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Volume 5492 Ground-based Instrumentation for Astronomy

Alan F. M. Moorwood, Masanori Iye September 2004

Conference Location: Glasgow, Scotland, United Kingdom Conference Date: Monday 21 June 2004

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Overview of Instrumentation at Major Observatories I

Select this Article		Instrumentation at the Keck Observatory Ian S. McLean and Sean Adkins Proc. SPIE 5492, 1 (2004); http://dx.doi.org/10.1117/12.552154 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The twin 10-m telescopes of the W.M. Keck Observatory have now been in operation for almost a decade. The original complement of first generation instruments remains in use (NIRC, HIRES, LRIS, and LWS) and all second generation instruments have been commissioned and are in regular operation (NIRSPEC, ESI, NIRC2 and DEIMOS). Both telescopes are equipped with Adaptive Optics (AO) systems, but only Keck II is equipped for AO science at the present time. Several detector upgrades and new third generation instruments are in progress. The blue side of the LRIS double spectrograph received two new E2V 2k x 4k CCDs in July 2002 and a 3-CCD mosaic upgrade to HIRES is scheduled for commissioning in mid-2004. An upgrade of the LRIS-R CCD is planned for completion in late 2005. The near-infrared integral field spectrometer for AO (OSIRIS) has passed critical design review and is in advanced fabrication, and studies for a near-infrared multi-object spectrometer are in the preliminary design phase. An Atmospheric Dispersion Compensator (ADC) for LRIS is currently under development. Other major developments include regular operation of the Keck-Keck interferometer, and the first successful closed-loop operations with the Laser Guide Star on Keck II.

Select this Article		Instrumentation at the ESO VLT Alan F. M. Moorwood Proc. SPIE 5492, 13 (2004); http://dx.doi.org/10.1117/12.553117 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract ESO celebrated the end of the first 5 years of very successful operation of its VLT in Chile on 1st April 2004 and is now set to expand this facility further with the addition of several 1.8 m, movable outrigger telescopes for interferometry, the VST (VLT survey telescope) and the VISTA (infrared) survey telescope. Here I will review briefly the status of the 8 operational 1st generation VLT/VLTI instruments plus the 3 in commissioning and the 3 still in development and will introduce the first 3 of the 2nd generation instruments which have recently been approved. I will also discuss briefly some of the 'Lessons Learned' from the development of the 1st generation instruments during an exercise conducted in 2003 with the participation of the external consortia of institutes to which ESO contracted out much of the instrument development.

Select this Article		Subaru instrumentation: today and tomorrow Masanori Iye Proc. SPIE 5492, 23 (2004); http://dx.doi.org/10.1117/12.552485 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract An updated overview of the performance and science achievements of the first generation observational instruments for the 8,2-m Subaru Telescope (http://subarutelescope.org/index.html) is presented. Also given is the status of the development of the second generation instruments.

Select this Article		Current and future facility instruments at the Gemini Observatory Douglas A. Simons, Joseph B. Jensen, Peter Gray, Manuel Lazo, Rolando Rogers, and John White Proc. SPIE 5492, 35 (2004); http://dx.doi.org/10.1117/12.549497 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Gemini's instrument program, which has existed for about a decade, has recently produced enough instruments to fully populate all of the instrument ports on both Gemini-N and Gemini-S. These delivered instruments, as well as those currently under construction and due to be delivered in the next ~2 years, are described in this report. We also summarize the bold new directions Gemini's development program will go in the next 5-10 years, as our Community embarks upon a new science mission to answer some of the most fundamental questions in astronomy.

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Overview of Instrumentation at Major Observatories II

Select this Article		First-generation instruments for the Magellan telescopes: characteristics, operation, and performance David J. Osip, Mark M. Phillips, Rebecca Bernstein, Greg Burley, Alan Dressler, James L. Elliot, Eric Persson, Stephen A. Shectman, and Ian Thompson Proc. SPIE 5492, 49 (2004); http://dx.doi.org/10.1117/12.552414 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Magellan Telescopes are a collaboration between the Observatories of the Carnegie Institution of Washington (OCIW), University of Arizona, Harvard University, University of Michigan, and Massachusetts Institute of Technology (MIT) consisting of two 6.5 meter telescopes located at Las Campanas Observatory, in the Chilean Andes. The Walter Baade telescope achieved first light in September 2000 and the Landon Clay telescope started science operations in September 2002. In addition to two modified spectroscopic instruments, the Boller and Chivens Spectrograph and the Low Dispersion Survey Spectrograph (LDSS-2), four first generation instruments are now deployed at the Magellan Telescopes. Here we briefly describe the operations and performance of MagIC - a direct imaging CCD camera, MIKE - a double echelle spectrograph, PANIC - a near-IR imager, and IMACS - a multi-purpose, multi-object imaging spectrograph.

Select this Article		The first-generation instruments for the Southern African Large Telescope (SALT) David A. H. Buckley, Peter L. Cottrell, Kenneth H. Nordsieck, Darragh E. O'Donoghue, and Ted B. Williams Proc. SPIE 5492, 60 (2004); http://dx.doi.org/10.1117/12.551291 \| Cited 6 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Southern African Large Telescope (SALT), which had its ground-breaking in September 2000, is rapidly nearing completion, with commissioning planned for most of 2004 and first science observations due to begin in early 2005. This paper describes the design and status of the SALT instrumentation, including the facility instruments (e.g. atmospheric dispersion compensator, guidance system, etc) and the First Generation science instruments: SALTICAM, a high-speed optical imager, PFIS, a versatile prime focus imaging spectrograph and SALT HRS, a fiber-fed high resolution echelle spectrograph. These first instruments are confined to the UV-visible region, and in the case of the first two, optimized for UV-blue performance, with a capability down to ~320 nm. The First Generation instruments, which are all seeing limited, will provide the following capabilities: broad and narrow band imaging, long-slit and multi-object spectroscopy (up to R ~ 6000), spectropolarimetry, Fabry-Perot imaging spectroscopy and precision high resolution spectroscopy (up to R ~ 80,000). Time resolved studies are an important aspect of the overall SALT science drivers and special efforts are being made to ensure an ability to run at >10 Hz, with minimal dead time, by employing frame transfer CCDs on two of the instruments (SALTICAM and PFIS). SALTICAM was installed on SALT in October 2003, while its full imaging mode will be commissioned in 2004. PFIS is currently on schedule for integration on SALT in December 2004, while SALT HRS is due to complete its Preliminary Design Review in July 2004.

Select this Article		Instrumentation at the Anglo-Australian Observatory Samuel C. Barden Proc. SPIE 5492, 75 (2004); http://dx.doi.org/10.1117/12.550286 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Anglo-Australian Observatory (AAO) has an instrumentation group for engineering, design, and fabrication that integrates tightly with an energetic group of instrument scientists1 to develop complex astronomical instruments. This instrumentation group puts ideas for innovative technical solutions generated by the instrument scientist group into reality. One demonstration of past achievement is the highly ambitious and successful 2dF instrument that yielded invaluable scientific insight into the cosmological structure of the universe. The more recent successes of the instrumentation group include the OzPoz fiber positioner for the FLAMES facility on the VLT and the award-winning, imaging and multi-object IRIS-2 infrared spectrograph for the AAT. VPH gratings were first put into action in LDSS++ on the AAT and numerous VPH gratings are now in routine use on the 6dF spectrograph for the UKST. Under development are a completely new and unique fiber positioning scheme (Echidna) for use in the FMOS instrument for Subaru; a double-beamed, VPH-based, bench-mounted spectrograph for 2dF; new IR and optical detector controllers; a renovation of the telescope and instrument control systems for the AAT; and a feasibility study for an Echidna-style positioner for the Gemini telescopes. Several other design studies are underway for new instrument technologies using leading edge and innovative concepts in robotics and fibers. The synergy between our scientists and engineers establishes a sound basis for solving the instrumentation challenges facing us.

Select this Article		Facility instruments for the GTC Jose M. Rodriguez Espinosa, Maria Luisa Garcia-Vargas, and Peter L. Hammersley Proc. SPIE 5492, 82 (2004); http://dx.doi.org/10.1117/12.551387 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Gran Telescopio Canarias (GTC1) 10m telescope is now being integrated at the ORM, in La Palma Spain. Likewise, three instruments are being prepared for first light and, as of this writing, are about to start their laboratory integration. These first light instruments are: 1) OSIRIS, a large field of view imager and multi-object spectrograph, optimized for tuneable filter imaging, 2) ELMER a very sensitive imager and spectrograph, also for the visible range, and 3) CANARICAM, a diffraction-limited imager, spectrograph, polarimeter and coronagrapher for the mid-IR. The GTC set of first light instruments will offer some special observational capabilities to the astronomical community, namely Tuneable filter Imaging in OSIRIS, fast spectroscopy and photometry in both, ELMER and OSIRIS, and 10 microns Coronagraphy and Polarimetry with CANARICAM.Yet another instrument, EMIR, a large field, near-IR multi-object spectrograph and imager is in the Detailed Design phase. EMIR will be the first of the GTC second generation set of instruments. At the planning stage are several future instruments that will arrive to the GTC with different calendars after Day One. In particular, FRIDA, a near-IR diffraction-limited imager and spectrograph, that will operate with the GTC Adaptive Optics system. FRIDA's conceptual design is being started by a consortium lead by UNAM (Mexico) and in which the IAC and the University of Florida also participate. FRIDA should be at the telescope by the time that the AO system is having first light. This is expected by late 2007 early 2008. There is interest in the GTC community for installing visiting instruments on the GTC, thus the GTC board is discussing a policy to allow visitor instruments, some of which have already been proposed to be hosted by the GTC. In particular, CIRCE is a near IR camera that is being built by the Department of Astronomy of the University of Florida in Gainesville for the GTC using private funds, under the GTC visitor instrument scheme. CIRCE should bridge the gap between Day One and the arrival of EMIR enabling near IR imaging capabilities to the GTC.

