Phase A, with an expected rst light at the VLT in 2031. We introduce here the Top Level Requirements (TLRs) derived from the main science cases, and then present an overview of the BlueMUSE system and its subsystems ful lling these TLRs. We speci cally emphasize the tradeo s that are made and the key distinctions compared to the MUSE instrument, upon which the system architecture is built.
The Visible Integral Field Replicable Unit Spectrograph (VIRUS), the instrument for the Hobby Eberly Telescope Dark Energy Experiment (HETDEX), consists of 78 replicated units, each with two integral field spectrograph channels. VIRUS reached the full complement of spectrographs in 2021 and has been undertaking the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX). The VIRUS design takes advantage of large-scale replication of simple units to significantly reduce engineering and production costs of building a facility instrument of this scale. With VIRUS being 156 realizations of the same spectrograph, this paper uncovers the statistical variations in performance of these units along with effective strategies for specifying large batches of components. Results of delivered spectrograph component performance compared to statistical batch specifications are presented. Based on variations in performance of individual spectrograph components, throughput curves are simulated for 156 VIRUS spectrograph channels. Once delivered, each unit is paired with a fiber bundle and throughput measurements are made on sky using twilight flats. We compare throughput variance from on-sky measurements of 140 channels to the simulated throughputs. We find that the variation in throughput matches that predicted by modeling of the combined individual component performance. The average overall throughput of VIRUS measured on-sky and the variability in unit performance meets specification for the HETDEX survey, which is now complete. This paper presents VIRUS as a proof of concept that massively replicated instruments provide a viable solution to scaling up instruments for the next generation of large surveys and telescopes.
4MOST is a versatile spectroscopic facility soon to be installed on the ESO VISTA Telescope at Paranal. Prior to shipment to Chile, our team is conducting a comprehensive characterization of the instrument in a controlled laboratory setting. This preparatory phase is crucial for ensuring the fulfilment of both technical specifications and some key user requirements. The goal of this verification campaign is to obtain characterization data which will benchmark the performance of the spectrographs and the calibration unit against established metrics. The data primarily tests the spectral performance of the three spectrographs, the stability of the system, including the calibration unit, as well as the fiber throughput, which are pivotal for the success of 4MOST’s ambitious science goals. Additionally, the verification contains a selection of user requirements, ensuring the instrument’s readiness for the diverse scientific objectives it aims to enable. The results from these tests inform the observational strategy for future normal science operations. In this paper we outline the undertaken preparatory work, the applied testing procedures, and the anticipated implications of these tests, and their results, in the context of the final verification at the telescope, commissioning and normal science operations. This initial test phase marks a critical juncture in the 4MOST project timeline, setting the stage for a successful commissioning.
BlueMUSE is an integral field spectrograph in an early development stage for the ESO VLT. For our design of the data reduction software for this instrument, we are first reviewing capabilities and issues of the pipeline of the existing MUSE instrument. MUSE has been in operation at the VLT since 2014 and led to discoveries published in more than 600 refereed scientific papers. While BlueMUSE and MUSE have many common properties we briefly point out a few key differences between both instruments. We outline a first version of the flowchart for the science reduction, and discuss the necessary changes due to the blue wavelength range covered by BlueMUSE. We also detail specific new features, for example, how the pipeline and subsequent analysis will benefit from improved handling of the data covariance, and a more integrated approach to the line-spread function, as well as improvements regarding the wavelength calibration which is of extra importance in the blue optical range. We finally discuss how simulations of BlueMUSE datacubes are being implemented and how they will be used to prepare the science of the instrument.
4MOST (4-meter Multi-Object Spectroscopic Telescope) is a wide-field, fiber-fed, high-multiplex spectroscopic survey facility to be installed on the 4-meter ESO telescope VISTA in Chile. The back-end consists of one high-resolution spectrograph (HRS) and two identical low-resolution spectrographs. 4MOST will afford with the HRS simultaneous observations of up to 812 targets on a hexagonal 4.4 square degrees field of view at a spectral resolution R<18,000 covering 392.6 to 679 nm in three channels. It is expected to be fully operational early 2024. In this paper, we present the integration and alignment applied for the HRS optics. The results of the tests of the fully integrated sub-system in our integration facility are discussed. The instrument schedule is outlined and the actual timeline of the previous procurement and manufacturing phase is given
BlueMUSE is a novel instrument under development for the ESO VLT, that builds on the legacy of MUSE, however with a blue wavelength range, a larger field-of-view (FoV), and higher spectral resolution. Driven by high-profile and unique science cases, the requirements present new challenges to the development of the instrument, although the fundamental layout will be based on the successful modular structure of the classical MUSE. In order to achieve the expected mean spectral resolution of R=3600 and radial velocity measurement accuracy of better than 1 km/s, as well as spectrophotometric performance, BlueMUSE must be equipped with a calibration unit to perform accurate wavelength, flat-field, and geometrical calibration. Lessons learned from MUSE show that the variation of the line-spread-function (LSF) across the FoV as a consequence of the field-splitter and image slicer layout requires a methodology to accurately measure the LSF as a function of x and y. Moreover, classical spectral line lamps that have been used traditionally for wavelength calibration present the problem of a scarce emission line coverage in the blue. BlueMUSE has entered pre-Phase-A in 2022. We report first results from conceptual design studies to address these challenges, in particular concepts of Fabry-Perot based tunable frequency combs, and as an alternative approach novel concepts with laser frequency combs or micro-ring resonator based combs in the blue.
The 4MOST instrument is a multi-object spectroscopic survey facility for the VISTA telescope at Paranal. The large multiplex gain for 4MOST is achieved by connecting over 2400 optical fibers from the telescope focal plane to three spectrographs. The final system features 812 fibers per spectrograph of around 25m in cable length. In addition, there are dedicated fiber cables for simultaneous calibration, for secondary guiding, and fiducial reference fibers for metrology. The fiber cable specifications, manufacture, assembly, and acceptance tests are described. Sub-system testing includes sparsely-populated fiber-slit-units, used for spectrograph alignment and performance verification and the fiber cable routing through the Cassegrain cable wrap.
MOSAIC is the Multi-Object Spectrograph for the ESO Extremely Large Telescope, approved to enter Phase B beginning 2022. It is conceived as a multi- purpose instrument covering the Visible and Near Infrared bandwidth (0.45 –1.8 μm) with two observing modes: spatially resolved spectroscopy with 8 integral field units; and the simultaneous observation of 200 objects in the VIS and NIR in unresolved spectroscopy.
We present an overview of the main MOSAIC science drivers and the actual baseline design for the instrument. The prototyping and developments undertaken by the consortium to evaluate the feasibility of the project are also discussed.
The 4-meter Multi-Object Spectroscopic Telescope (4MOST), wide-field, high-multiplex spectroscopic survey facility will enable the simultaneous spectroscopy of up to 2400 targets within a 2.5° diameter field of view. A secondary guider system optical relay and data production description is described. The role of this guider is for fine rotational and target alignment corrections. The output of the 12 times 7 fibres are arranged such that the CCD detector can be read out in continuous read mode. The position of all fibres are illuminated at their spectrograph end and measured using a camera system at the positioner end. For the secondary guide bundles, only the central fibre is illuminated. A notch filter is used in the image relay in such a way that that the back illumination light is reflected from back illumination fibres to illuminate only the central fibres of each guide probe. This allows on-sky guiding while the fibres are being positioned.
A status overview of 4MOST is presented, a new high-multiplex, wide-field spectroscopic survey facility under construction for ESO's VISTA telescope at Paranal. Its key specifications are: a large field of view of 4.4 deg2 and a high multiplex capability, with 1624 fibres feeding two low-resolution spectrographs (R = λ/Δλ ~ 6500), and 812 fibres transferring light to the high-resolution spectrograph (R ~ 20 000). The 4MOST system integration has commenced and the selection process for ESO community survey programmes has been started. This overview presents the expected performance of the instrument, the science the consortium expects to carry out, and the unique operational scheme of 4MOST.
