4MOST is a new high-multiplex, wide-field spectroscopic survey facility under construction for ESO's 4m-VISTA telescope at Paranal, Chile. Its key specifications are: a large field of view of 4.4 square degrees, a high multiplex fibre positioner based on the tilting spine principle positioning 2436 science fibres, 1624 fibres going to two low-resolution spectrographs (R = λ/Δλ ~ 6500), and 812 fibres transferring light to the high-resolution spectrograph (R ~ 20,000). The instrument is entirely completed and is being shipped to Paranal Observatory, Chile in the first few months of 2024. Commissioning will take place summer 2024 with full operations expected to start early 2025. An overview will be given of instrument capabilities, the planned, and the unique operational scheme of 4MOST.
4MOST is a new high-multiplex, wide-field spectroscopic survey facility under construction for ESO's 4m-VISTA telescope at Paranal, Chile. Its key specifications are: a large field of view of 4.4 square degrees, a high multiplex fibre positioner based on the tilting spine principle that positions 2436 science fibres in the focal surface of which 1624 fibres go to two low-resolution optical spectrographs (R = λ/Δλ ~ 6500) and 812 fibres transfer light to the high-resolution optical spectrograph (R ~ 20,000). Currently, almost all subsystems are completed and full testing in Europe will be finished in spring 2023, after which 4MOST will be shipped to Chile. An overview is given of instrument construction and capabilities, the planned science of the consortium and the recently selected community programmes, and the unique operational scheme of 4MOST.
The new era of Multi-Object Spectrograph (MOS) Survey projects, in particular WEAVE (on the WHT at the ING) and 4MOST (on VISTA at ESO Paranal), require complex data flow systems. These systems encompass the software development for target selection, fibre configuration and observation at the telescope front-end and spectral processing, spectral analysis and archiving at the back-end. The system must also include quality control procedures, signaling mechanisms and alert reporting to ensure optimal use of telescope time and scientifically robust data products. Key to ensuring a fully functioning data flow system by first light are Operational Rehearsals (OpR) which use simulated data in end-to-end tests of the entire system. The Cambridge Astronomical Survey Unit (CASU) has been integral in defining and coordinating these OpR efforts, in its role of providing the back-end data management and the spectral processing pipelines, for both WEAVE and 4MOST. The WEAVE OpR programme is complete and we await first light. The first two rehearsal stages (OpR1 and OpR2) of the 4MOST OpR programme are complete while the third, and most complex, stage will commence in 2022.
We present an update on the overall integration progress of the WEAVE next-generation spectroscopy facility for the William Herschel Telescope (WHT), now scheduled for first light in early-2021, with almost all components now arrived at the observatory. We also present a summary of the current planning behind the 5-year initial phase of survey operations, and some detailed end-to-end science simulations that have been implemented to evaluate the final on-sky performance after data processing. WEAVE will provide optical ground-based follow up of ground-based (LOFAR) and space-based (Gaia) surveys. WEAVE is a multi-object and multi-IFU facility utilizing a new 2-degree prime focus field of view at the WHT, with a buffered pick-and-place positioner system hosting 1000 multi-object (MOS) fibres, 20 mini integral field units, or a single large IFU for each observation. The fibres are fed to a single (dual-beam) spectrograph, with total of 16k spectral pixels, located within the WHT GHRIL enclosure on the telescope Nasmyth platform, supporting observations at R~5000 over the full 370-1000nm wavelength range in a single exposure, or a high resolution mode with limited coverage in each arm at R~20000.
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.