Select this Article		Performance of the Hobby-Eberly Telescope and facility instruments Gary J. Hill, Phillip J. MacQueen, Lawrence W. Ramsey, and Matthew D. Shetrone Proc. SPIE 5492, 94 (2004); http://dx.doi.org/10.1117/12.552439 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Hobby-Eberly Telescope (HET) is a revolutionary large telescope of 9.2 meter aperture, located in West Texas at McDonald Observatory. The HET operates with a fixed segmented primary and has a tracker which moves the four-mirror corrector and prime focus instrument package to track the sidereal and non-sidereal motions of objects. The HET has been taking science data for five years, but the image quality and primary mirror stability have been far from specifications. Work over the past two years has improved performance significantly, and demonstrated site-seeing limited images of 0.8 arcsec., showing that the telescope will meet all specifications. The performance of the HET is discussed in detail.The first phase of HET instrumentation includes three facility instruments: the Low Resolution Spectrograph (LRS), the Medium Resolution Spectrograph (MRS), and High Resolution Spectrograph (HRS). The current status of the instruments is described. Upcoming near infrared capabilities for the LRS and MRS are also discussed.

Select this Article		An overview of instrumentation for the Large Binocular Telescope R. Mark Wagner Proc. SPIE 5492, 108 (2004); http://dx.doi.org/10.1117/12.550645 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract An overview of instrumentation for the Large Binocular Telescope is presented. Optical instrumentation includes the Large Binocular Camera (LBC), a pair of wide-field (27'x 27') UB/VRI optimized mosaic CCD imagers at the prime focus, and the Multi-Object Double Spectrograph (MODS), a pair of dual-beam blue-red optimized long-slit spectrographs mounted at the straight-through F/15 Gregorian focus incorporating multiple slit masks for multi-object spectroscopy over a 6\arcmin\ field and spectral resolutions of up to 8000. Infrared instrumentation includes the LBT Near-IR Spectroscopic Utility with Camera and Integral Field Unit for Extragalactic Research (LUCIFER), a modular near-infrared (0.9-2.5 μm) imager and spectrograph pair mounted at a bent interior focal station and designed for seeing-limited (FOV: 4'x 4') imaging, long-slit spectroscopy, and multi-object spectroscopy utilizing cooled slit masks and diffraction limited (FOV: 0'.5 x 0'.5) imaging and long-slit spectroscopy. Strategic instruments under development for the remaining two combined focal stations include an interferometric cryogenic beam combiner with near-infrared and thermal-infrared instruments for Fizeau imaging and nulling interferometry (LBTI) and an optical bench beam combiner with visible and near-infrared imagers utilizing multi-conjugate adaptive optics for high angular resolution and sensitivity (LINC/NIRVANA). In addition, a fiber-fed bench spectrograph (PEPSI) capable of ultra high resolution spectroscopy and spectropolarimetry (R = 40,000-300,000) will be available as a principal investigator instrument. The availability of all these instruments mounted simultaneously on the LBT permits unique science, flexible scheduling, and improved operational support.

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Optical Imaging

Select this Article		A smart fast camera Roberto Ragazzoni, Carmelo Arcidiacono, Emiliano Diolaiti, Jacopo Farinato, Anna M. Moore, and Roberto Soci Proc. SPIE 5492, 121 (2004); http://dx.doi.org/10.1117/12.552035 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract It is generally believed that very fast cameras imaging large Fields of View translate into huge optomechanics and mosaics of very large contiguous CCDs. It has already been suggested that seeing limited imaging cameras for telescopes whose diameters are larger than 20m are considered virtually impossible for a reasonable cost. We show here that, using existing technology and at a moderate price, one can build a Smart Fast Camera, a device that placed on aberrated Field of View, including those of slow focal ratios, is able to provide imaging at an equivalent focal ratio as low as F/1, with a size that is identical to the large focal ratio focal plane size. The design allows for easy correction of aberrations over the Field of View. It has low weight and size with respect to any focal reducer or prime focus station of the same performance. It can be applied to existing 8m-class telescopes to provide a wide field fast focal plane or to achieve seeing-limited imaging on Extremely Large Telescopes. As it offers inherently fast read-out in a massive parallel mode, the SFC can be used as a pupil or focal plane camera for pupil-plane or Shack-Hartmann wavefront sensing for 30-100m class telescopes.

Select this Article		High-resolution imaging in the visible from the ground without adaptive optics: new techniques and results Craig D. Mackay, John Baldwin, Nicholas Law, and Peter Warner Proc. SPIE 5492, 128 (2004); http://dx.doi.org/10.1117/12.550443 \| Cited 7 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Many astronomical imaging studies, such as those of weak gravitational lensing, call for better angular resolution than is normally possible from the ground over wide fields of view . For many of these studies astronomers need images which show a consistent point spread function across the field even if this comes at the expense of the ultimate in angular resolution at the centre of the field. Adaptive Optics does not show any prospect of being able to achieve fields of view as large as are needed at visible wavelengths and therefore a new technique of delivering high resolution images from the ground must be developed. Electron multiplying CCDs are available that allow images to be taken at high speed without the usual penalty of read noise. We have developed a new technique called Lucky Imaging which achieves high resolution by selecting the better images from a sequence of images, then shifting and adding each to give a much higher resolution output image. Resolutions in the range 0.1-0.2 arc seconds can be obtained routinely under relatively good conditions on a 2.5 metre telescope working in I band (850 nanometres) and using as much as 30% of the images taken. Even under poorer conditions we find that image selection allows the final resolution to be better than the traditional seeing value by a factor of as much as three. This paper describes the technique and some of the results obtained using this method.

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Optical Spectroscopy I

Select this Article		Performance of FLAMES at the VLT: one year of operation Luca Pasquini, Roberto Castillo, Hans Dekker, Reinhard Hanuschik, Andreas Kaufer, Andrea Modigliani, Ralf Palsa, Francesca Primas, Riccardo Scarpa, Jonathan Smoker, and Burkhard Wolff Proc. SPIE 5492, 136 (2004); http://dx.doi.org/10.1117/12.550437 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Four years after its announcement at SPIE, FLAMES, the VLT fibre facility, has been completed, integrated into the VLT observatory and commissioned. It has been in operation since February 2003. More than 250000 scientific (single) spectra have been obtained, which have enabled the on-sky performance of the instrument to be compared to the predictions. We show that in several relevant aspects the real instrument significantly outperforms the specified astronomical performance. Some of the early scientific results are finally presented.

Select this Article		The exoplanet hunter HARPS: performance and first results Gero Rupprecht, Francesco Pepe, Michel Mayor, Didier Queloz, Francois Bouchy, Gerardo Avila, Willy Benz, Jean-Loup Bertaux, X. Bonfils, Th. Dall, Bernard Delabre, Hans Dekker, Wolfgang Eckert, Michel Fleury, Alain Gilliotte, et al. Proc. SPIE 5492, 148 (2004); http://dx.doi.org/10.1117/12.551267 \| Cited 6 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract HARPS is a new high resolution fibre-fed spectrograph dedicated to theextremely precise measurement of stellar radial velocities. After being used for about one year including the commissioning runs we report a very successful implementation of the measures taken to maximise stability, efficiency and spectral performance. Using the Simultaneous ThAr Reference Method a short term precision of 0.2 m/s during one night and a long term precision of the order of 1 m/s have been achieved. Equipped with a fully automated data reduction pipeline that produces solar system barycentric radial velocities in near real-time, HARPS promises to deliver data of unequalled quality. HARPS will primarily be used for the search for exoplanets and in the field of asteroseismology. First exciting scientific results confirm these expectations.

Select this Article		bHROS installation and system performance Margaret E. Aderin Proc. SPIE 5492, 160 (2004); http://dx.doi.org/10.1117/12.550960 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Gemini bHROS instrument, (Bench-Mounted High Resolution Optical Spectrograph) was delivered to the Gemini South Telescope in March 2003, after passing it's onsite acceptance test at UCL (University College London). The instrument was installed through the 2003 period, getting its final components, the fibre system, in September of that year. A number of nights were then allocated to the instrument to verify it throughput.This paper discusses the installation of the bHROS system in the pier lab and the difficulties encountered getting an accurate measure of the throughput of the system. An overview of the measured performance of the instrument and details of additional, proposed, system enhancements is given and an indication of the timescales for its release to the astronomical community is discussed.

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Optical Spectroscopy II

Select this Article		First science observations with the ACES echelle spectrograph Robert O. Reynolds and Michael Lloyd-Hart Proc. SPIE 5492, 172 (2004); http://dx.doi.org/10.1117/12.552334 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The use of spectrographs with telescopes having high order adaptive optics (AO) systems offers the possibility of achieving near diffraction-limited spectral resolution with ground-based telescopes, as well as important advantages for instrument design. The use of an optical fiber to couple the instrument to the telescope affords additional advantages such as flexibility in the placement of the instrument and improved homogeneity of the input illumination function. In the case of Steward Observatory's Adaptively Coupled Echelle Spectrograph (ACES), the instrument is normally coupled to the telescope with an 8 micron diameter near single-mode optical fiber, although the instrument can be used at fixed focus locations without the fiber for telescopes so equipped. The use of a fiber coupler results in the phenomenon known as 'modal noise', where the transmission of multiple modes in the fiber leads to a wavelength-dependent variation in illumination that limits flat fielding precision. We have largely eliminated this effect through the use of an automated fiber stretcher device. We report here on improvements to the fiber feed optics and on interim observations made with the instrument at a conventional telescope not equipped with adaptive optics.

Select this Article		Scientific and technical performance of GMOS: the Gemini Multi-Object Spectrograph David Crampton and Richard Murowinski Proc. SPIE 5492, 181 (2004); http://dx.doi.org/10.1117/12.550950 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract GMOS is the first telescope - spectrograph combination that acts as a complete system to deliver enhanced image quality and stability while simultaneously exploiting the large aperture of an 8m telescope. The entire system (optics, mechanics, software, detectors) was designed to take advantage of the best images that the Gemini telescopes produce while being extremely reliable and efficient. The built-in wavefront sensor allows the telescope to quickly point at an object, optimize its focus and then track it precisely for many hours (possibly over several nights) while maintaining perfect telescope and instrument focus and providing first order image compensation. As a result of the carefully-engineered design of its structure and mechanisms and its active flexure control system, GMOS offers unique scientific opportunities. A recent enhancement was the implementation of the "nod and shuffle" technique to give improved sky subtraction for very faint object spectroscopy. Some of the scientific highlights of GMOS' many modes (Imaging, MOS, IFU, precision velocities) are reviewed, and some of the "lessons-learned" during the first few years of operation are described.