Following a successful Phase A study, we introduce the delivered conceptual design of the MOSAIC1 multi-object spectrograph for the ESO Extremely Large Telescope (ELT). MOSAIC will provide R~5000 spectroscopy over the full 460-1800 nm range, with three additional high-resolution bands (R~15000) targeting features of particular interest. MOSAIC will combine three operational modes, enabling integrated-light observations of up to 200 sources on the sky (high-multiplex mode) or spectroscopy of 10 spatially-extended fields via deployable integral-field units: MOAO6 assisted high-definition (HDM) and Visible IFUs (VIFU). We will summarise key features of the sub-systems of the design, e.g. the smart tiled focal-plane for target selection and the multi-object adaptive optics used to correct for atmospheric turbulence, and present the next steps toward the construction phase.
MOSAIC is a concept for a multi-object spectrograph for the Extremely Large Telescope (ELT). It is planned to cover the wavelength range from 460 nm to 1800 nm with 5 visible spectrographs and 5 near-infrared spectrographs. The ELT is far from diffraction limited in the visible wavelength range. Rather than developing a large and complex AO system, it was decided that the instrument will be seeing limited in the visible. Spot sizes are therefore about 2.8 mm in diameter in the ELT focal plane, and need to be sampled by multiple fibers with large core diameter. As a result, large optics is required to achieve the science requirements on spectral resolution, bandwidth and multiplex. We work in close collaboration with manufacturers to design an instrument that is feasible and meets the scientific requirements.
Fibre fed spectroscopy requires that the output distribution of the optical fibre is as stable as possible. Effects like scrambling and FRD play an important role in any fibre fed instrument design, since they affect directly the output distribution of multi-mode fibres. These effects depend, among other factors, on the excited propagation modes. The propagation modes of different fibre geometries have different spatial distributions, therefore could show different scrambling and FRD characteristics. A model is being developed at the Leibniz-Institute for Astrophysics Potsdam (AIP) that shows the intrinsic effect of scrambling and FRD in optical fibres. The model is based on the Eigenmode Expansion Method (EEM). With this theoretical frame work should be possible to compare the results of mode excitation in different fibre geometries. This work is part of a PhD Thesis involved in the fibre system of MOSAIC, a multi-object spectrograph for the E-ELT.
The 4MOST1 instrument is a multi-object-spectrograph for the ESO-VISTA telescope. The 4MOST long fiber feed links the AESOP2 fiber positioner to two low-resolution spectrographs (1624 fibers) and one high-resolution spectrograph (812 fibers). In addition to the 2436 science fibers, the system includes guide fiber bundles, metrology fiducial fibers and simultaneous calibration fibers for the spectrographs. To validate the design approaches, including fiber connectors and cable rotator, pre-production fiber cables have been built and evaluated. This paper presents the near final design of the fiber feed subsystem and its performance results pertaining to throughput homogeneity, focal ratio degradation, and connector loss of the pre-production cables.
Product Assurance is an essential activity to support the design and construction of complex instruments developed for major scientific programs. The international size of current consortia in astrophysics, the ambitious and challenging developments, make the product assurance issues very important. The objective of this paper is to focus in particular on the application of Product Assurance Activities to a project such as MOSAIC, within an international consortium. The paper will also give a general overview on main product assurance tasks to be implemented during the development from the design study to the validation of the manufacturing, assembly, integration and test (MAIT) process and the delivery of the instrument.
4MOST is a fibre-fed, multi-object spectroscopic survey facility to be installed on the VISTA telescope at ESO's Paranal observatory. This paper presents the final mechanical design of the optical fibre route from the fibre positioner at the focal plane of VISTA to the fibre-slits within the high- and low-resolution spectrographs below the azimuth platform. The technical challenges are to provide a safe, durable and efficient fibre route for over 2400 fibres. To accommodate the movements of the telescope, a Cassegrain Cable Wrap and a novel elevation chain concept has been prototyped and extensively tested to validate the design solutions.
The Hobby-Eberly Telescope Wide Field Upgrade includes deployment of the fiber-fed VIRUS and LRS2 spectrographs. In total, over 35,000 optical fibers of around 20m lengths are coupled to the telescope. This paper discusses the routing of those fibers, the hardware for securing them, and their deployment. Routing of the fibers to accommodate telescope motion while minimizing length and bend is presented. Hardware solutions for securing the fibers with details of the input and output terminations are included. Operations to safely install the fibers on the telescope are also covered.
The Visible Integral Field Replicable Unit Spectrograph (VIRUS), the instrument for the Hobby Eberly Telescope Dark Energy Experiment (HETDEX), consists of 78 replicable units, each with two integral field spectrographs. The VIRUS design takes advantage of large-scale replication of simple units to significantly reduce engineering and production costs of building a facility instrument of this scale. With VIRUS being 156 realizations of the same spectrograph, this paper uncovers the statistical variations in production of these units. Lab relative throughput measures are compared with independently measured grating and optical element performance allowing for potential diagnosis for the cause of variation due to spectrograph elements. Based on variations in performance of individual optical components, throughput curves are simulated for 156 VIRUS spectrograph channels. Once delivered, each unit is paired with a fiber bundle and throughput measurements are made on sky using twilight flats. We compare throughput variance from on-sky measurements to the simulated throughputs. We find that the variation in throughput matches that predicted by modeling of the individual optics performance. This paper presents the results for the 40 VIRUS units now deployed.
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 Visible Integral-field Replicable Unit Spectrograph (VIRUS) consists of 156 identical spectrographs (arrayed as 78 pairs, each with a pair of spectrographs) fed by 35,000 fibers, each 1.5 arcsec diameter, at the focus of the upgraded 10 m Hobby-Eberly Telescope (HET). VIRUS has a fixed bandpass of 350-550 nm and resolving power R~750. The fibers are grouped into 78 integral field units, each with 448 fibers and 20 m average length. VIRUS is the first example of large-scale replication applied to optical astronomy and is capable of surveying large areas of sky, spectrally. The VIRUS concept offers significant savings of engineering effort and cost when compared to traditional instruments. The main motivator for VIRUS is to map the evolution of dark energy for the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX), using 0.8M Lyman-alpha emitting galaxies as tracers. The VIRUS array has been undergoing staged deployment starting in late 2015. Currently, more than half of the array has been populated and the HETDEX survey started in 2017 December. It will provide a powerful new facility instrument for the HET, well suited to the survey niche of the telescope, and will open up large spectroscopic surveys of the emission line universe for the first time. We will review the current state of production, lessons learned in sustaining volume production, characterization, deployment, and commissioning of this massive instrument.
The Visible Integral-field Replicable Unit Spectrograph (VIRUS) consists of 156 identical spectrographs (arrayed as 78 pairs) fed by 35,000 fibers, each 1.5 arcsec diameter, at the focus of the upgraded 10 m Hobby-Eberly Telescope (HET). VIRUS has a fixed bandpass of 350-550 nm and resolving power R~700. VIRUS is the first example of industrial-scale replication applied to optical astronomy and is capable of surveying large areas of sky, spectrally. The VIRUS concept offers significant savings of engineering effort, cost, and schedule when compared to traditional instruments. The main motivator for VIRUS is to map the evolution of dark energy for the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX‡), using 0.8M Lyman-alpha emitting galaxies as tracers. The VIRUS array is undergoing staged deployment during 2016 and 2017. It will provide a powerful new facility instrument for the HET, well suited to the survey niche of the telescope, and will open up large spectroscopic surveys of the emission line universe for the first time. We will review the production, lessons learned in reaching volume production, characterization, and first deployment of this massive instrument.