We present an update on the overall construction progress of the WEAVE next-generation spectroscopy facility for the William Herschel Telescope (WHT), now that all the major fabrication contracts are in place. We also present a summary of the current planning behind the 5-year initial phase of survey operations, and some detailed end-to-end science simulations that have been effected to evaluate the final on-sky performance after data processing. WEAVE will provide optical ground-based follow up of ground-based (LOFAR) and space-based (Gaia) surveys. WEAVE is a multi-object and multi-IFU facility utilizing a new 2-degree prime focus field of view at the WHT, with a buffered pick-and-place positioner system hosting 1000 multi-object (MOS) fibres, 20 integral field units, or a single large IFU for each observation. The fibres are fed to a single (dual-beam) spectrograph, with total of 16k spectral pixels, located within the WHT GHRIL enclosure on the telescope Nasmyth platform, supporting observations at R~5000 over the full 370-1000nm wavelength range in a single exposure, or a high resolution mode with limited coverage in each arm at R~20000. The project has experienced some delays in procurement and now has first light expected for the middle of 2019.
We present an overview and status update of the 4MOST project at the Final Design Review. 4MOST is a major new wide-field, high-multiplex spectroscopic survey facility under development for the VISTA telescope at the Paranal Observatory of ESO. Starting in 2022, 4MOST will deploy 2436 optical fibres in a 4.1 square degree field-of-view using a fibre positioner based on the tilting spine principle. The fibres will feed one high-resolution (R~20,000) and two low-resolution (R~5000) spectrographs that all have fixed configuration, 3-channel designs with identical 6k x 6k CCD detectors. Updated performance estimates will be presented based on components already manufactured and pre-production prototypes of critical subsystems.
The 4MOST science goals are mostly driven by a number of large area, space-based observatories of prime European interest: Gaia and PLATO (Galactic Archeology and Stellar Physics), eROSITA (High-Energy Sky), and Euclid (Cosmology and Galaxy Evolution). Science cases based on these observatories, along with wide-area ground-based facilities such as LSST, VISTA and VST drive the ten Consortium Surveys covering a large fraction of the Southern sky, with bright time mostly devoted to the Milky Way disk and bulge areas and the Magellanic Clouds, and the dark/gray time largely devoted to extra-galactic targets. In addition there will be a significant fraction of the fibre-hours devoted to Community Surveys, making 4MOST a true general-purpose survey facility, capable of delivering spectra of samples of objects that are spread over a large fraction of the sky.
The 4MOST Facility Simulator was created to show the feasibility of the innovative operations scheme of 4MOST with all surveys operating in parallel. The simulator uses the mock catalogues created by the science teams, simulates the spectral throughput and detection of the objects, assigns the fibres at each telescope pointing, creates pointing distributions across the sky and simulates a 5-year survey (including overhead, calibration and weather losses), and finally does data quality analyses and computes the science Figure-of-Merits to assess the quality of science produced. The simulations prove the full feasibility of running different surveys in parallel.
We present an overview of the 4MOST project at the Preliminary Design Review. 4MOST is a major new wide-field, high-multiplex spectroscopic survey facility under development for the VISTA telescope of ESO. 4MOST has a broad range of science goals ranging from Galactic Archaeology and stellar physics to the high-energy physics, galaxy evolution, and cosmology. Starting in 2021, 4MOST will deploy 2436 fibres in a 4.1 square degree field-of-view using a positioner based on the tilting spine principle. The fibres will feed one high-resolution (R~20,000) and two medium resolution (R~5000) spectrographs with fixed 3-channel designs and identical 6k x 6k CCD detectors. 4MOST will have a 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. The 4MOST Facility Simulator (4FS) was developed to demonstrate the feasibility of this observing concept, showing that we can expect to observe more than 25 million objects in each 5-year survey period and will eventually be used to plan and conduct the actual survey.
We present the Final Design of the WEAVE next-generation spectroscopy facility for the William Herschel Telescope (WHT), together with a status update on the details of manufacturing, integration and the overall project schedule now that all the major fabrication contracts are in place. We also present a summary of the current planning behind the 5-year initial phase of survey operations. WEAVE will provide optical ground-based follow up of ground-based (LOFAR) and space-based (Gaia) surveys. WEAVE is a multi-object and multi-IFU facility utilizing a new 2-degree prime focus field of view at the WHT, with a buffered pick-and-place positioner system hosting 1000 multi-object (MOS) fibres, 20 integral field units, or a single large IFU for each observation. The fibres are fed to a single (dual-beam) spectrograph, with total of 16k spectral pixels, located within the WHT GHRIL enclosure on the telescope Nasmyth platform, supporting observations at R~5000 over the full 370-1000nm wavelength range in a single exposure, or a high resolution mode with limited coverage in each arm at R~20000. The project is now in the manufacturing and integration phase with first light expected for early of 2018.