Select this Article		Interferometric resolution boosting for spectrographs David J. Erskine and Jerry Edelstein Proc. SPIE 5492, 190 (2004); http://dx.doi.org/10.1117/12.549947 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Externally dispersed interferometry (EDI) is a technique for enhancing the performance of spectrographs for wide bandwidth high resolution spectroscopy and Doppler radial velocimetry. By placing a small angle-independent interferometer near the slit of a spectrograph, periodic fiducials are embedded on the recorded spectrum. The multiplication of the stellar spectrum times the sinusoidal fiducial net creates a moire pattern, which manifests high detailed spectral information heterodyned down to detectably low spatial frequencies. The latter can more accurately survive the blurring, distortions and CCD Nyquist limitations of the spectrograph. Hence lower resolution spectrographs can be used to perform high resolution spectroscopy and radial velocimetry. Previous demonstrations of ~2.5x resolution boost used an interferometer having a single fixed delay. We report new data indicating ~6x Gaussian resolution boost (140,000 from a spectrograph with 25,000 native resolving power), taken by using multiple exposures at widely different interferometer delays.

Select this Article		RITMOS: a micromirror-based multi-object spectrometer Reed D. Meyer, Kevin J. Kearney, Zoran Ninkov, Christopher T. Cotton, Peter Hammond, and Bryan D. Statt Proc. SPIE 5492, 200 (2004); http://dx.doi.org/10.1117/12.549897 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Rochester Institute of Technology Multi-Object Spectrometer (RITMOS) utilizes a Texas Instruments Digital Micromirror Device (DMD) for target selection, instead of the fiber bundles or customized slit masks normally used in multi-object spectroscopy. The DMD, which sits at the telescope focal plane, is an 848 x 600 array of 17 micron square mirrors that can individually deflect incident light into one of two output paths: an imaging path or a spectroscopy path. In standard operation, all light is deflected towards the imaging path, consisting of an Offner relay which reimages the DMD onto a CCD detector. The locations of spectroscopic targets are then noted, and the micromirrors corresponding to these targets are then deflected towards the spectroscopy path. This path utilizes a 1200 l/mm transmission grating to disperse images of the micromirror pattern onto a second CCD detector. The spectroscopic parameters (e.g., 0.66 Å/pixel dispersion for a 13.5 micron/pixel detector) were chosen for MK spectral classification. Among the benefits of replacing a fiber bundle or custom slit mask with a DMD are the latter's instantaneous reconfigurability and its aptitude for the study of compact fields. RITMOS is thus suited towards spectral classification surveys of star clusters. We present a description of the instrument, details of its design, and initial measurements, including multi-object stellar spectra.

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Optical Spectroscopy III

Select this Article		X-shooter: UV-to-IR intermediate-resolution high-efficiency spectrograph for the ESO VLT Sandro D'Odorico, Michael I. Andersen, Paolo Conconi, Vincenzo De Caprio, Bernard Delabre, Paolo Di Marcantonio, Hans Dekker, Mark D. Downing, Gert Finger, Paul Groot, Hiddo H. Hanenburg, Francois Hammer, David Horville, Jens Hjorth, Lex Kaper, et al. Proc. SPIE 5492, 220 (2004); http://dx.doi.org/10.1117/12.550005 \| Cited 4 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract X-shooter is a single target spectrograph for the Cassegrain focus of one of the VLT UTs. It covers in a single exposure the spectral range from the UV to the H band with a possible extension into part of the K band. It is designed to maximize the sensitivity in this spectral range through the splitting in three arms with optimized optics, coatings, dispersive elements and detectors. It operates at intermediate resolutions (R=4000-14000, depending on wavelength and slit width) sufficient to address quantitatively a vast number of astrophysical applications while working in a background-limited S/N regime in the regions of the spectrum free from strong atmospheric emission and absorption lines. The small number of moving functions (and therefore instrument modes) and fixed spectral format make it easy to operate and permit a fast response. A mini-IFU unit (1.8" x 4") can be inserted in the telescope focal plane and is reformatted in a slit of 0.6"x 12" .The instrument includes atmospheric dispersion correctors in the UV and visual arms. The project foresees the development of a fully automatic data reduction package. The name of the instrument has been inspired by its capability to observe in a single shot a source of unknown flux distribution and redshift. The instrument is being built by a Consortium of Institutes from Denmark, France, Italy and the Netherlands in collaboration with ESO. When it operation, its observing capability will be unique at very large telescopes.

Select this Article		Status of Elmer: a multipurpose instrument for the GTC 10-m telescope Maria Luisa Garcia-Vargas, Peter L. Hammersley, Ernesto Sanchez-Blanco, Ralf Kohley, Juan Manuel Martin Fleitas, Lluis Cavaller-Marques, Manuel Maldonado Medina, and Rafael Vilela Proc. SPIE 5492, 230 (2004); http://dx.doi.org/10.1117/12.550074 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract ELMER is an instrument for the GTC designed to observe between 365 and 1000 nm. The observing modes for the instrument at Day One shall be: Imaging, Long Slit and Mask-Multi-object Spectroscopy, Slit-less multi-object spectroscopy, Fast Photometry and Fast short-slit spectroscopy, over a FOV of 4.2 arcmin diameter. Spectral resolutions of 250, 1000 and 2500, covering the whole spectral range, will be available. ELMER has been designed and managed within the GTC Project Office. ELMER is currently in the final stage of testing previous to be shipped to the Observatory. The general description of this instrument and its expected scientific performance are summarised.

Select this Article		Honeycomb: a concept for a programmable integral field spectrograph Joss Bland-Hawthorn, Andrew J. McGrath, Will Saunders, Roger Haynes, and Peter Gillingham Proc. SPIE 5492, 242 (2004); http://dx.doi.org/10.1117/12.550291 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract An unsolved problem in astronomical instrumentation is an imaging integral field spectrograph where the user has the freedom to specify arbitrarily complex, contiguous or disjoint regions over the focal plane, rather than a contiguous rectangular field. We present a new concept to solve this problem. Our device allows the user to format the field of view with fibre bundles packed into arbitrary patterns. The field of view is segmented by a large N(N microlens array (e.g. N=1000). This element divides the wavefront into small beams which pass through a metal plate drilled with a grid of holes in the same format as the microlens array. On the reverse side of the grid, hexagonal blocks comprising 67 input fibres are plugged into position on the grid with a pair of sliding "croupier" sticks. The fibred blocks transport the light to the spectrograph. The blocks are held magnetically and the plugging ensures accurate and repeatable registration with respect to the microlens array. The grid plate is micromachined with baffled holes in order to ensure photometric uniformity over the field of view.

Select this Article		VIRUS: a massively replicated IFU spectrograph for HET Gary J. Hill, Phillip J. MacQueen, Carlos Tejada, Francisco J. Cobos, Povilas Palunas, Karl Gebhardt, and Niv Drory Proc. SPIE 5492, 251 (2004); http://dx.doi.org/10.1117/12.552474 \| Cited 4 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We investigate the role of industrial replication in the construction of the next generation of spectrographs for large telescopes. In this paradigm, a simple base spectrograph unit is replicated to provide multiplex advantage, while the engineering costs are amortized over many copies. We argue that this is a cost-effective approach when compared to traditional spectrograph design, where each instrument is essentially a one-off prototype with heavy expenditure on engineering effort. As an example of massive replication, we present the design of, and the science drivers for, the Visible IFU Replicable Ultra-cheap Spectrograph (VIRUS). This instrument is made up of 132 individually small and simple spectrographs, each fed by a fiber integral field unit. The total VIRUS-132 instrument covers ~29 sq. arcminutes per observation, providing integral field spectroscopy from 340 to 570 nm, simultaneously, of 32,604 spatial elements, each 1 sq. arcsecond on the sky. VIRUS-132 will be mounted on the 9.2 m Hobby-Eberly Telescope and fed by a new wide-field corrector with a science field in excess of 16.5 arcminutes diameter. 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 >102 spectrographs making up a whole.

Select this Article		WiFeS: the wide field spectrograph Michael A. Dopita, Liam E. Waldron, Peter McGregor, Peter Conroy, Matthew C. Doolan, Ross Zhelem, Gabe Bloxham, Will Saunders, Damien Jones, and Lee Pfitzner Proc. SPIE 5492, 262 (2004); http://dx.doi.org/10.1117/12.541264 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract WiFeS is a powerful integral field, double-beam, concentric, image-slicing spectrograph designed to deliver excellent thoughput, precision spectrophotometric performance and superb image quality along with wide spectral coverage throughout the 320-1000 nm wavelength region. It is currently under construction at the Research School of Astronomy and Astrophysics of the Australian National University (ANU), and will be mounted on the ANU 2.3m telescope at Siding Spring Observatory. It will provide a 25x31 arc sec field with 0.5 arc sec sampling along each of twenty five 31x1.0 arc sec slitlets. The output format is arranged to match the 4096x4096 pixel CCD detectors in each of two cameras individually optimized for the blue and the red ends of the spectrum, respectively. A process of "interleaved nod-and-shuffle" will be applied to permit quantum noise-limited sky subtraction. Using VPH gratings, spectral resolutions modes of 3000 and 7000 will be provided. The full spectral range is covered in a single exposure in the R=3000 mode, and in two exposures in the R=7000 mode. The use of transmissive coated optics, VPH gratings and optimized mirror coatings ensures a throughput (including telescope and atmosphere) that peaks above 30%. The concentric image-slicer design ensures an excellent and uniform image quality across the full field. To maximize the scientific return, the whole instrument is configured for remote observing, pipeline data reduction, and the accumulation of calibration image libraries.

Select this Article		High-contrast differential-aberration-free 3D spectrometer for the Planet Finder instrument Eric Prieto, Michel Saisse, Pascale Hibon, Jean-Luc Beuzit, and Anne-Marie Lagrange Proc. SPIE 5492, 271 (2004); http://dx.doi.org/10.1117/12.550575 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We will present a design of a high contrast 3D spectrometer with the attractive characteristics to provide very low differential aberrations. This concept, very well suited for an instrument as planet finder, is based on our expertise in slicer unit. Thanks to a control of diffraction and roughness effect, this new concept will provide spectrograph entrance sub-slit with a high purity. Very low level of cross-talk signal is expected. Associated with the slicer unit, we will present a spectrograph concept allowing to guaranty a negligible level of differential aberration between wavelength in the spectrum.