The 4MOST instrument is a multi-object-spectrograph for the ESO-VISTA telescope. The 4MOST fiber feed subsystem is composed of a fiber positioner (AESOP) holding 2436 science fibers based on the Echidna tilting spine concept, and the fiber cable, which feeds two low-resolution spectrographs (1624 fibers) and one high-resolution spectrograph (812 fibers). In order to optimize the fiber feed subsystem design and provide essential information required for the spectrograph design, prototyping and testing has been undertaken. In this paper we give an overview of the current fiber feed subsystem design and present the preliminary FRD, scrambling, throughput and system performance impact results for: maximum and minimum spine tilt, fiber connectors, cable de-rotator simulator for fiber cable lifetime tests.
The accurate characterization of the field at the output of the optical fibres is of relevance for precision spectroscopy in astronomy. The modal effects of the fibre translate to the illumination of the pupil in the spectrograph and impact on the resulting point spread function (PSF). A Model is presented that is based on the Eigenmode Expansion Method (EEM) that calculates the output field from a given fibre for different manipulations of the input field. The fibre design and modes calculation are done via the commercially available Rsoft-FemSIM software. We developed a Python script to apply the EEM. Results are shown for different configuration parameters, such as spatial and angular displacements of the input field, spot size and propagation length variations, different transverse fibre geometries and different wavelengths. This work is part of the phase A study of the fibre system for MOSAIC, a proposed multi-object spectrograph for the European Extremely Large Telescope (ELT-MOS).
VIRUS is a massively replicated spectrograph built for HETDEX, the Hobby Eberly Telescope Dark Energy Experiment. It consists of 156 channels within 78 units fed by 34944 fibers over the 22 arcminute field of the upgraded HET. VIRUS covers a relatively narrow bandpass (350-550nm) at low resolution (R ~ 700) to target the emission of Lyman-alpha emitters (LAEs) for HETDEX. VIRUS is a first demonstration of industrial style assembly line replication in optical astronomy. Installation and testing of VIRUS units began in November of 2015. This winter we celebrated the first on sky instrument activity of the upgraded HET, using a VIRUS unit and LRS2-R (the upgraded facility Low Resolution Spectrograph for the HET). Here we describe progress in VIRUS installation and commissioning through June 2016. We include early sky data obtained to characterize spectrograph performance and on sky performance of the newly upgraded HET. As part of the instrumentation for first science light at the HET, the IFU fed spectrographs were used to test a full range of telescope system functionality including the field calibration unit (FCU).We also use placement of strategic IFUs to map the new HET field to the fiber placement, and demonstrate actuation of the dithering mechanism key to HETDEX observations.
After having demonstrated that an IFU, attached to a microscope rather than to a telescope, is capable of differentiating complex organic tissue with spatially resolved Raman spectroscopy, we have launched a clinical validation program that utilizes a novel optimized fiber-coupled multi-channel spectrograph whose layout is based on the modular MUSE spectrograph concept. The new design features a telecentric input and has an extended blue performance, but otherwise maintains the properties of high throughput and excellent image quality over an octave of wavelength coverage with modest spectral resolution. We present the opto-mechanical layout and details of its optical performance.
MUSE (Multi Unit Spectroscopic Explorer) is a second generation instrument built for ESO (European Southern
Observatory). The MUSE project is supported by a European consortium of 7 institutes.
After the finalisation of its integration in Europe, the MUSE instrument has been partially dismounted and shipped to
the VLT (Very Large Telescope) in Chile. From October 2013 till February 2014, it has then been reassembled, tested
and finally installed on the telescope its final home. From there it collects its first photons coming from the outer limit
of the visible universe.
This critical moment when the instrument finally meets its destiny is the opportunity to look at the overall outcome of
the project and the final performance of the instrument on the sky. The instrument which we dreamt of has become
reality. Are the dreamt performances there as well?
These final instrumental performances are the result of a step by step process of design, manufacturing, assembly, test
and integration. Now is also time to review the path opened by the MUSE project. What challenges were faced during
those last steps, what strategy, what choices did pay off? What did not?
4MOST, the 4m Multi-Object Spectroscopic Telescope, features a 2.5 degree diameter field-of-view with ~2400 fibers in
the focal plane that are configured by a fiber positioner based on the tilting spine principle (Echidna/FMOS) arranged in
a hexagonal pattern. The fibers feed two types of spectrographs; ~1600 fibers go to two spectrographs with resolution
R>5000 and ~800 fibers to a spectrograph with R>18,000. Part of the ongoing optimization of the fiber feed subsystem
design includes early prototyping and testing of key components such as fiber connectors and fiber cable management.
Performance data from this testing will be used in the 4MOST instrument simulator (TOAD) and 4MOST system design
optimization. In this paper we give an overview of the current fiber feed subsystem design, simulations and prototyping
plans.
The use of deployable fibre-bundles plays an increasing role in the design of future Multi-Object-Spectrographs (MOS).
Within a research and development project for "Enabling Technologies for the E-ELT", various miniaturized, fibrebundles
were designed, built and tested for their suitability for a proposed ELT-MOS instrument.
The paper describes the opto-mechanical designs of the bundles and the different manufacture approaches, using glued,
stacked and fused optical fibre bundles. The fibre bundles are characterized for performance, using dedicated testbenches
in the laboratory and at a telescope simulator. Their performance is measured with respect to geometric
accuracy, throughput, FRD behavior and cross-talk between channels.
We here report on recent progress on astronomical optical frequency comb generation at innoFSPEC-Potsdam and
present preliminary test results using the fiber-fed Multi Unit Spectroscopic Explorer (MUSE) spectrograph. The
frequency comb is generated by propagating two free-running lasers at 1554.3 and 1558.9 nm through two dispersionoptimized
nonlinear fibers. The generated comb is centered at 1590 nm and comprises more than one hundred lines with
an optical-signal-to-noise ratio larger than 30 dB. A nonlinear crystal is used to frequency double the whole comb
spectrum, which is efficiently converted into the 800 nm spectral band. We evaluate first the wavelength stability using
an optical spectrum analyzer with 0.02 nm resolution and wavelength grid of 0.01 nm. After confirming the stability
within 0.01 nm, we compare the spectra of the astro-comb and the Ne and Hg calibration lamps: the astro-comb exhibits
a much larger number of lines than lamp calibration sources. A series of preliminary tests using a fiber-fed MUSE
spectrograph are subsequently carried out with the main goal of assessing the equidistancy of the comb lines. Using a
P3d data reduction software we determine the centroid and the width of each comb line (for each of the 400 fibers
feeding the spectrograph): equidistancy is confirmed with an absolute accuracy of 0.4 pm.
4MOST is a wide-field, high-multiplex spectroscopic survey facility under development for the VISTA telescope of the European Southern Observatory (ESO). Its main science drivers are in the fields of galactic archeology, high-energy physics, galaxy evolution and cosmology. 4MOST will in particular provide the spectroscopic complements to the large
area surveys coming from space missions like Gaia, eROSITA, Euclid, and PLATO and from ground-based facilities like VISTA, VST, DES, LSST and SKA. The 4MOST baseline concept features a 2.5 degree diameter field-of-view with ~2400 fibres in the focal surface that are configured by a fibre positioner based on the tilting spine principle. The fibres feed two types of spectrographs; ~1600 fibres go to two spectrographs with resolution R<5000 (λ~390-930 nm) and
~800 fibres to a spectrograph with R>18,000 (λ~392-437 nm and 515-572 nm and 605-675 nm). Both types of spectrographs are fixed-configuration, three-channel spectrographs. 4MOST will have an unique operations concept in which 5 year public surveys from both the consortium and the ESO community will be combined and observed in parallel during each exposure, resulting in more than 25 million spectra of targets spread over a large fraction of the
southern sky. The 4MOST Facility Simulator (4FS) was developed to demonstrate the feasibility of this observing
concept. 4MOST has been accepted for implementation by ESO with operations expected to start by the end of 2020.
This paper provides a top-level overview of the 4MOST facility, while other papers in these proceedings provide more
detailed descriptions of the instrument concept[1], the instrument requirements development[2], the systems engineering implementation[3], the instrument model[4], the fibre positioner concepts[5], the fibre feed[6], and the spectrographs[7].