C. Jakob Walcher, Roelof de Jong, Tom Dwelly, Olga Bellido, Thomas Boller, Cristina Chiappini, Sofia Feltzing, Mike Irwin, Richard McMahon, Andrea Merloni, Olivier Schnurr, Nicholas Walton
The 4MOST instrument is a multi-object spectrograph to be mounted to the VISTA telescope at ESOs La- Silla-Paranal observatory. 4MOST will deliver several 10s of millions of spectra from surveys typically lasting 5 years. 4MOST will address Galactic and extra-galactic science cases simultaneously, i.e. by observing targets from a large number of different surveys within one science exposure. This parallel mode of operations as well as the survey nature of 4MOST require some 4MOST-specific operations features within the overall operations model of ESO. These features are necessary to minimize any changes to the ESO operations model at the La- Silla-Paranal observatory on the one hand, and to enable parallel science observing and thus the most efficient use of the instrument on the other hand. The main feature is that the 4MOST consortium will not only deliver the instrument, but also contractual services to the user community, which is why 4MOST is also described as a 'facility'. We describe the operations model for 4MOST as seen by the consortium building the instrument. Among others this encompasses: 1) A joint science team for all participating surveys (i.e. including community surveys as well as those from the instrument-building consortium). 2) Common centralized tasks in observing preparation and data management provided as service by the consortium. 3) Transparency of all decisions to all stakeholders. 4) Close interaction between science and facility operations. Here we describe our efforts to make parallel observing mode efficient, flexible, and manageable.
The 4MOST[1] instrument is a concept for a wide-field, fibre-fed high multiplex spectroscopic instrument facility on the
ESO VISTA telescope designed to perform a massive (initially >25x106 spectra in 5 years) combined all-sky public
survey. The main science drivers are: Gaia follow up of chemo-dynamical structure of the Milky Way, stellar radial
velocities, parameters and abundances, chemical tagging; eROSITA follow up of cosmology with x-ray clusters of
galaxies, X-ray AGN/galaxy evolution to z~5, Galactic X-ray sources and resolving the Galactic edge;
Euclid/LSST/SKA and other survey follow up of Dark Energy, Galaxy evolution and transients. The surveys will be
undertaken simultaneously requiring: highly advanced targeting and scheduling software, also comprehensive data
reduction and analysis tools to produce high-level data products. The instrument will allow simultaneous observations of
~1600 targets at R~5,000 from 390-900nm and ~800 targets at R<18,000 in three channels between ~395-675nm
(channel bandwidth: 45nm blue, 57nm green and 69nm red) over a hexagonal field of view of ~ 4.1 degrees. The initial
5-year 4MOST survey is currently expect to start in 2020. We provide and overview of the 4MOST systems: optomechanical,
control, data management and operations concepts; and initial performance estimates.
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].
WEAVE is an approved massive wide field multi-object optical spectrograph (MOS) currently entering its build phase, destined for use on the 4.2-m William Herschel Telescope (WHT). It will be commissioned and begin survey operations in 2017. This paper describes the core processing system (CPS) system being developed to process the bulk data flow from WEAVE. We describe the processes and techniques to be used in producing the scientifically validated 'Level 1' data products from the WEAVE data. CPS outputs will include calibrated one-d spectra and initial estimates of basic parameters such as radial velocities (for stars) and redshifts (for galaxies).