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Poster Presentations: Optical Instrumentation I

Select this Article		Large-field reflective integral field systems for visible and infrared spectroscopy Robert Content, Cornelis M. Dubbeldam, David J. Robertson, Ray M. Sharples, and Simon L. Morris Proc. SPIE 5492, 281 (2004); http://dx.doi.org/10.1117/12.552022 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Optical designs of fore-optics and Advanced Image Slicer (AIS) systems made for the second generation VLT instruments KMOS1 and MUSE2,3 conceptual design studies are presented. KMOS is an infrared multi-integral-field spectrograph with 24 fields, each 2.8" x 2.8" with a 0.2" resolution, patrolling a 7' field. The described optics of KMOS are the fore-optics, from the images given by the pickoff system to the slicers, and the slicer systems themselves. The study also includes a derotator design in case the instrument would have been too heavy to be attached to the telescope. MUSE is an integral field spectrograph for the 0.465 m to 1 m bandwidth with a 1' x 1' field and a resolution of 0.2". Two optical designs were proposed, one mostly transmissive which is now the baseline, the other mostly using reflective optics. The later is described in this paper. It includes a derotator, an atmospheric dispersion corrector, a transmissive removable magnifier, a transmissive field splitter that cut the field in 24 subfields, the relay optics of each subfield to each slicer and the slicer systems. While MUSE is for the visible and would then in principle need transmissive optics, the use of reflective optics is justified because its minimum wavelength is 0.465 m; modern reflective coatings give transmission larger than 98% for these wavelengths. We discuss the development of the manufacturing of AIS to extend its application to the visible from its actual use in the IR.

Select this Article		Optical design of PANORAMIX-II, the OMM wide-field VIS-NIR camera Simon Thibault, Michel Doucet, and Laurent Drissen Proc. SPIE 5492, 293 (2004); http://dx.doi.org/10.1117/12.552936 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract In this paper, we present the optical design of the optical train of Panoramix-II, a wide-field VIS-NIR camera to be installed at the cassegrain focus of OMM (Observatoire du Mont Megnantic, Quebec, Canada). This camera is optimized for g (0.41-0.55), r (0.556-0.689), i (0.693-0.867) and z (0.851-0.95) operating region and used a 2kX4k EEV detector. The sky will be imaged onto the focal plane at an optical speed of F/2.35 yielding an image scale of 0.75 arcsecond per 13.5 μm pixel. The design image quality is 0.75 arcsecond 50% diffraction encircled energy over the central 27 arcmin field and no images worse than 0.85 arcsecond over the 55 arcminute diameter camera field. The optical design distortion at the corners is less than 0.08%. The Panoramix-II camera have a set of filters is used at the internal pupil. The image of the pupil is sufficiently sharp to limit the filter size. We discuss the principle characteristics of the imager, the specifications, the optical design, the performances, a ghost study and finally a tolerance anlaysis.

Select this Article		FALCON: extending adaptive optics corrections to cosmological fields Mathieu Puech and Frederic Sayede Proc. SPIE 5492, 303 (2004); http://dx.doi.org/10.1117/12.549805 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract FALCON (a Fiber spectrograph with Adaptive optics on Large fields to correct at Optical and Near-infrared) is an original concept for a next generation instrumentation at ESO VLT or at future ELTs. It is a multi-objects integral field spectrograph with multiple integral field small units, each being coupled with atmospheric tomography in order to reach spatial and spectral resolution ideally suited for distant galaxy studies: typically 0.15 - 0.25 arcsec and R>=5000 in the 0.8-1.8 μm wavelength range. In the FALCON concept the adaptive optics correction is only applied on small and discrete areas selected on a large field. This approach implies to develop some miniaturized devices for adaptive optics correction and wavefront sensing. We present here some recent technological results.

Select this Article		Manufacturing, integration, and testing of ELMER structure and mechanisms Bernardo Ronquillo, Miguel A. Vega, Miquel Ona, Ester Porras, Ignacio Mayor, David Roy, Sergio Camps, Francisco J. Pereda, Maria Luisa Garcia-Vargas, Manuel Maldonado Medina, Juan Manuel Martin Fleitas, and Ernesto Sanchez Proc. SPIE 5492, 312 (2004); http://dx.doi.org/10.1117/12.549816 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract ELMER is an optical instrument for the GTC designed to observe between 3650 and 10000 Armstrong. The observing modes for the instrument at Day One shall be: Imaging, Long Slit Spectroscopy, Mask-multi-object spectroscopy, Slit-less multi-object spectroscopy, Fast Photometry and Fast short-slit spectroscopy. It will be installed at the Nasmyth-B focal station at Day One, but it will also be designed to operate at the Folded Cassegrain focal station. The physical configuration of the instrument consists of a front section where the focal plane components are mounted (Slit Unit) and a rear section with the rest of the components (Field Lens, Prism/Grism/VPH Wheel, Filter Wheel, Collimator, Camera, Folder Mirrors, Shutter and Cryostat with the detector). Both sections are connected through a hexapod type structure. The optical path is bent twice with the two folder mirrors providing a compact system.The design phase of the ELMER Structure and Mechanisms finished on November 2002. Procurement and manufacturing covered from December 2002 to June 2003. Mechanical and electrical integration was accomplished on September 2003. Test campaign at factory covered from the end of September to mid November. Critical performance of the mechanics has been carefully tested during this period: positional tolerances of optical interfaces, repeatability of the 5 mechanisms (4 rotating wheels and collimator linear stage) and deflections of the instrument due to gravity. Results from the tests are widely within the specified values, providing a top performance instrument.

Select this Article		HERMES: a high-resolution spectrograph for the Mercator Telescope Gert Raskin, Hans Van Winckel, and Geert Davignon Proc. SPIE 5492, 322 (2004); http://dx.doi.org/10.1117/12.549883 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Hermes, a high-resolution fiber-fed echelle spectrograph is currently under development for the 1.2-meter Mercator Telescope at the Roque De Los Muchachos Observatory on La Palma. The optical design is based on a large R2.6 echelle grating, operating in quasi-Littrow and white-pupil configuration, and a double-prism cross-disperser. This instrument records the complete optical spectrum from 380 to 875 nm in one single exposure on a 2k x 4k CCD. Order separation is sufficiently large to record two interleaved spectra simultaneously through two 60-mm core fibers: one spectrum of the object and one of the nearby sky or, alternatively, of a wavelength calibration lamp for high-precision radial velocity measurements. This type of observations also benefits from the high instrumental stability, owing to bench-mounting the spectrograph with a fixed configuration in a precisely temperature and humidity controlled chamber. Modest telescope size calls for high detection efficiency and great efforts in the design of both the fiber link and the spectrograph itself go in that direction. We aim at a peak-efficiency larger than 25% for the complete system. With a large fiber aperture of 2.3 arcsec, the resolving powerλ/ΔλΑ is 50000, a value that can be increased to 90000 with an adjustable slit at the fiber exit. This instrument mounted on a flexible telescope has a wide astronomical scope, going from asteroseismology to binary star research and chemical studies of stars and circumstellar material. We present the spectrograph design and we report on the project status.

Select this Article		The Goodman spectrograph J. Christopher Clemens, J. Adam Crain, and Robert Anderson Proc. SPIE 5492, 331 (2004); http://dx.doi.org/10.1117/12.550069 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Goodman Spectrograph is an imaging, multi-object spectrograph for the SOuthern Astrophysical Research telescope (SOAR). It is one of the first designed to take advantage of Volume Phase Holographic (VPH) gratings by employing an articulated camera. This aspect of the mechanical design has had complicating effects on a number of usually simple systems, and has led to some unorthodox solutions. The spectrograph is also highly optimized for efficiency from 320 to 850 nm, and designed for rapid configuration changes, so that its throughput makes it competitive with instruments on larger telescopes. We present the high level requirements that have driven the mechanical and electronic systems, and show their implementation in the completed instrument. It is too early to assess the overall system performance, but tests of the modular subsystems show promising results. We discuss the expected overall performance and discuss mitigation strategies should that performance fall short of our goals.

Select this Article		Testing the optics of the instrument ELMER for the GTC 10-m telescope Ernesto Sanchez-Blanco and Maria Luisa Garcia-Vargas Proc. SPIE 5492, 341 (2004); http://dx.doi.org/10.1117/12.550081 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract ELMER is a visible imager and spectrograph for the GTC. ELMER is currently in the final stage of testing (at the PO in La Laguna, Tenerife) previous to be shipped to the Observatorio del Roque de los Muchachos in the island of La Palma, where the GTC telescope is being integrated. ELMER Optics has been exhaustively tested at different steps, from the blanks to the final assemblies in order to guarantee the required performance. In this contribution, we will describe the tests done to the different optical components until now. Blank testing, WFE Image quality and transmission tests have been carried out for most of the components. A brief review of some of these tests is included in the following sections as well as a list of references where the test assemblies and the results are discussed in detail.

Select this Article		Ukidna: the RAVE machine Andrew J. McGrath, Will Saunders, Fred Watson, and Stan Miziarski Proc. SPIE 5492, 353 (2004); http://dx.doi.org/10.1117/12.550284 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Anglo-Australian Observatory is currently designing a new fibre positioner for the UK Schmidt Telescope. The instrument will have 2250 fibres, positioned with sub-arcsecond accuracy across a six degree field of view, and will have a reconfiguration time of one minute. The instrument is to enable the RAVE survey of high precision abundances and velocities for up to 50 million stars. The design is largely adapted from the AAO's FMOS-Echidna fibre positioner for Subaru. New design challenges for Ukidna include the enormous number of fibres, the large focal surface, and the field curvature of the Schmidt telescope. These features are mostly shared with the expected needs of future prime-focus multi-fibre systems on 8-30m class telescopes. We present details and performance of the multi-actuator design.

Select this Article		KAOS: kilo-aperture optical spectrograph Samuel C. Barden, Arjun Dey, Brian Boyle, and Karl Glazebrook Proc. SPIE 5492, 364 (2004); http://dx.doi.org/10.1117/12.550287 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A design is described for a potential new facility capable of taking detailed spectroscopy of millions of objects in the Universe to explore the complexity of the Universe and to answer fundamental questions relating to the equation of state of dark energy and to how the Milky Way galaxy formed. The specific design described is envisioned for implementation on the Gemini 8-meter telescopes. It utilizes a 1.5° field of view and samples that field with up to ~5000 apertures. This Kilo-Aperture Optical Spectrograph (KAOS) is mounted at prime focus with a 4-element corrector, atmospheric dispersion compensator (ADC), and an Echidna-style fiber optic positioner. The ADC doubles as a wobble plate, allowing fast guiding that cancels out the wind buffeting of the telescope. The fibers, which can be reconfigured in less than 10 minutes, feed to an array of 12 spectrographs located in the pier of the telescope. The spectrographs are capable of provided spectral resolving powers of a few thousand up to about 40,000.