VIRUS is the massively replicated fiber-fed spectrograph being built for the Hobby-Eberly Telescope to support
HETDEX (the Hobby-Eberly Telescope Dark Energy Experiment). The instrument consists of 156 identical
channels, fed by 34,944 fibers contained in 78 integral field units, deployed in the 22 arcminute field of the
upgraded HET. VIRUS covers 350-550nm at R ≈ 700 and is built to target Lyman α emitters at 1.9 < z < 3.5 to
measure the evolution of dark energy. Here we present the assembly line construction of the VIRUS spectrographs,
including their alignment and plans for characterization. We briefly discuss plans for installation on the telescope.
The spectrographs are being installed on the HET in several stages, and the instrument is due for completion
by the end of 2014.
MUSE (Multi Unit Spectroscopic Explorer) is a second generation instrument, built for ESO (European Southern
Observatory) and dedicated to the VLT (Very Large Telescope). This instrument is an innovative integral field
spectrograph (1x1 arcmin2 Field of View), operating in the visible wavelength range, from 465 nm to 930 nm. The
MUSE project is supported by a European consortium of 7 institutes.
After the finalisation of its integration and test in Europe validated by its Preliminary Acceptance in Europe, the MUSE
instrument has been partially dismounted and shipped to the VLT (Very Large Telescope) in Chile. From October 2013
till February 2014, it has then been reassembled, tested and finally installed on the telescope its final home. From there
it will collect its first photons coming from the outer limit of the visible universe.
To come to this achievement, many tasks had to be completed and challenges overcome. These last steps in the project
life have certainly been ones of the most critical. Critical in terms of risk, of working conditions, of operational
constrains, of schedule and finally critical in terms of outcome: The first light and the final performances of the
instrument on the sky.
VIRUS is the visible, integral-field replicable unit spectrograph for the Hobby-Eberly-Telescope (HET) consisting of 75
integral-field-units that feed 150 spectrographs. The full VIRUS instrument features over 33,000 fibres, each projecting
to 1.5 arcseconds diameter on sky, deployed at the prime focus of the upgraded 10m HET. The assembly and acceptance
testing for all IFUs includes microscopic surface quality inspections, astrometry of fibre positions, relative throughput
measurements, focal-ratio-degradation evaluation, and system acceptance using a VIRUS reference spectrograph to
verify the image quality, spectral transmission, stability, or to detect any stray light issues.
The Visible Integral-field Replicable Unit Spectrograph (VIRUS) consists of a baseline build of 150 identical
spectrographs (arrayed as 75 unit pairs) fed by 33,600 fibers, each 1.5 arcsec diameter, at the focus of the upgraded 10
m Hobby-Eberly Telescope (HET). VIRUS has a fixed bandpass of 350-550 nm and resolving power R~700. VIRUS is
the first example of industrial-scale replication applied to optical astronomy and is capable of surveying large areas of
sky, spectrally. The VIRUS concept offers significant savings of engineering effort, cost, and schedule when compared
to traditional instruments.
The main motivator for VIRUS is to map the evolution of dark energy for the Hobby-Eberly Telescope Dark Energy
Experiment (HETDEX), using 0.8M Lyman-α emitting galaxies as tracers. The full VIRUS array is due to be deployed starting at the end of 2014 and will provide a powerful new facility instrument for the HET, well suited to the
survey niche of the telescope, and will open up large area surveys of the emission line universe for the first time.
VIRUS is in full production, and we are about half way through. We review the production design, lessons learned in
reaching volume production, and preparation for deployment of this massive instrument. We also discuss the application
of the replicated spectrograph concept to next generation instrumentation on ELTs.
The 4MOST consortium is currently halfway through a Conceptual Design study for ESO with the aim to develop a wide-field ( < 3 square degree, goal < 5 square degree), high-multiplex ( < 1500 fibres, goal 3000 fibres) spectroscopic survey facility for an ESO 4m-class telescope (VISTA). 4MOST will run permanently on the telescope to perform a 5 year public survey yielding more than 20 million spectra at resolution R∼5000 (λ=390–1000 nm) and more than 2 million spectra at R~20,000 (395–456.5 nm and 587–673 nm). The 4MOST design is especially intended to complement three key all-sky, space-based observatories of prime European interest: Gaia, eROSITA and Euclid. Initial design and performance estimates for the wide-field corrector concepts are presented. Two fibre positioner concepts are being considered for 4MOST. The first one is a Phi-Theta system similar to ones used on existing and planned facilities. The second one is a new R-Theta concept with large patrol area. Both positioner concepts effectively address the issues of fibre focus and pupil pointing. The 4MOST spectrographs are fixed configuration two-arm spectrographs, with dedicated spectrographs for the high- and low-resolution fibres. A full facility simulator is being developed to guide trade-off decisions regarding the optimal field-of-view, number of fibres needed, and the relative fraction of high-to-low resolution fibres. The simulator takes mock catalogues with template spectra from Design Reference Surveys as starting point, calculates the output spectra based on a throughput simulator, assigns targets to fibres based on the capabilities of the fibre positioner designs, and calculates the required survey time by tiling the fields on the sky. The 4MOST consortium aims to deliver the full 4MOST facility by the end of 2018 and start delivering high-level data products for both consortium and ESO community targets a year later with yearly increments.
MUSE (Multi Unit Spectroscopic Explorer) is a second generation instrument built for ESO (European Southern
Observatory) to be installed in Chile on the VLT (Very Large Telescope). The MUSE project is supported by a
European consortium of 7 institutes.
After the critical turning point of shifting from the design to the manufacturing phase, the MUSE project has now
completed the realization of its different sub-systems and should finalize its global integration and test in Europe.
To arrive to this point many challenges had to be overcome, many technical difficulties, non compliances or
procurements delays which seemed at the time overwhelming. Now is the time to face the results of our organization, of
our strategy, of our choices. Now is the time to face the reality of the MUSE instrument.
During the design phase a plan was provided by the project management in order to achieve the realization of the
MUSE instrument in specification, time and cost. This critical moment in the project life when the instrument takes
shape and reality is the opportunity to look not only at the outcome but also to see how well we followed the original
plan, what had to be changed or adapted and what should have been.
MUSE (Multi Unit Spectroscopic Explorer) is a second generation VLT integral field spectrograph (1x1arcmin² Field of View) developed for the European Southern Observatory (ESO), operating in the visible wavelength range (0.465-0.93 μm). A consortium of seven institutes is currently assembling and testing MUSE in the Integration Hall of the
Observatoire de Lyon for the Preliminary Acceptance in Europe, scheduled for 2013.
MUSE is composed of several subsystems which are under the responsibility of each institute. The Fore Optics derotates
and anamorphoses the image at the focal plane. A Splitting and Relay Optics feed the 24 identical Integral Field Units
(IFU), that are mounted within a large monolithic instrument mechanical structure. Each IFU incorporates an image
slicer, a fully refractive spectrograph with VPH-grating and a detector system connected to a global vacuum and
cryogenic system. During 2011, all MUSE subsystems were integrated, aligned and tested independently in each
institute. After validations, the systems were shipped to the P.I. institute at Lyon and were assembled in the Integration
Hall
This paper describes the end-to-end optical alignment procedure of the MUSE instrument. The design strategy, mixing
an optical alignment by manufacturing (plug and play approach) and few adjustments on key components, is presented.
We depict the alignment method for identifying the optical axis using several references located in pupil and image
planes. All tools required to perform the global alignment between each subsystem are described. The success of this
alignment approach is demonstrated by the good results for the MUSE image quality.
MUSE commissioning at the VLT (Very Large Telescope) is planned for 2013.
The Multi-Unit Spectroscopic Explorer (MUSE), an integral-field spectrograph for the ESO Very Large Telescope, has
been built and integrated by a consortium of 7 European institutes. MUSE can simultaneously record spectra across a
field of view of 1 square arcminute in the wavelength range from 465nm to 930nm. The calibration unit (CU) for MUSE
was developed to provide accurate flat fielding, spectral, geometrical, image quality and efficiency calibration for both
the wide-field and AO-assisted narrow-field modes. This paper describes the performance of the CU and electronics,
from the subsystem validation to the integration, alignment and use in the MUSE instrument.