We present an overview of and status report on the WEAVE next-generation spectroscopy facility for the William
Herschel Telescope (WHT). WEAVE principally targets optical ground-based follow up of upcoming ground-based
(LOFAR) and space-based (Gaia) surveys. WEAVE is a multi-object and multi-IFU facility utilizing a new 2-degree
prime focus field of view at the WHT, with a buffered pick-and-place positioner system hosting 1000 multi-object
(MOS) fibres, 20 integral field units, or a single large IFU for each observation. The fibres are fed to a single
spectrograph, with a pair of 8k(spectral) x 6k (spatial) pixel cameras, located within the WHT GHRIL enclosure on the
telescope Nasmyth platform, supporting observations at R~5000 over the full 370-1000nm wavelength range in a single
exposure, or a high resolution mode with limited coverage in each arm at R~20000. The project is now in the final
design and early procurement phase, with commissioning at the telescope expected in 2017.
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.
We present the preliminary design of the WEAVE next generation spectroscopy facility for the William Herschel
Telescope (WHT), principally targeting optical ground-based follow up of upcoming ground-based (LOFAR) and spacebased
(Gaia) surveys. WEAVE is a multi-object and multi-IFU facility utilizing a new 2 degree prime focus field of view
at the WHT, with a buffered pick and place positioner system hosting 1000 multi-object (MOS) fibres or up to 30
integral field units for each observation. The fibres are fed to a single spectrograph, with a pair of 8k(spectral) x 6k
(spatial) pixel cameras, located within the WHT GHRIL enclosure on the telescope Nasmyth platform, supporting
observations at R~5000 over the full 370-1000nm wavelength range in a single exposure, or a high resolution mode with
limited coverage in each arm at R~20000.
Wide-field multi-object spectroscopy is a high priority for European astronomy over the next decade. Most 8-10m
telescopes have a small field of view, making 4-m class telescopes a particularly attractive option for wide-field
instruments. We present a science case and design drivers for a wide-field multi-object spectrograph (MOS) with
integral field units for the 4.2-m William Herschel Telescope (WHT) on La Palma. The instrument intends to take
advantage of a future prime-focus corrector and atmospheric-dispersion corrector (Agocs et al, this conf.) that will
deliver a field of view 2 deg in diameter, with good throughput from 370 to 1,000 nm. The science programs cluster into
three groups needing three different resolving powers R: (1) high-precision radial-velocities for Gaia-related Milky Way
dynamics, cosmological redshift surveys, and galaxy evolution studies (R = 5,000), (2) galaxy disk velocity dispersions
(R = 10,000) and (3) high-precision stellar element abundances for Milky Way archaeology (R = 20,000). The multiplex
requirements of the different science cases range from a few hundred to a few thousand, and a range of fibre-positioner
technologies are considered. Several options for the spectrograph are discussed, building in part on published design
studies for E-ELT spectrographs. Indeed, a WHT MOS will not only efficiently deliver data for exploitation of
important imaging surveys planned for the coming decade, but will also serve as a test-bed to optimize the design of
MOS instruments for the future E-ELT.
Gaia is an approved ESA cornerstone project, currently scheduled for launch in late 2011. Gaia will provide photometric, positional, spectroscopic and radial velocity measurements with the accuracies needed to produce a stereoscopic and kinematic census of about one billion stars in our Galaxy and throughout the Local Group, addressing its core science goals to quantify the formation and assembly history of a large spiral galaxy, the Milky Way. Gaia will achieve this by obtaining a six-dimensional (spatial & kinematic) phase-space map of the Galaxy, complemented by an optimised high-spatial resolution multi-colour photometric survey, and the largest stellar spectroscopic and radial velocity surveys ever made. The Gaia data set will be constructed from 2 × 1012 observations (image CCD transits), whose analysis is a very complex task, involving both real-time (this proposal) and end-of-mission data products. This paper describes the UK Gaia Data Flow System activities as part of the emerging European wide Gaia Data Processing system. We describe the data processing challenges that need to be overcome to meet the heavy demands placed by Gaia. We note the construction processes required to handle the photometric reduction of the data from Gaia's 100+ focal plane CCDs, the pipeline needed to support the 'science alerts' and epoch photometry handling, and the spectroscopic processing system. We note the system software and hardware architecture, and how the data products will be generated to ensure compliance with emerging VO standards.