Select this Article		Optical design of CAOS: a high-resolution spectropolarimeter for the Catania Astrophysical Observatory 0.91-m telescope Paolo Spano, F. Leone, Salvatore Scuderi, Santo Catalano, and Filippo M. Zerbi Proc. SPIE 5492, 373 (2004); http://dx.doi.org/10.1117/12.550344 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract CAOS (Catania Astrophysical Observatory Spectrograph) is a high-resolution (R~60,000), fiber fed, bench-mounted, prism cross-dispersed, white-pupil R-4 echelle spectrograph with polarimetric capabilities, for the 0.91m telescope on Mt. Etna. Wavelengths from 390 to 710 nm are covered in one-shot with a 2Kx2K 13.5 micron CCD. Inherent high efficiency of the spectrograph and optimum matching between fibers and spectrograph will allow high throughput for the overall system. This instrument will replace the existing spectrograph, with a net gain in spectral resolution (about a factor 2) and in efficiency (about a factor 10), extending current studies undertaken by Catania Astrophysical Observatory in stellar physics.

Select this Article		Optical design of the PEPSI high-resolution spectrograph at LBT Michael I. Andersen, Paolo Spano, Manfred Woche, Klaus G. Strassmeier, and Erik Beckert Proc. SPIE 5492, 381 (2004); http://dx.doi.org/10.1117/12.550533 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract PEPSI is a high-resolution, fiber fed echelle spectrograph with polarimetric capabilities for the LBT. In order to reach a maximum resolution R=120.000 in polarimetric mode and 300.000 in integral light mode with high efficiency in the spectral range 390-1050~nm, we designed a white-pupil configuration with Maksutov collimators. Light is dispersed by an R4 31.6 lines/mm monolithic echelle grating mosaic and split into two arms through dichroics. The two arms, optimized for the spectral range 390-550~nm and 550-1050~nm, respectively, consist of Maksutov transfer collimators, VPH-grism cross dispersers, optimized dioptric cameras and 7.5K x 7.5K 8~μ CCDs. Fibers of different core sizes coupled to different image-slicers allow a high throughput, comparable to that of direct feed instruments. The optical configuration with only spherical and cylindrical surfaces, except for one aspherical surface in each camera, reduces costs and guarantees high optical quality. PEPSI is under construction at AIP with first light expected in 2006.

Select this Article		AAOmega: a scientific and optical overview Will Saunders, Terry Bridges, Peter Gillingham, Roger Haynes, Greg A. Smith, John D. Whittard, Vladimir Churilov, Allan Lankshear, Scott Croom, Damien Jones, and Christopher Boshuizen Proc. SPIE 5492, 389 (2004); http://dx.doi.org/10.1117/12.550871 \| Cited 8 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract AAOmega is a new spectrograph for the existing 2dF and SPIRAL multifibre systems on the Ango-Australian Telescope. It is a bench-mounted, dual-beamed, articulating, all-Schmidt design, using volume phase holographic gratings. The wavelength range is 370-950nm, with spectral resolutions from 1400-10000. Throughput, spectral coverage, and maximum resolution are all more than doubled compared with the existing 2dF spectrographs, and stability is increased by orders of magnitude. These features allow entirely new classes of observation to be undertaken, as well as dramatically improving existing ones. AAOmega is scheduled for delivery and commissioning in Semester 2005B.

Select this Article		High-resolution spectrograph with R4 echelle for LAMOST Yongtian Zhu, Xuhua Wu, Lei Wang, and Qiufeng Luo Proc. SPIE 5492, 401 (2004); http://dx.doi.org/10.1117/12.551012 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A preliminary design study for a high-resolution echelle spectrograph to be used for LAMOST (The large Sky Area Multi-Object Fiber Spectroscopic Telescope) that is currently under construction is presented. In order to obtain a resolution-slit product of about 40000 as required by science case, the less expensive design used a 105mm beam feeding a 408mm deep Echelle is good solution.The optical design of high resolution Echelle spectrograph for LAMOST is given. This spectrograph will be more powerful tool for astrophysical research using high-resolution spectroscopy in China. Some new technology and novel design concepts have been adopted in this spectrograph, such as white pupil collimator system, R4 Echelle with large blaze angle, and the fold and off-axial Schimidt camera without center obstruction and so on.

Select this Article		AAOmega: a multipurpose fiber-fed spectrograph for the AAT Greg A. Smith, Will Saunders, Terry Bridges, Vladimir Churilov, Allan Lankshear, John Dawson, David Correll, Lew Waller, Roger Haynes, and Gabriella Frost Proc. SPIE 5492, 410 (2004); http://dx.doi.org/10.1117/12.551013 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The AAOmega project replaces the two 2dF spectrographs, which are mounted on the top end of the Anglo Australian Telescope, with a bench mounted double beam spectrograph covering 370 to 950nm. The 2dF positioner, field plate tumbler mechanism, and fiber retractors will be retained. The new spectrograph will be fed by 392 fibers from either of the two 2dF field plates, or by the 512 fiber Spiral integral field unit, located at the Cassegrain focus. New instrument control electronics has also been designed to drive the spectrograph.Stability will be improved by locating the spectrograph off the telescope, but the 2df fibers must be extended to thirty-eight metres length. Despite this, using fibers with improved characteristics, increased pupil diameter, volume phase holographic (VPH) gratings with articulated cameras, and more efficient coatings on optics we achieve a minimum twofold increase in throughput. We will also fit larger (4k x 2k pixel) detectors. The spectrograph comprises: a F/3.15 Schmidt collimator, incorporating a dichroic beamsplitter; interchangeable VPH gratings; and articulating red and blue F/1.3 Schmidt cameras. The beamsplitter may be exchanged with others which cut off at different wavelengths. A full suite of VPH gratings are provided to cover resolution to 8000.

Select this Article		Optical wavelength image slicer Matthew C. Doolan, Michael A. Dopita, Liam E. Waldron, John Hart, Ross Zhelem, Gabe Bloxham, Peter Conroy, Peter McGregor, and Leigh Pfitzner Proc. SPIE 5492, 421 (2004); http://dx.doi.org/10.1117/12.551045 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Wide Field Spectrograph (WiFeS) is a high-throughput double-beamimage-slicing spectrograph that will operate over the visiblewavelength range 320nm to 1000nm. Designed by the Australian NationalUniversity's Research School of Astronomy and Astrophysics (RSAA) atMount Stromlo, WiFeS is based on an Integral Field Unit (IFU) andVolume Phased Holographic (VPH) grating technology.Central to the IFU design is a visible wavelength imageslicer. Traditionally, such a slicer has been difficult to realise,due to the requisite high surface quality demanded to reduce scatterfrom each slice.In this paper, we discuss both the novel design and manufacture of theWiFeS slicer assembly. Preliminary results are presented that clearlydemonstrate the effectiveness of the design.

Select this Article		Optomechanical design of the MUSE spectrograph structure Ian J. Lewis, James Lynn, Stephanie Yang, Wing Lau, and Roger L. Davies Proc. SPIE 5492, 429 (2004); http://dx.doi.org/10.1117/12.551392 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We describe some of the design work behind the structural design of the MUSE spectrograph for the VLT. In particular we consider the limitations on the instrument layout and the effect of its mechanical and thermal properties on the overall instrument performance.

Select this Article		A new concept for echelle spectrographs: the SOAR Telescope Echelle Spectrograph Bruno V. Castilho, Bernard Delabre, and Clemens D. Gneiding Proc. SPIE 5492, 433 (2004); http://dx.doi.org/10.1117/12.551733 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present the design of the SOAR Telescope Echelle Spectrograph (STELES). The instrument is part of the Brazilian participation on the 4.1m SOAR telescope second-generation instrumentation. A multi-institutional team is designing the echelle spectrograph with UV capability. In view of its high image quality and moderately large collecting area, SOAR will be able to yield high quality spectroscopic data for a large variety of objects of astrophysical interests. Another point that should be explored in SOAR is the near UV capability, not available in most of the current available high-resolution spectrographs. The proposed spectrograph is a R4 cross-dispersed echelle fed by the SOAR Nasmyth focus, operating in a quasi-Littrow white pupil configuration, and a resolving power of R ~ 50,000, covering the 300-890nm spectral range in one shot.The concept developed for this spectrograph is based on VPH grating crossdispersers and all spherical optics (including the collimator mirrors). The transfer collimator is mounted in a position so that the 100mm F/8.5 beam is resized to 50mm, allowing very compact cameras design. These modifications on the standard quasi-Littrow, white pupil configuration design yield a very efficient, compact and cheaper spectrograph.

Select this Article		Results from upgrades to the radial velocity instrument, ET, at the KPNO 2.1 m Julian C. van Eyken, Jian Ge, Suvrath Mahadevan, Curtis DeWitt, Jerry Friedman, Padraic Finnerty, Deqing Ren, and Mike Zugger Proc. SPIE 5492, 445 (2004); http://dx.doi.org/10.1117/12.551889 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A radial velocity (RV) survey instrument, Exoplanet Tracker (ET), has been commissioned at the Kitt Peak 2.1m telescope. It is a fiber-fed,fixed-delay Michelson interferometer followed by a medium resolution volume phase holographic spectrograph (operating at ~5000) for the visual band, and is planned to be opened to the public for RV related research in 2005. Since 2002 the measured total throughput of ET from above the atmosphere to the detector has been improved to about 18% (or 50% for the instrument itself from the fiber input to the detector), ~5 times higher than the current cross-dispersed echelle spectrometers for Doppler planet searches. We present new preliminary results from our improved version of ET, with 600 Angstrom wavelength coverage, showing RV measurements for HD 130322 (V=8.05), a known planet-bearing star, using 15 min exposures. A best short-term Doppler precision of 2.9 m/s has been achieved with this new instrument. We will start a pilot planet search of around 500 V=8--9 mag. stars with the 2.1m telescope in the Spring of 2005, and a multiple object RV feasibility study will also be conducted at the Sloan 2.5m wide field telescope in Spring 2005.

Select this Article		A multi-object double spectrograph for the Large Binocular Telescope Darren L. DePoy, Bruce Atwood, Stanley R. Belville, David F. Brewer, Paul L. Byard, Mark Derwent, Jennifer L. Marshall, Jerry A. Mason, C. Morgan, Thomas P. O'Brien, Patrick S. Osmer, Daniel P. Pappalardo, Richard W. Pogge, David P. Steinbrecher, Edward J. Teiga, et al. Proc. SPIE 5492, 452 (2004); http://dx.doi.org/10.1117/12.552275 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We are building a Multi-Object Double Spectrograph for the Large Binocular Telescope. The instrument is designed to have high throughput from 320 to 1000 nm, spectral resolutions of 1,000-10,000, and multi-object capability over a 6 arcminute field. The design incorporates a dichroic and splits the science beam into a blue and a red channel, each of which can illuminate an 8,192 pixel long detector (with 15 micron pixels) with good image quality. The highly modular design can hold up to three gratings and an imaging flat and a selection of filters in each channel, all of which are quickly accessible; this allows for substantial observing flexibility. Progress on the construction of the instrument and future plans will be described.