The Visible Integral-field Replicable Unit Spectrograph (VIRUS) consists of a baseline build of 150 identical
spectrographs (arrayed as 75 units, each with a pair of spectrographs) fed by 33,600 fibers, each 1.5 arcsec diameter,
deployed over the 22 arcminute field of the upgraded 10 m Hobby-Eberly Telescope (HET). The goal is to deploy 82
units. VIRUS has a fixed bandpass of 350-550 nm and resolving power R~700. VIRUS is the first example of
industrial-scale replication applied to optical astronomy and is capable of spectral surveys of large areas of sky. This
approach, in which a relatively simple, inexpensive, unit spectrograph is copied in large numbers, offers significant
savings of engineering effort, cost, and schedule when compared to traditional instruments.
The main motivator for VIRUS is to map the evolution of dark energy for the Hobby-Eberly Telescope Dark Energy
Experiment (HETDEX) using 0.8M Lyman-α emitting galaxies as tracers. The full VIRUS array is due to be deployed
by early 2014 and will provide a powerful new facility instrument for the HET, well suited to the survey niche of the
telescope. VIRUS and HET will open up wide-field surveys of the emission-line universe for the first time. We present
the production design and current status of VIRUS.
We report on extensive testing carried out on the optical fibers for the VIRUS instrument. The primary result of
this work explores how 10+ years of simulated wear on a VIRUS fiber bundle affects both transmission and focal
ratio degradation (FRD) of the optical fibers. During the accelerated lifetime tests we continuously monitored
the fibers for signs of FRD. We find that transient FRD events were common during the portions of the tests
when motion was at telescope slew rates, but dropped to negligible levels during rates of motion typical for
science observation. Tests of fiber transmission and FRD conducted both before and after the lifetime tests
reveal that while transmission values do not change over the 10+ years of simulated wear, a clear increase in
FRD is seen in all 18 fibers tested. This increase in FRD is likely due to microfractures that develop over time
from repeated flexure of the fiber bundle, and stands in contrast to the transient FRD events that stem from
localized stress and subsequent modal diffusion of light within the fibers. There was no measurable wavelength
dependence on the increase in FRD over 350 nm to 600 nm. We also report on bend radius tests conducted
on individual fibers and find the 266 μm VIRUS fibers to be immune to bending-induced FRD at bend radii
of R 10 cm. Below this bend radius FRD increases slightly with decreasing radius. Lastly, we give details
of a degradation seen in the fiber bundle currently deployed on the Mitchell Spectrograph (formally VIRUS-P)
at McDonald Observatory. The degradation is shown to be caused by a localized shear in a select number of
optical fibers that leads to an explosive form of FRD. In a few fibers, the overall transmission loss through the
instrument can exceed 80%. These results are important for the VIRUS instrument, and for both current and
proposed instruments that make use of optical fibers, particularly when the fibers are in continual motion during
an observation, or experience repeated mechanical stress during their deployment.≥
MUSE (Multi Unit Spectroscopic Explorer) is a second generation instrument developed for ESO (European Southern
Observatory) and will be assembled to the VLT (Very Large Telescope) in 2013. The MUSE instrument can
simultaneously record 90.000 spectra in the visible wavelength range (465-930nm), across a 1*1arcmin² field of view,
thanks to 24 identical Integral Field Units (IFU). A collaboration of 7 institutes has partly validated and sent their subsystems
to CRAL (Centre de Recherche Astrophysique de Lyon) in 2011, where they have been assembled together.
The global test and validation process is currently going on to reach the Preliminary Acceptance in Europe in 2012. The
sharing of performances has been based on 5 main functional sub-systems. The Fore Optics sub-system derotates and
anamorphoses the VLT Nasmyth focal plane image, the Splitting and Relay Optics associated with the Main Structure
are feeding each IFU with 1/24th of the field of view. Each IFU is composed of a 3D function insured by an image slicer
system and a spectrograph, and a detection function by a 4k*4k CCD cooled down to 163°K. The 5th function is the
calibration and data reduction of the instrument. This article depicts the sequence of tests that has been completely
reshafled mainly due to planning constraints. It highlights the priority given to the most critical performances tests of the
sub-systems and their results. It enhances then the importance given to global tests. Finally, it makes a status on the
verification matrix and the validation of the instrument and gives a critical view on the risks taken.
The 24 IFU from MUSE are equipped with 4K x 4K CCD detectors which are operated at cryogenic temperature around
160 K. The large size of the chip combined with a rather fast camera (F/2) impose strong positioning constrains. The
sensitive surface should remain in an angular envelope of less than 30 arc sec in both directions. The ambitious goal of
having the same spectrum format on every detector imposes also a very accurate positioning in the image plane. The
central pixel has to be located in a square smaller 50 microns relative to the external references.
The first part of the paper describes the mechanical design of the detector head. We concentrate on the various aspects of
the design with its very complex interfaces. The opto-mechanical concept is presented with an emphasis on the
robustness and reliability. We present also the necessary steps for the extreme optimization of the cryogenic performance
of this compact design driven with a permanent view of the production in series.
The techniques and procedures developed in order to meet and verify the very tight positioning requirements are
described in a second part. Then the 24 fully assembled systems undergo a system verification using one of the MUSE
spectrographs. These tests include a focus series, the determination of the PSF across the chip and a subsequent
calculation of the tip/tilt and shift rotation of the detector versus the optical axis.
Martin Roth, Karl Zenichowski, Nicolae Tarcea, Jürgen Popp, Silvia Adelhelm, Marvin Stolz, Andreas Kelz, Christer Sandin, Svend-Marian Bauer, Thomas Fechner, Thomas Jahn, Emil Popow, Bernhard Roth, Paul Singh, Mudit Srivastava, Dieter Wolter
Astronomical instrumentation is most of the time faced with challenging requirements in terms of sensitivity, stability,
complexity, etc., and therefore leads to high performance developments that at first sight appear to be suitable only for
the specific design application at the telescope. However, their usefulness in other disciplines and for other applications
is not excluded. The ERA2 facility is a lab demonstrator, based on a high-performance astronomical spectrograph, which
is intended to explore the innovation potential of fiber-coupled multi-channel spectroscopy for spatially resolved
spectroscopy in life science, material sciences, and other areas of research.
MUSE (Multi Unit Spectroscopic Explorer) is a second generation instrument developed for ESO (European Southern
Observatory) to be installed on the VLT (Very Large Telescope) in year 2012. The MUSE project is supported by a
European consortium of 7 institutes. After a successful Final Design Review the project is now facing a turning point
which consist in shifting from design to manufacturing, from calculation to test, ... from dream to reality.
At the start, many technical and management challenges were there as well as unknowns. They could all be derived of
the same simple question: How to deal with complexity? The complexity of the instrument, of the work to de done, of
the organization, of the interfaces, of financial and procurement rules, etc.
This particular moment in the project life cycle is the opportunity to look back and evaluate the management methods
implemented during the design phase regarding this original question. What are the lessons learn? What has been
successful? What could have been done differently? Finally, we will look forward and review the main challenges of the
MAIT (Manufacturing Assembly Integration and Test) phase which has just started as well as the associated new
processes and evolutions needed.
MUSE (Multi Unit Spectroscopic Explorer) is a second generation instrument developed for ESO (European Southern Observatory) and will be assembled to the VLT (Very Large Telescope) in 2012. The MUSE instrument can simultaneously record 90.000 spectra in the visible wavelength range (465-930nm), across a 1*1arcmin2 field of view, thanks to 24 identical Integral Field Units (IFU). A collaboration of 7 institutes has successfully passed the Final Design Review and is currently working on the first sub-assemblies. The sharing of performances has been based on 5 main functional sub-systems. The Fore Optics sub-system derotates and anamorphoses the VLT Nasmyth focal plane image, the Splitting and Relay Optics associated with the Main Structure are feeding each IFU with 1/24th of the field of view.