KEYWORDS: Cameras, Facial recognition systems, Projection systems, 3D image processing, Sensors, 3D modeling, Databases, Stereoscopic cameras, Data modeling, 3D metrology
We describe a camera capable of recording 3D images of objects. It does this by projecting thousands of spots onto an object and then measuring the range to each spot by determining the parallax from a single frame. A second frame can be captured to record a conventional image, which can then be projected onto the surface mesh to form a rendered skin.
The camera is able of locating the images of the spots to a precision of better than one tenth of a pixel, and from this it can determine range to an accuracy of less than 1 mm at 1 meter. The data can be recorded as a set of two images, and is reconstructed by forming a 'wire mesh' of range points and morphing the 2 D image over this structure. The camera can be used to record the images of faces and reconstruct the shape of the face, which allows viewing of the face from various angles. This allows images to be more critically inspected for the purpose of identifying individuals. Multiple images can be stitched together to create full panoramic images of head sized objects that can be viewed from any direction. The system is being tested with a graph matching system capable of fast and accurate shape comparisons for facial recognition. It can also be used with "models" of heads and faces to provide a means of obtaining biometric data.
KEYWORDS: Astronomy, Observatories, Galactic astronomy, Data modeling, Radio astronomy, X-ray astronomy, Astronomical imaging, Radio optics, X-ray optics, Data storage
The AstroGrid (http://www.astrogrid.org) project is developing a
virtual observatory capability to support efficient and effective
exploitation of key astronomical data sets of importance to the UK
community. It's initial focus is providing the necessary data-grid
infrastructure and data-mining tools to support data generated by
projects such as WFCAM, VISTA, e-MERLIN, SOHO and Cluster. AstroGrid
is a partnership formed by UK archive centres and astronomical
computer scientists. Key capabilities of AstroGrid enable
multi-disciplinary astronomy, making use of data streams from
frontline astronomical instrumentation. This paper presents the
development and deployment plans of AstroGrid, describing the products
and capabilities already released through the fifth project iteration
release. Use of these in early adopter science programmes is noted.
AstroGrid is a strongly science driven project that aims to deploy
relevant aspects of Grid and Data-Grid technologies. These are
discussed here, with an in-depth treatment of specific AstroGrid
technological developments to support e.g. collaborative workspaces in
the form of MySpace, being discussed elsewhere in this conference.
Finally, AstroGrid's close involvement in broader European
initiatives, the Astrophysical Virtual Observatory (AVO) and the
International Virtual Observatory Alliance (IVOA) is highlighted.
MySpace is a component of AstroGrid, the Virtual Observatory
infrastructure system being developed in the UK under the national
e-Science programme. The MySpace service will provide both temporary
and long-term storage for Virtual Observatory users. This work space
will typically be used to hold results extracted from archives, but can hold any sort of data. In addition, the MySpace service will provide cache storage for distributed processes which are running on the user's behalf. The novel feature of the MySpace service is that, although the individual items are geographically dispersed, the user can access and navigate the work space seamlessly and easily, as though all the items were stored in a single location. MySpace is written in Java and deployed as a set of Web services. It is a fully integrated component of the AstroGrid system, but its modular nature means that it can be installed and used in isolation or, in principle, in conjunction with components from other Virtual Observatory projects. Functionality similar to that of MySpace is likely to be a common requirement in Virtual Observatory projects. MySpace is under active development and its current state and future plans are described.
Current astronomical facilities on the WWW support anonymous access to public-domain resources with very limited workflows. To meet even current aspirations, the Virtual Observatory needs to operate extensive workflows that also include access to restricted resources.