Select this Article		CHEOPS/ZIMPOL: a VLT instrument study for the polarimetric search of scattered light from extrasolar planets Daniel Gisler, Hans Martin Schmid, Christian Thalmann, Hans Peter Povel, Jan O. Stenflo, Franco Joos, Markus Feldt, Rainer Lenzen, Jaap Tinbergen, Raffaele Gratton, Remko Stuik, Daphne M. Stam, Wolfgang Brandner, Stefan Hippler, Massimo Turatto, et al. Proc. SPIE 5492, 463 (2004); http://dx.doi.org/10.1117/12.550366 \| Cited 14 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present results from a phase A study supported by ESO for a VLT instrument for the search and investigation of extrasolar planets.The envisaged CHEOPS (CHaracterizing Extrasolar planets by Opto-infrared Polarization and Spectroscopy) instrument consists of an extreme AO system, a spectroscopic integral field unit and an imaging polarimeter. This paper describes the conceptual design of the imaging polarimeter which is based on the ZIMPOL (Zurich IMaging POLarimeter) technique using a fast polarization modulator combined with a demodulating CCD camera. ZIMPOL is capable of detecting polarization signals on the order of p=0.001% as demonstrated in solar applications. We discuss the planned implementation of ZIMPOL within the CHEOPS instrument, in particular the design of the polarization modulator. Further we describe strategies to minimize the instrumental effects and to enhance the overall measuring efficiency in order to achieve the very demanding science goals.

Select this Article		CCD camera and data acquisition system of the scientific instrument ELMER for the GTC 10-m telescope Ralf Kohley, Juan Manuel Martin-Fleitas, Lluis Cavaller-Marques, Peter L. Hammersley, Marcos Suarez-Valles, Rafael Vilela, and Francis Beigbeder Proc. SPIE 5492, 475 (2004); http://dx.doi.org/10.1117/12.550415 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract ELMER is a multi-purpose instrument for the GTC designed for both, Imaging and Spectrosopy in the visible range. The CCD camera employs a E2V Technologies CCD44-82 detector mounted in a high performance LN2 Bath Cryostat based on an ESO design and a SDSU-II CCD controller with parallel interface. The design including the low-noise fan-out electronics has been kept flexible to allow alternatively the use of MIT/LL CCID-20 detectors. We present the design of the CCD camera and data acquisition system and first performance test results.

Select this Article		OmegaCAM: wide-field imaging with fine spatial resolution Konrad Kuijken, Ralf Bender, Enrico Cappellaro, Bernard Muschielok, Andrea Baruffolo, Enrico Cascone, H.-J. Hess, Olaf Iwert, Harald Nicklas, Klaus Reif, Edwin Valentijn, Dietrich Baade, K. G. Begeman, Alessandro Bortolussi, Danny Boxhoorn, et al. Proc. SPIE 5492, 484 (2004); http://dx.doi.org/10.1117/12.550892 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract OmegaCAM is the wide-field camera for the VLT Survey Telescope beingcompleted for ESO's Paranal observatory. The instrument, as well as the telescope, have been designed for very good, natural seeing-limited image quality over a 1 degree field. At the heart of the project are a square-foot photometric shutter, a 12-filter storage/exchange mechanism, a 16k x 16k CCD detector mosaic, and plenty of software for instrument control and data handling, analysis and archiving.

Select this Article		The OmegaCAM real-time image analysis system Konrad Kuijken, Andrea Baruffolo, Paolo Bagnara, and Carlo Magagna Proc. SPIE 5492, 494 (2004); http://dx.doi.org/10.1117/12.550920 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract OmegaCAM, the wide-field CCD camera for the VLT Survey Telescope, will have an on-line image analysis system, the design of which will be described here. Aim of the system is to provide continuous, real-time image aberration coefficients that can be used to correct the telescope primary mirror figure, and the secondary mirror position and attitude. Wavefront sensing is performed using a curvature-like system, which consists of two CCDs mounted out of focus (one in front, one behind focus) in the outer part of the focal plane. During observations short exposures of bright guide stars are continuously read out, the defocussed images are then decomposed into terms that correspond to wavefront aberrations. The optical design of the wavefront sensor, the image analysis algorithm and software, and system operations will be described.

Select this Article		Multiwavelength imaging concepts for exoplanet detection David Lafreniere, Rene Doyon, Rene Racine, Christian Marois, and Daniel Nadeau Proc. SPIE 5492, 500 (2004); http://dx.doi.org/10.1117/12.551798 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Direct exoplanet detections are currently limited by speckle noise arising from residual atmospheric wavefront errors and optical aberrations. Simultaneous spectral differential imaging (SSDI) is a high contrast imaging technique that aims at reducing this noise by the subtraction of images obtained simultaneously in adjacent narrow spectral bands. SSDI performances are severely degraded by differential optical aberrations between channels. We discuss two novel approaches to implement SSDI in which there are no differential aberrations. The first uses a microlens array at the focal plane to sample the point spread function (PSF) and micro-filters on the backside of each microlens to separate colors. The micropupils are immediately imaged on the detector. The second preserves the microlens array at the focal plane but re-images the array of micropupils through a beam-splitter on the detector. In both concepts the PSF measurement is made at the microlens array, so all optics is common prior to the PSF measurement in all colors. A simple prototype was used to test the concepts; preliminary results yield noise attenuation of ~10^-2.

Select this Article		The double Prime Focus camera for the Large Binocular Telescope Roberto Ragazzoni, Emanuele Giallongo, Fabio Pasian, Carmelo Arcidiacono, Andrea Baruffolo, Emiliano Diolaiti, Andrea Di Paola, Fabio Faccin, Jacopo Farinato, Adriano Fontana, F. Gasparo, Fernando Pedichini, Riccardo Smareglia, Roberto Speziali, and Elise Vernet Proc. SPIE 5492, 507 (2004); http://dx.doi.org/10.1117/12.552136 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Prime Focus for the Large Binocular Telescope are a couple of Prime Focus stations each equipped with four 4kx2k CCDs and a six lenses corrector with an aspheric surface and the first lens as large as roughly 800mm in diameter. These cameras will cover almost half degree of Field of View on 8m-class telescopes with unprecedented velocity of F/1.4. The two units are optimized for the Red and Blue portions of the visible wavelength and additionally an extension to J and H bands is foreseen. An overview of the project, including the optomechanics, the cryogenics, the electronics, and the software is given along with a preliminary account of lessons learned and on how much the second unit, the Red one, the schedule of which is shifted with respect to the Blue one by several months, will take advantage from the experience gained in the Blue unit assembly and integration.

Select this Article		Optical alignment of the LBT prime focus camera Emiliano Diolaiti, Jacopo Farinato, Roberto Ragazzoni, Elise Vernet, Carmelo Arcidiacono, and Fabio Faccin Proc. SPIE 5492, 513 (2004); http://dx.doi.org/10.1117/12.552224 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract While this paper is written, the Blue channel of the double prime focus camera for the Large Binocular Telescope is being commissioned at the telescope. We report here on the optical alignment of the prime focus corrector, a rather challenging activity, due to the tight alignment tolerances and to the size of the lenses. Furthermore we describe the current plans about the alignment of the prime focus corrector with the primary mirror of the telescope, which is foreseen in the next few months.

Select this Article		Subaru next-generation wide-field camera: HyperSuprime Yutaka Komiyama, Satoshi Miyazaki, Hidehiko Nakaya, Hisanori Furusawa, and Kunio Takeshi Proc. SPIE 5492, 525 (2004); http://dx.doi.org/10.1117/12.552437 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We summarize the design and the specification of a next generation instrument for Subaru Telescope: a very wide-field (2°ϕ) CCD camera which we name HyperSuprime. The latest design of the corrector ensures 80% encircled energy diameter of 0".3 from 600 nm to 1100 nm over the 2°ϕ field of view. The size of the focal plane is 612 mm in diameter and covered by about 170 four side buttable 2kx4k CCDs. Fully depleted CCD which is now being developed is the primary candidate for HyperSuprime. The readout electronics is connected behind the CCD and this CCD package is screwed to the cold plate with three positioning pins. The large entrance window of the dewar is supported with additional ribs so that the dewar is evacuated and CCDs are cooled down to about -80°C. HyperSuprime equips with a filter exchanger which can accommodate four large mosaicked filters and a roll-type shutter.

Select this Article		Mass-producing spectra: the SDSS spectrographic system Peter R. Newman, Dan C. Long, Stephanie A. Snedden, S. J. Kleinman, Atsuko Nitta, Michael Harvanek, Jurek Krzesinski, Howard J. Brewington, J. C. Barentine, Eric H. Neilsen, Jr., and David J. Schlegel Proc. SPIE 5492, 533 (2004); http://dx.doi.org/10.1117/12.541394 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Sloan Digital Sky Survey is the largest redshift survey conducted to date, and the principal survey observations have all been conducted on the dedicated SDSS 2.5m and 0.5m telescopes at Apache Point Observatory. While the whole survey has many unique features, this article concentrates on a description of the systems surrounding the dual fibre-input spectrographs that obtain all the survey spectra and that are capable of recording 5,760 individual spectra per night on an industrial, consistent, mass-production basis. It is hoped that the successes and lessons learned will prove instructive for future large spectrographic surveys.

Select this Article		PEPPER: a photometer designed for the direct detection of extrasolar planets Matthew C. Graham, Dan E. Potter, and Laird Close Proc. SPIE 5492, 545 (2004); http://dx.doi.org/10.1117/12.552253 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract PEPPER, a high-speed differential Polarization-Encoded Photometer and Polarimeter, is designed to perform self-calibrated shot noise-limited photometry from the ground to directly detect the light from the phase changes of close-in extrasolar planets. This is accomplished by using high-speed electro-optical switching techniques coupled with zero-read noise photon counting detectors to eliminate errors due to sky and detector gain drift variability. Here we present the design concept behind the photometer mode of PEPPER as well as some initial results from lab and on-sky engineering tests of the prototype instrument. The polarimeter mode of the instrument is presented in a seperate paper.