Each IFU is composed of a 3D function insured by an image slicer system and a spectrograph, and a detection function
by a 4k*4k CCD cooled down to 163°K. The 5th function is the calibration and data reduction of the instrument. This
article depicts the breakdown of performances between these sub-systems (throughput, image quality...), and underlines
the constraining parameters of the interfaces either internal or with the VLT. The validation of all these requirements is a
critical task started a few months ago which requires a clear traceability and performances analysis.
Supercontinuum white light sources (SCLS) are intense, spatially coherent laser sources with a very broad and flat
spectral energy distribution which have very quickly found ubiquitous use in optical laboratories. As photonics is now
providing more and more applications for astronomical instrumentation, the possible use of SCLS as a calibration light
source for spectroscopy has been tested. A standard industrial SCLS was coupled to the calibration unit of the PMAS
integral field spectrophotometer and compared directly to the PMAS standard tungsten filament lamp that is normally
used for calibration exposures. We report on comparative measurements concerning flux, spectral energy distribution,
and temporal stability.
Astrophotonics offers a solution to some of the problems of building instruments for the next generation of telescopes
through the use of photonic devices to miniaturise and simplify instruments. It has already proved its worth in
interferometry over the last decade and is now being applied to nightsky background suppression. Astrophotonics offers
a radically different approach to highly-multiplexed spectroscopy to the benefit of galaxy surveys such as are required to
determine the evolution of the cosmic equation of state. The Astrophotonica Europa partnership funded by the EU via
OPTICON is undertaking a wide-ranging survey of the technological opportunities and their applicability to high-priority
astrophysical goals of the next generation of observatories. Here we summarise some of the conclusions.
The Multi-Unit Spectroscopic Explorer (MUSE) is an integral-field spectrograph for the ESO Very Large Telescope.
After completion of the Final Design Review in 2009, MUSE is now in its manufacture and assembly phase. To achieve
a relative large field-of-view with fine spatial sampling, MUSE features 24 identical spectrograph-detector units. The
acceptance tests of the detector sub-systems, the design and manufacture of the calibration unit and the development of
the Data Reduction Software for MUSE are under the responsibility of the AIP. The optical design of the spectrograph
implies strict tolerances on the alignment of the detector systems to minimize aberrations. As part of the acceptance
testing, all 24 detector systems, developed by ESO, are mounted to a MUSE reference spectrograph, which is illuminated
by a set of precision pinholes. Thus the best focus is determined and the image quality of the spectrograph-detector
subsystem across wavelength and field angle is measured.
The Visible Integral-Field Replicable Unit Spectrograph (VIRUS) is an integral field spectrograph to support
observations for the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX). The VIRUS instrument is fed by
more than 33,000 optical fibers and consists of 150 spectrographs in 75 individual, identical units. This paper discusses
the evolution in mechanical design of the VIRUS unit spectrographs to maximize the cost benefit from volume
production. Design features which enable volume manufacture and assembly are discussed. Strategies for reducing
part count while enabling precision alignment are detailed. Design considerations for deployment, operation, and
maintenance en mass at the Hobby-Eberly Telescope are also made. In addition, several enabling technologies are
described including the use of cast aluminum in vacuum housings, use of cast Invar, and processing cast parts for
precision tolerances.
The Visual Integral-Field Replicable Unit Spectrograph (VIRUS) instrument is being built to support observations for
the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) project. The instrument consists of 150+ identical
fiber-fed integral field optical spectrographs. This instrument provides a unique challenge in astronomical
instrumentation: each of the 150+ instruments must be identical and each component must be interchangeable amongst
every other spectrograph in order to ease assembly and maintenance of the instrument. In this paper we describe plans
for the production-line assembly of the spectrographs. In particular, we discuss the assembly procedures and design
choices that will ensure uniformity of the spectrographs and support the project schedule.
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.
The quantity and length of optical fibers required for the Hobby-Eberly Telescope* Dark Energy eXperiment
(HETDEX) create unique fiber handling challenges. For HETDEX‡, at least 33,600 fibers will transmit light from the
focal surface of the telescope to an array of spectrographs making up the Visible Integral-Field Replicable Unit
Spectrograph (VIRUS). Up to 96 Integral Field Unit (IFU) bundles, each containing 448 fibers, hang suspended from the
telescope's moving tracker located more than 15 meters above the VIRUS instruments. A specialized mechanical system
is being developed to support fiber optic assemblies onboard the telescope. The discrete behavior of 448 fibers within a
conduit is also of primary concern. A life cycle test must be conducted to study fiber behavior and measure Focal Ratio
Degradation (FRD) as a function of time. This paper focuses on the technical requirements and design of the HETDEX
fiber optic support system, the electro-mechanical test apparatus for accelerated life testing of optical fiber assemblies.
Results generated from the test will be of great interest to designers of robotic fiber handling systems for major
telescopes. There is concern that friction, localized contact, entanglement, and excessive tension will be present within
each IFU conduit and contribute to FRD. The test apparatus design utilizes six linear actuators to replicate the movement
of the telescope over 65,000 accelerated cycles, simulating five years of actual operation.
The PMAS integral field spectrophotometer, operated at the Calar Alto Observatory 3.5m Telescope, is one of the most
demanded instruments of its kind. The optical system was designed for a camera field of view to accommodate a 4K×4K
detector with 15μm pixels. However, due to a failure of one of the initially foreseen 2K×4K CCDs in a mosaic
configuration, only half of the available field of view could be covered to date. Owing to the high demand from the user
community, an upgrade to the full complement of 4K×4K pixels was envisaged, based on the availability of the new e2v
CCD231 device. We describe the specification, implementation, test, and commissioning of this new detector for PMAS.
The Visible Integral-field Replicable Unit Spectrograph (VIRUS) consists of a baseline build of 150 identical
spectrographs (arrayed as 75 units, each with a pair of spectrographs) fed by 33,600 fibers, each 1.5 arcsec diameter,
deployed over the 22 arcminute field of the upgraded 10 m Hobby-Eberly Telescope (HET). The goal is to deploy 96
units. VIRUS has a fixed bandpass of 350-550 nm and resolving power R~700. VIRUS is the first example of
industrial-scale replication applied to optical astronomy and is capable of spectral surveys of large areas of sky. The
method of industrial replication, in which a relatively simple, inexpensive, unit spectrograph is copied in large numbers,
offers significant savings of engineering effort, cost, and schedule when compared to traditional instruments.
The main motivator for VIRUS is to map the evolution of dark energy for the Hobby-Eberly Telescope Dark Energy
Experiment (HETDEX+) using 0.8M Lyman-α emitting galaxies as tracers. The full VIRUS array is due to be deployed
in late 2011 and will provide a powerful new facility instrument for the HET, well suited to the survey niche of the
telescope. VIRUS and HET will open up wide field surveys of the emission-line universe for the first time. We present
the design, cost, and current status of VIRUS as it enters production, and review performance results from the VIRUS
prototype. We also present lessons learned from our experience designing for volume production and look forward to
the application of the VIRUS concept on future extremely large telescopes (ELTs).