AstroGrid (see http://www.astrogrid.org/), a UK eScience project with collaborating groups drawn from the major UK data archive centres, is currently creating the UK's virtual observatory (Lawrence, 2002, these proceedings). We present use cases from AstroGrid's survey of requirements that show a need for a pervasive infrastructure for identifying users and controlling access to facilities and data. We describe in outline AstroGrid's architecture for this infrastructure.
We have proposed a new Nasmyth instrument for the William Herschel Telescope which exploits the potential of wide field-of-view correction of atmospheric turbulence to produce a versatile, high spatial resolution, high efficiency, multi-object spectrograph and imager optimized for the 0.7-1.6 micron region. Using a low-altitude Rayleigh beacon guide star to correct the boundary layer turbulence which dominates the atmospheric seeing at La Palma on more than 25 percent of nights, MOSAIC combines the angular resolution gains of adaptive optics with the observing efficiency gains of multiple-object spectroscopy. Additional operating modes could include a narrow-band tunable filter and a fiber feed to a bench-mou8nted high resolution echelle spectrography. The instruments would provide a unique capability on 4-meter telescopes, opening up a wide variety of new scientific capabilities ranging from spectroscopic studies of crowded star fields to resolved studies of the kinematics of distant galaxies.
Imaging surveys of the bright 5007 angstrom line in nearby early-type galaxies and the bulges of spirals have catalogued many planetary nebulae. Planetary nebulae arise from the late stages of evolution of low mass stars and are thus representative of a large fraction of the stellar population by number. In about 80 percent of planetary nebulae the abundances of the well observed lighter elements are not affected by the nucleo synthesis which occurs on the Asymptotic Giant Branch, so the nebular abundances can be related to those of the progenitor star. Planetary nebular abundances compared with those of H II regions in spirals, as indicators of abundance gradients and enrichment history. Planetary nebulae provide point probes of the stellar abundance and, in contrast to integrated line of sight stellar spectra, can be used to measure the abundance spread.
The advent of new large CCD array cameras necessitates computing systems that are highly optimized but also enable flexibility of operation and ease of programming. We describe `UltraDAS', a CCD-control and data-acquisition system for the Isaac Newton Group of Telescopes that achieves these aims by combining high-performance detector- controllers with modern programming techniques on current UNIX workstations.
The Isaac Newton Group comprises three telescopes: the 4.2m William Herschel Telescope, the 2.5m Isaac Newton Telescope, and the 1.0m Jacobus Kaptyen Telescope. The operational capability of the ING has been increased by integrating the fault reporting system with the archiving of data. All data obtained from the telescope are automatically archived and stored on-line in a 500 slot CDROM jukebox. The flexible image transport system headers are stripped, stored in a Sybase database and are available immediately for inspection via a web-based user interface. Users have the option to save files to disc for FTP download and display the data using a standard image tool. After six months the original data are sent from the ING to the RGO Astronomy Data Center in Cambridge. The ING science archive may be interrogated, and the data is available for general download. The ING fault database is also implemented as a Sybase database. In addition to standard features, links can be made to individual data files. These can be subsequently downloaded from the archive on request. This system greatly aids in ensuring the integrity of data obtained across the ING telescopes and helps engineers when analyzing many kinds of faults. Access to data on-line is being exploited in automating the dissemination of data obtained during service observing. Pipeline processed data will also be integrated into the system. In order to handle increased data flows with new larger CCD arrays, a system based on high capacity DVD disks is planned.
The computing equipment of the 2.5-m Isaac Newton Telescope and the 1.0-m Jacobus Kapteyn Telescope is being upgraded to improve improve observing efficiency and ease of use, and to reduce maintenance and operation costs. These upgrades have been staged over a period of two years to reduce the impact on operations. Elements of this architecture will be used in the forthcoming upgrades to the 4.2-m William Herschel Telescope. The revised systems have allowed the introduction of a major new instrument for the INT: the Wide Field Camera, shortly to be equipped with a mosaic of four 4096 by 2048 EEV CCDs. On the JKT, the new equipment paves the way for remote operation.
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