Select this Article		Mounting large lenses for the MMT's f/5 wide-field corrector: lessons learned Robert G. Fata, Vladimir Kradinov, and Daniel Fabricant Proc. SPIE 5492, 553 (2004); http://dx.doi.org/10.1117/12.552289 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract At its f/5 focus, the 6.5 meter converted MMT uses a refractive corrector to produce excellent images over a field of view as large as 1° in diameter. We describe the construction challenges we encountered and the lessons we learned mounting the ~30 inch diameter lenses for this wide-field corrector. The corrector was completed in May 2002, was commissioned in May and June of 2003, and is now in regular use at the MMT for spectroscopic and imaging observations.

Select this Article		The SOAR optical imager: status and first results Hugo E. Schwarz, Michael C. Ashe, Maxime Boccas, Marco Bonati, Francisco Delgado, Ramon Gavez, Manuel Martinez, Patricio Schurter, Ricardo Schmidt, Roberto Tighe, and Alistair R. Walker Proc. SPIE 5492, 564 (2004); http://dx.doi.org/10.1117/12.553185 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We briefly describe the SOAR Optical Imager (SOI), the first light instrument for the 4.1m SOuthern Astronomical Research (SOAR) telescope now being commissioned on Cerro Pachn in the mountains of northern Chile. The SOI has a mini-mosaic of 2 2kx4k CCDs at its focal plane, a focal reducer camera, two filter cartridges, and a linear ADC. The instrument was designed to produce precision photometry and to fully exploit the expected superb image quality of the SOAR telescope over a 5.5x5.5 arcmin² field with high throughput down to the atmospheric cut-off, and close reproduction of photometric pass-bands throughout 310-1050 nm. During early engineering runs in April 2004, we used the SOI to take images as part of the test program for the actively controlled primary mirror of the SOAR telescope, one of which we show in this paper. Taken just three months after the arrival of the optics in Chile, we show that the stellar images have the same diameter of 0.74" as the simultaneously measured seeing disk at the time of observation. We call our image "Engineering 1^st Light" and in the near future expect to be able to produce images with diameters down to 0.3" in the R band over a 5.5' field during about 20% of the observing time, using the tip-tilt adaptive corrector we are implementing.

Select this Article		Study on the optical fiber positioning medium-term system for LAMOST Hongzhuan Hu, Xiaobo Peng, Chao Zhai, Weimin Li, and Xiaozheng Xing Proc. SPIE 5492, 574 (2004); http://dx.doi.org/10.1117/12.549785 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract This paper proposes research of a structure of LAMOST fiber positioning medium-term system; its construction and its tests are briefly introduced. This medium-term system includes several parts as follow: a main control computer, a unit controller, a set of drive circuits, 19 optical positioning units that positioning 19 optical fiber ends on the small simulate focal plane with diameter of 180 mm, a CCD camera, a frame grabber, and control programs. Tests on the system have indicated that positioning precision of 19 units is less than 0.04 mm on the whole focal plane with diameter of 180 mm. On medium-term system, some important problem for LAMOST building has test and research, for example: Fiber positioning precision, mechanism interference among the units, anti-jamming of drive circuits, unit's work life-span and reliability, temperature raising, etc. Test results have established stability foundation for LAMOST construction.

Select this Article		The measurement system for fiber positioning unit of LAMOST Weimin Li, Xiaozheng Xing, Jin Yi, Hongzhuan Hu, Chao Zhai, and Qiaoyun Yu Proc. SPIE 5492, 584 (2004); http://dx.doi.org/10.1117/12.550880 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The paper proposes the measurement system for the fiber positioning unit of LAMOST(Large Sky Area of Multi-Object Fiber Spectroscope Telescope). It consists of an area CCD sensor, an image acquisition card, and a lens. The fiber is illuminated by light source from one end. The end of the fiber on the focal plate is imaged on the area CCD sensor by the lens. The image of the fiber end is acquired by the area CCD sensor, and transferred into a computer by the image grabber. Some pro-processed methods are used to process the digital image of the fiber. According to further digital image processing, the position of the fiber is obtained. The paper focuses on the calibration method of the digital area CCD camera. The measurement system calibrates the camera with the calibration board. The calibration board has some holes illuminated by an area LED. The positions of those holes are pre-measured precisely. Then, the systematic error of the measurement is figured out through the calibration procession. The optical aberration is fitted by the quartic surface. The measurement system can measure the position of the fiber on the positioning unit precisely. The precision of the measurement system is 0.010mm.

Select this Article		HIPO: a high-speed imaging photometer for occultations Edward W. Dunham, James L. Elliot, Thomas A. Bida, and Brian W. Taylor Proc. SPIE 5492, 592 (2004); http://dx.doi.org/10.1117/12.552152 \| Cited 6 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract HIPO is a special purpose instrument for SOFIA, the Stratospheric Observatory For Infrared Astronomy. It is a high-speed, imaging photometer that will be used for a variety of time-resolved precise photometry observations, including stellar occultations by solar system objects and transits by extrasolar planets. HIPO has two independent CCD detectors and can also co-mount with FLITECAM, an InSb imager and spectrometer, making simultaneous photometry at three wavelengths possible. HIPO's flexible design and high-speed imaging capability make it well suited to carry out initial test observations on the completed SOFIA system, and to this end a number of additional features have been incorporated. Earlier papers have discussed the design requirements and optical design of HIPO. This paper provides an overview of the instrument, describes the instrument's features, and reviews the actual performance, in most areas, of the completed instrument.

Select this Article		Photon counting and fast photometry with L3 CCDs Simon M. Tulloch Proc. SPIE 5492, 604 (2004); http://dx.doi.org/10.1117/12.550353 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The new L3 Technology CCDs from E2V allow detector read noise to be decoupled from readout speed. If operated at sufficiently high gain, the read noise drops to sub-electron levels and photon counting becomes possible. At ING we have incorporated CCD60 , CCD87 and CCD97 L3 detectors into cryogenic cameras coupled to SDSU controllers for a variety of tests both in the lab and on-sky using the 4.2m William Herschel Telescope. These detectors have been operated in proportional and photon-counting mode using an in-house Linux based DAS. We have gained a number of insights into photon counting optimisation, how to cope with the effects of the L3 pipeline delay and the reduction of internal device-generated spurious charge. We have also discovered a statistical method for determining the gain of an L3 system from pulse height analysis of the individual photon events. Our on-sky test program has consisted to date of high frame rate photometry of the Crab Nebula Pulsar.

Select this Article		Design of a stable fixed delay interferometer prototype for the ET project Suvrath Mahadevan, Jian Ge, Curtis DeWitt, Julian C. van Eyken, and Gerald Friedman Proc. SPIE 5492, 615 (2004); http://dx.doi.org/10.1117/12.550447 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The ET instrument being developed at Penn State is a novel approach that is capable of precision radial velocity measurements using a modest resolution. A prototype version of this instrument is now set up permanently at the Kitt Peak 2.1m telescope and has recovered the radial velocity curve of 51 Peg. The stability of the Michelson interferometer used in the setup is very crucial to obtain accurate velocity results. In this paper we discuss the issues associated with field widening and temperature compensation over a wide wavelength range and also describe the design of a prototype interferometer that meets these criteria. Our current prototype design built in the lab already outperforms our old interferometer over short time spans. A new interferometer based on the prototype will replace our current actively stabilized interferometer at Kitt Peak. The increased stability will enable us to start our planet search program in 2005, and to observe targets suitable for asteroseismology.

Select this Article		Design and construction of the IMACS-IFU: a 2000-element integral field unit Juergen Schmoll, George N. Dodsworth, Robert Content, and Jeremy R. Allington-Smith Proc. SPIE 5492, 624 (2004); http://dx.doi.org/10.1117/12.549803 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The IMACS-IFU is an Integral Field Unit built for the IMACS spectrograph at the Magellan-I-Telescope at Las Campanas Observatory. It consists of two rectangular fields of 5 by 7 square arec seconds, spearated by roughly one arc minute. With a total number of 2000 spatial elements it is the second largest fiber-lenslet based IFU worldwide, working in a wavelength range between 400 and 900 nm. Due to the equally sized fields classical background subtraction, beam switching and shuffling are possible observation techniques. One particular design challenge was the single, half a metre long curved slit in combination with a non telecentric output. Besides the construction some preliminary results are described.

Select this Article		Cryogenic tests of volume-phase holographic gratings Naoyuki Tamura, Graham J. Murray, Peter Luke, Colin Blackburn, David J. Robertson, Nigel A. Dipper, Ray M. Sharples, and Jeremy R. Allington-Smith Proc. SPIE 5492, 634 (2004); http://dx.doi.org/10.1117/12.550797 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present results from cryogenic tests of a Volume-Phase Holographic(VPH) grating at 200 K measured at near-infrared wavelengths. The aimsof these tests were to see whether the diffraction efficiency andangular dispersion of a VPH grating are significantly different at a low temperature from those at a room temperature, and to see how manycooling and heating cycles the grating can withstand. We have completed 5 cycles between room temperature and 200 K, and find that the performance is nearly independent of temperature, at least over the temperature range which we are investigating. In future, we will not only try more cycles between these temperatures but also performmeasurements at a much lower temperature (e.g., ~80 K).

Select this Article		Operational performance of OzPoz: the multifiber positioner on the VLT Peter Gillingham, Jonathan Smoker, Matthew Colless, and Andreas Kaufer Proc. SPIE 5492, 643 (2004); http://dx.doi.org/10.1117/12.550966 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract OzPoz is the multi-fiber positioner feeding the spectrographs GIRAFFE and UVES from a Nasmyth focus of VLT Unit Telescope 2. Together with GIRAFFE and UVES, it forms the FLAMES facility. FLAMES has been available for observing since successful completion of its science verification in Jan/Feb 2003. An aim of paramount importance in the design and construction of OzPoz was achievement of high reliability with minimal maintenance in the demanding Cerro Paranal VLT environment. Judged by its first 13 months of operation, it has been very successful in this respect, with an average of only 1% of observing time lost to problems; in the last 5 months of this period, the average was less than 0.1%. Of about 360 fibers and fiber bundles fed from deployable buttons on the two field plates, only one has become unusable (through breakage). The time taken to re-configure the fibers on one plate is always less than the exposure time (a minimum of 20 minutes) on the other (observing) plate, so no observing time is lost on that account and the time to interchange the two plates and acquire the new field is only about 5 minutes. The faintness of objects for which useful spectra can be obtained depends on the accuracy with which the sky background can be subtracted and this, in turn, depends on how well the relative spectral transmissions of fibers allocated to sky and to objects can be calibrated. An accuracy of 0.3% rms has been achieved.