Summary: The Multi Unit Spectroscopic Explorer (MUSE) is a second-generation VLT panoramic integral-field
spectrograph currently in manufacturing, assembly and integration phase. MUSE has a field of 1x1 arcmin2 sampled at
0.2x0.2 arcsec2 and is assisted by the VLT ground layer adaptive optics ESO facility using four laser guide stars. The
instrument is a large assembly of 24 identical high performance integral field units, each one composed of an advanced
image slicer, a spectrograph and a 4kx4k detector. In this paper we review the progress of the manufacturing and report
the performance achieved with the first integral field unit.
innoFSPEC Potsdam is presently being established as in interdisciplinary innovation center for fiber-optical
spectroscopy and sensing, hosted by Astrophysikalisches Institut Potsdam and the Physical Chemistry group of Potsdam
University, Germany. The center focuses on fundamental research in the two fields of fiber-coupled multi-channel
spectroscopy and optical fiber-based sensing. Thanks to its interdisciplinary approach, the complementary methodologies
of astrophysics on the one hand, and physical chemistry on the other hand, are expected to spawn synergies that
otherwise would not normally become available in more standard research programmes. innoFSPEC targets future
innovations for next generation astrophysical instrumentation, environmental analysis, manufacturing control and
process monitoring, medical diagnostics, non-invasive imaging spectroscopy, biopsy, genomics/proteomics, high-throughput
screening, and related applications.
We have conducted extensive tests of both transmission and focal ratio degradation (FRD) on two integral field
units currently in use on the VIRUS-P integral field spectrograph. VIRUS-P is a prototype for the VIRUS
instrument proposed for the Hobby-Eberly Telescope at McDonald Observatory. All tests have been conducted
at an input f-ratio of F/3.65 and with an 18% central obscuration in order to simulate optical conditions on the
HET. Transmission measurements were conducted with narrow-band interference filters (FWHM: 10 nm) at 10
discrete wavelengths (337 to 600 nm), while FRD tests were made at 365 nm, 400 nm and 600 nm. The influence
of wavelength, end immersion, fiber type and length on both FRD and transmission is explored. Most notably,
we find no wavelength dependence on FRD down to 365 nm. All fibers tested are within the VIRUS instrument
specifications for both FRD and transmission. We present the details of our differential FRD testing method and
explain a simple and robust technique of aligning the test bench and optical fiber axes to within ±0.1 degrees.
The Multi-Unit Spectroscopic Explorer (MUSE) is an integral-field spectrograph for the VLT for the next decade. Using
an innovative field-splitting and slicing design, combined with an assembly of 24 spectrographs, MUSE will provide
some 90,000 spectra in one exposure, which cover a simultaneous spectral range from 465 to 930nm. The design and
manufacture of the Calibration Unit, the alignment tests of the Spectrograph and Detector sub-systems, and the
development of the Data Reduction Software for MUSE are work-packages under the responsibility of the AIP, who is a
partner in a European-wide consortium of 6 institutes and ESO, that is led by the Centre de Recherche Astronomique de
Lyon. MUSE will be operated and therefore has to be calibrated in a variety of modes, which include seeing-limited and
AO-assisted operations, providing a wide and narrow-field-of-view. MUSE aims to obtain unprecedented ultra-deep 3D-spectroscopic
exposures, involving integration times of the order of 80 hours at the VLT. To achieve the corresponding
science goals, instrumental stability, accurate calibration and adequate data reduction tools are needed. The paper
describes the status at PDR of the AIP related work-packages, in particular with respect to the spatial, spectral, image
quality, and geometrical calibration and related data reduction aspects.
During 2007, a new polarimetric observing mode was added to the existing integral-field spectrograph PMAS. Initially,
this instrumental upgrade is aimed to measure the linear polarization states and to determine the three Stokes parameters
I, Q and U. The PMAS instrument offers an integral-field of view of up to 256 square arcseconds, while the spectrograph
covers a wavelength region from 340 to 900 nm. The paper presents the opto-mechanical design of the polarimetric unit,
summarizes calibration and test results and describes the first data taken during commissioning at the Calar Alto
observatory. Given the range of applications and the large parameter space (two spatial coordinates, one wavelength
dimension, plus polarimetric information), the realization of the PMAS 2D-Spectro-Polarimeter provides a unique
capability for night-time astrophysical observations, such as the study of scattering processes or magnetic fields for a
range of astronomical targets.
The Hobby-Eberly Telescope Dark Energy eXperiment [HETDEX] will employ over 43,000 optical fibers to feed light
to 192 Visible Integral-Field Replicable Unit Spectrographs [VIRUS]. Each VIRUS instrument is fed by 224 fibers. To
reduce cost, the spectrographs are combined into pairs; thus, two bundles of 224 fibers are combined into a single
Integral Field Unit [IFU] of 448 fibers. On the input end the fibers are arranged in a square 'dense-pack' array at the
HET focal surface. At the output end the IFU terminates in two separate linear arrays which provide entry slits for each
spectrometer unit. The IFU lengths must be kept to an absolute minimum to mitigate losses; however, consideration of
overall project cost and duration of the science mission have resulted in the generation of two competing concepts.
Multiple axes of motion are imposed on the IFUs as they span the shortest distance from the focal surface to each
VIRUS unit. Arranging and supporting 96 IFUs, that have a total mass over 450 kg, in a manner that is compatible with
these complex translations, together with the management of accompanying forces on the tracking mechanism of the
HET, presents a significant technical challenge, which is further compounded by wind buffeting. The longer IFU
concept is favored due to overall project cost, but requires tests to assure that the fibers can withstand forces associated
with a height differential of 16.25 meters without FRD losses or breakage.
We describe the design, construction, and performance of VIRUS-P (Visible Integral-field Replicable Unit
Spectrograph - Prototype), the prototype for 150+ identical fiber-fed integral field spectrographs for the Hobby-Eberly
Telescope Dark Energy Experiment (HETDEX). VIRUS-P was commissioned in 2007, is in regular service on the
McDonald Observatory 2.7 m Smith telescope, and offers the largest field of any integral field spectrograph. The 246-fiber IFU uses a densepak-type fiber bundle with a 1/3 fill factor. It is fed at f/3.65 through a telecentric, two-group
dioptric focal reducer. The spectrograph's double-Schmidt optical design uses a volume phase holographic grating at
the pupil between the articulating f/3.32 folded collimator and the f/1.33 cryogenic prime focus camera. High on-sky
throughput is achieved with this catadioptric system by the use of high reflectivity dielectric coatings, which set the
340-670 nm bandwidth. VIRUS-P is gimbal-mounted on the telescope to allow short fibers for high UV throughput,
while maintaining high mechanical stability. The instrument software and the 18 square arcmin field, fixed-offset guider
provide rapid acquisition, guiding, and precision dithering to fill in the IFU field. Custom software yields Poisson noise
limited, sky subtracted spectra. The design characteristics are described that achieved uniformly high image quality with
low scattered light and fiber-to-fiber cross talk. System throughput exceeds requirements and peaks at 40%. The
observing procedures are described, and example observations are given.
VIRUS is a planned integral-field instrument for the Hobby-Eberly Telescope (HET). In order to achieve a large field-of-view and high grasp at reasonable costs, the approach is to replicate integral-field units (IFU) and medium sized spectrographs many times. The Astrophysical Institute Potsdam (AIP) contributes to VIRUS with the development and testing of the IFU prototype. While the overall project is presented by Hill et al.1, this paper describes the opto-mechanical design and the manufacture of the fiber-based IFU subsystem. The initial VIRUS development aims to produce a prototype and to measure its performance. Additionally, techniques will be investigated to allow industrial replication of the highly specific fiber-bundle layout. This will be necessary if this technique is to be applied to the next generation of even larger astronomical instrumentation.
We present the design of, and the science drivers for, the Visible Integral-field Replicable Unit Spectrograph (VIRUS). This instrument is made up of 145 individually small and simple spectrographs, each fed by a fiber integral field unit. The total VIRUS-145 instrument covers ~30 sq. arcminutes per observation, providing integral field spectroscopy from 340 to 570 nm, simultaneously, of 35,670 spatial elements, each 1 sq. arcsecond on the sky. This corresponds to 15 million resolution elements per exposure. VIRUS-145 will be mounted on the Hobby-Eberly Telescope and fed by a new wide-field corrector with 22 arcminutes diameter field of view. VIRUS represents a new approach to spectrograph design, offering the science multiplex advantage of huge sky coverage for an integral field spectrograph, coupled with the engineering multiplex advantage of >100 spectrographs making up a whole. VIRUS is designed for the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) which will use baryonic acoustic oscillations imprinted on the large-scale distribution of Lyman-α emitting galaxies to provide unique constraints on the expansion history of the universe that can constrain the properties of dark energy.
Unlike some integral field units (IFUs) in front of conventional slit spectrographs, PMAS is a dedicated fiber-optical integral field spectrograph, featuring two different types of IFUs to address both high spatial resolution and wide field-of-view (FoV) in a single instrument. The instrument was designed, built, and tested completely in-house at the Astrophysical Institute Potsdam from 1996 to 2000. It was commissioned at the Calar Alto 3.5m Telescope in May 2001. PMAS employs an all-refractive fiber spectrograph, built with CaF2 optics, to provide good transmission and high image quality over the entire nominal wavelength range. A set of user-selectable reflective gratings provides low to medium spectral resolution in first order of approx. 1.5, 3.2, and 7 Å, depending on the groove density (1200, 600, 300 gr/mm). The standard IFU uses a 16×16 element lens array, which provides seeing-limited sampling in a relatively small field-of-view (FOV) in one of three magnifications (8×8, 12×12, or 16×16 arcsec2, respectively). The additional fiber bundle IFU (PPak) expands the FOV to a hexagonal area with a footprint of 65×74 arcsec2.
The Multi Unit Spectroscopic Explorer (MUSE) is a second-generation VLT panoramic integral-field spectrograph under preliminary design study. MUSE has a field of 1x1 arcmin2 sampled at 0.2x0.2 arcsec2 and is assisted by the VLT ground layer adaptive optics ESO facility using four laser guide stars. The simultaneous spectral range is 0.465-0.93 μm, at a resolution of R~3000. MUSE couples the discovery potential of a large imaging device to the measuring capabilities of a high-quality spectrograph, while taking advantage of the increased spatial resolution provided by adaptive optics. This makes MUSE a unique and tremendously powerful instrument for discovering and characterizing objects that lie beyond the reach of even the deepest imaging surveys. MUSE has also a high spatial resolution mode with 7.5x7.5 arcsec2 field of view sampled at 25 milli-arcsec. In this mode MUSE should be able to obtain diffraction limited data-cubes in the 0.6-0.93 μm wavelength range. Although the MUSE design has been optimized for the study of galaxy formation and evolution, it has a wide range of possible applications; e.g. monitoring of outer planets atmosphere, environment of young stellar objects, super massive black holes and active nuclei in nearby galaxies or massive spectroscopic surveys of stellar fields in the Milky Way and nearby galaxies.
PPak is a new fiber-bundle, developed at the Astrophysical Institute Potsdam for the existing PMAS 3D-instrument. The intention of PPak is to provide a large integral field-of-view in combination with a large collecting area per fiber for the study of extended low-surface brightness objects. The PPak system consists of a focal reducer lens and a fiber bundle, featuring an innovative design with object, sky and calibration fibers. With a field-of-view of 74 x 65 arcseconds, PPak currently is the world's widest integral field unit that provides a semi-contiguous regular sampling of extended astronomical objects. Its pre-optics and fiber-diameter, combined with the versatility and efficiency of the PMAS spectrograph, allows PPak to make a unique trade-off between total light-collecting power and spectral resolution.
PMAS is a fiber-coupled lens array type of integral field spectrograph, which was commissioned at the Calar Alto 3.5m Telescope in May 2001. The optical layout of the instrument was chosen such as to provide a large wavelength coverage, and good transmission from 0.35 to 1 μm. One of the major objectives of the PMAS development has been to perform 3D spectrophotometry,
taking advantage of the contiguous array of spatial elements over
the 2-dimensional field-of-view of the integral field unit. With science results obtained during the first two years of operation, we illustrate that 3D spectroscopy is an ideal tool for faint object spectrophotometry.
The Multi Unit spectroscopic Explorer (MUSE) is a second generation VLT panoramic integral-field spectrograph operating in the visible wavelength range. MUSE has a field of 1 x 1 arcmin2 sampled at 0.2x0.2 arcsec2 and is assisted by a ground layer adaptive optics system using four laser guide stars. The simultaneous spectral range is 0.465-0.93 μm, at a resolution of R~3000. MUSE couples the discovery potential of a large imaging device to the measuring capabilities of a high-quality spectrograph, while taking advantage of the increased spatial resolution provided by adaptive optics. This makes MUSE a unique and tremendously powerful instrument for discovering and characterizing objects that lie beyond the reach of even the deepest imaging surveys. MUSE has also a high spatial resolution mode with 7.5 x 7.5 arcse2 field of view sampled at 25 milli-arcsec. In this mode MUSE should be able to get diffraction limited data-cube in the 0.6-1 μm wavelength range. Although MUSE design has been optimized for the study of galaxy formation and evolution, it has a wide range of possible applications; e.g. monitoring of outer planets atmosphere, young stellar objects environment, supermassive black holes and active nuclei in nearby galaxies or massive spectroscopic survey of stellar fields.
PMAS is a versatile integral field spectrograph based on the principle of a fiber-coupled lens array type of IFU. The instrument was commissioned at the Calar Alto 3.5m Telescope in May 2001. PMAS is offered as a common user instrument at Calar Alto since 2002. However, it has remained flexible enough to be used as a testbed for new observing techniques. Since the instrument is sensitive in the wavelength range from 0.35 to 1 μm, it is being used to experiment with faint object 3D spectroscopy for a variety of objects in stellar and extragalactic astronomy. Among these experiments, we have implemented a nod-shuffle mode of operation, which is a beam switching technique to achieve a high degree of sky subtraction accuracy. We describe the technical details of the special solution found for PMAS and first results obtained in test observations of faint haloes of planetary nebulae.
PMAS, the Potsdam Multi-Aperture Spectrophotometer, was successfully
commissioned at the Calar Alto 3.5m telescope during 2001. PMAS is a medium-resolution, lensarray/fiber based integral field spectrograph,
covering the whole optical wavelength range from 350 to 900 nm with optimized high efficiency in the blue. We review the commissioning activities and present the current status of this new instrument.
PMAS, the Potsdam Multi-Aperture Spectrophotometer, has a modular layout which was intended to provide for flexible operation as a travelling instrument and to accomodate different telescopes. The Telescope Module is the part of the instrument which serves the purpose of mechanical and optical interfacing to the telescope. It contains optical systems to re-image the telescope focal plane onto the lens array, to illuminate the lens array from an internal calibration light source, and to observe an area around the 3D spectroscopy field-of-view with a cryogenic CCD system for acquisition, guiding, and for the simultaneous determination of point-spread-function templates for 3D deconvolution. We discuss the opto-mechanical design and manufacture of these subsystems.
PMAS, the Potsdam Multi-Aperture Spectrophotometer, is a new integral field (IF or 3D) instrument. It features a lenslet/optical fiber type integral field module and a dedicated fiber
spectrograph. As the instrumental emphasis is on photometric stability and high efficiency, good flat field characteristic across the integral field is needed. The PMAS fiber module is unique in the sense that the design allows the replacement of individual fibers. This property, together with the fact that the fibers are index-matched at both ends, makes it possible to achieve and maintain a high efficiency. We present the opto-mechanical design for this fiber-module and, using various data sets from previous observing runs, demonstrate the increase of performance as a result of the optimization of the fiber-components.
Martin Roth, Svend-Marian Bauer, Frank Dionies, Thomas Fechner, Thomas Hahn, Andreas Kelz, Jens Paschke, Emil Popow, Juergen Schmoll, Dieter Wolter, Uwe Laux, Werner Altmann
PMAS has been designed and is currently being integrated as a traveling instrument of the Astrophysical Institute Potsdam. It is a UV-visual integral field spectrograph, with optimized efficiency and stability for use as a 3D spectrophotometer. PMAS is prototyped for first light at the Calar Alto 3.5m telescope with an option to go to other telescopes. We present the final design layout, details of the mechanics, optics, detector systems, and instrument control. We report on the current status of the integration.
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