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Poster Presentations: Optical Instrumentation II

Select this Article		Test observations of the Kyoto Tridimensional Spectrograph II at the University of Hawaii 88-in and Subaru Telescopes Hajime Sugai, Takashi Hattori, Atsushi Kawai, Shinobu Ozaki, George Kosugi, Hiroshi Ohtani, Tadashi Hayashi, Tsuyoshi Ishigaki, Motomi Ishii, Minoru Sasaki, Atsushi Shimono, Yoshiko Okita, Jun Sudo, and Norihide Takeyama Proc. SPIE 5492, 651 (2004); http://dx.doi.org/10.1117/12.550987 \| Cited 4 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract In order to investigate the physical conditions of ionized gas in galaxies, as well as its kinematics, we have developed the Kyoto tridimensional spectrograph II (3DII). It is a multi-mode instrument designed for Cassegrain focus, including integral field spectrograph (IFS) and Fabry-Perot imager modes. We have designed it compact so that we can mount it at 2-m class telescopes as well as at 8-m Subaru telescope.We have succeeded in test observations of the 3DII. In the IFS mode the spatial resolution of 0".5 and 0".4 was obtained in 30-minute exposures at University of Hawaii 88-inch (UH88) and Subaru, respectively, in relatively good weather conditions. Each of 37 × 37 microlenses subtends 0".1 in Subaru's case. Thissamples well the image size. A wider field of view is emphasized in the case of UH88. Because our micropupil spectroscopy is free from a slit effect, we have reached the accuracy of an order of one tenth of a pixel for deriving velocity fields in terms of velocity center while the full width at half maximum of the instrumental profile corresponds to two pixels. At Subaru we have used a container designed in a collaboration with National Astronomical Observatory,Japan: it fits with a robotic instrument exchanger. The containerincludes two heat exchangers to keep its surface cool and avoid degrading the image quality. We have established effective observational sequences by realizing a software interface with Subaru operating system. Some results from target observations are shown.

Select this Article		Development of the Wide Field Grism Spectrograph 2 Mariko Uehara, Chie Nagashima, Koji Sugitani, Makoto Watanabe, Shuji Sato, Tetsuya Nagata, Motohide Tamura, Noboru Ebizuka, Andrew J. Pickles, Klaus W. Hodapp, Yoichi Itoh, Makoto Nakano, and Katsuo Ogura Proc. SPIE 5492, 661 (2004); http://dx.doi.org/10.1117/12.551055 \| Cited 5 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We have developed the Wide Field Grism Spectrograph 2 (WFGS2) for the f/10 focus of the University of Hawaii 2.2 m telescope (UH88). This instrument provides slit-less, wide-field spectroscopy as well as imaging and long-slit spectroscopy. Two CCD cameras of UH88, Tektronix 2k x 2k and OPTIC 4k x 4k, can be used as a detector. The spectral coverage is 380 - 970 nm, and the field of view is 11'.5 x 11'.5 with a pixel scale of 0".34 (Tektronix) or 0".21 /pixel (OPTIC) in the imaging mode. WFGS2 has two replica grisms (R = 620 at 650 nm and R = 730 at 400 nm) and a Volume-Phase Holographic (VPH) grism (R = 2500 at 664 nm). The VPH grism enables intermediate-dispersion spectroscopy with this transmission system. Two long-slits with widths of 0".6 and 0".9 can be used. The Sloan Digital Sky Survey (g', r', i', z') and narrow-band (wide H alpha, H alpha, and [SII]+Li) filters are equipped.The first light observation was done in November 2003.We present the details of WFGS2, including the results ofthe first light observation.

Select this Article		Performances of HARPS and FEROS fibers in La Silla ESO Observatory Gerardo Avila, Dominique Kohler, Ernesto Araya, Alain Gilliotte, and Wolfgang Eckert Proc. SPIE 5492, 669 (2004); http://dx.doi.org/10.1117/12.551303 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Optical fibres have been extensively used at ESO to link telescopes to spectrographs. The last two developments included the preparation of the fibres for the HARPS and FEROS instruments in La Silla Observatory. The HARPS fibre bundle uses a high efficient scrambler for precise measurements of radial velocities (< 1 m/s). The FEROS fibre micro-lenses were updated to match the 2.2 m telescope with emphasis in optimizing the efficiency. This paper describes the features and performances of these fibres.

Select this Article		Design of low-cost and reliable instrumentation for robotic telescopes Christopher J. Mottram, Iain A. Steele, and Lusia Morales Proc. SPIE 5492, 677 (2004); http://dx.doi.org/10.1117/12.551337 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract In this paper we discuss the requirements for producing instrumentation suitable for robotic use, ona fully automated telescope. The design compromises and simplifications needed to produceinstruments that can be left unattended for long periods of operation are investigated. We describe how we structure the control system to provide fail-safe operation of the instruments.

Select this Article		The REM optical slitless spectrograph (ROSS) Gino Tosti, Marco Bagaglia, Carlo Campeggi, Nicola Masetti, Alessandro Monfardini, Luciano Nicastro, Eliana Palazzi, Elena Pian, Giorgio Sciuto, Filippo M. Zerbi, Guido Chincarini, Lucio A. Antonelli, Paolo Conconi, Stefano Covino, Giuseppe Cutispoto, et al. Proc. SPIE 5492, 689 (2004); http://dx.doi.org/10.1117/12.551421 \| Cited 5 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Fast ground based simultaneous optical-near infrared observation of gamma-ray bursts (GRBs) is a mandatory priority to understand the physical mechanisms at work in these objects. The REM (Rapid Eye Mount) telescope, recently installed at La Silla (ESO, Chile), is an example of a new generation of small robotic telescopes having the capability to allow simultaneous optical and near infrared photometry and low resolution spectroscopy. The REM Optical Slitless Spectrograph (ROSS) is the optical instrument mounted on REM. ROSS has been attached, in one of the two Nasmyth foci, orthogonally to the optical axis and receives the optical light deflected by a beam splitter (dichroic), which leaves the infrared beam to continue along the optical axis where the infrared camera (REM-IR) is installed. Low resolution optical spectroscopy is obtained using an Amici prism mounted on the same filter wheel where are also mounted the broad-band V, R, I photometric filters. The detector head is a commercial camera hosting a Marconi 1024×1024 CCD chip.

Select this Article		Integral field spectroscopy with the Gemini Near-Infrared Spectrograph Jeremy R. Allington-Smith, Cornelis M. Dubbeldam, Robert Content, Colin J. Dunlop, David J. Robertson, Jay Elias, Bernadette Rodgers, and James E. Turner Proc. SPIE 5492, 701 (2004); http://dx.doi.org/10.1117/12.551627 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Astronomical Instrumentation Group (AIG) of the University of Durham has recently completed an integral fieldunit (IFU) for use on the Gemini-South telescope with the Gemini Near-Infrared Spectrograph (GNIRS) built by theNational Optical Astronomy Observatories (NOAO, USA). When the IFU is deployed remotely inside the instrumentcryostat, GNIRS is converted into an integral field spectrograph with a field of 5 × 3 arcsec2 and spatial sampling of0.15 × 0.15 arcsec2, optimised for 1-2.5μm but operable up to 5μm. We present summaries of the design andconstruction and results from laboratory testing. We also show results obtained at the telescope where a throughput of90% was measured at 2.5μm, and show that this is consistent with predictions of a simple model where surfacescattering is the dominant loss mechanism. The throughput data are well fit by the roughness measured in thelaboratory. Finally, we show a few examples of astrophysical data from the commissioning run in April 2004.

Select this Article		All-sky extrasolar planet searches with multi-object dispersed fixed-delay interferometer in optical and near IR Jian Ge, Suvrath Mahadevan, Julian C. van Eyken, Curtis DeWitt, Jerry Friedman, and Deqing Ren Proc. SPIE 5492, 711 (2004); http://dx.doi.org/10.1117/12.551989 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract An all sky survey for extrasolar planets with wide field telescopes, Sloan 2.5m and WIYN 3.5 telescopes, is being developed. This survey will use a multi-object version of current Exoplanet Tracker (ET) Doppler instrument commissioned at the KPNO 2.1m telescope in June 2004. This instrument is based on dispersed fixed-delay interferometer, a combination of a Michelson interferometer with a moderate dispersion spectrometer (Ge 2002). This custom designed instrument (f/2 optics) has a wavelength coverage of ~ 600 Å with a 4kx4k CCD camera at a spectral resolution of R = 5,000. The measured instrument detection efficiency, including telescope, fiber, interferometer, spectrometer and detector losses, has ~ 18% (or 50% throughput from the fiber input to the detector), more than 4 times higher than current echelle instruments being used for planet detection. ET has been able to routinely obtain S/N ~ 80 data for V ~ 8 mag. stars in 15 min exposures with the KPNO 2.1m. It allows us to reach ~ 3.5 m/s Doppler precision for radial velocity (RV) stable stars with S/N ~ 120 per pixel. It also allows us to confirm an exoplanet curve of HD 130322 (V = 8.05) with rms Doppler error of 12.3 m/s (preliminary results). We are in the middle of design of two prototype multiple object RV instrument for the Sloan and WIYN telescopes, which are capable of observing 50 stars (V ~ 8-13) in a single exposure. We plan to conduct the all sky survey for planets around ~ 1 millions of stars with Sloan starting in 2008. Our goal is to identify ~ 100,000 extrasolar planets with ~ 1,000 solar analogues through this survey.

Select this Article		Development of the wide-field IFU PPak Andreas Kelz, Marc Verheijen, Martin M. Roth, Uwe Laux, and Svend-Marian Bauer Proc. SPIE 5492, 719 (2004); http://dx.doi.org/10.1117/12.551990 \| Cited 4 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract PPak is a new fiber-bundle, developed at the Astrophysical Institute Potsdamfor the existing PMAS 3D-instrument. The intention of PPak is to providea large integral field-of-view in combination with a large collecting areaper fiber for the study of extended low-surface brightness objects.The PPak system consists of a focal reducer lens and a fiber bundle, featuringan 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.

Select this Article		Faint object 3D spectroscopy with PMAS Martin M. Roth, Thomas Becker, Andreas Kelz, and Petra Bohm Proc. SPIE 5492, 731 (2004); http://dx.doi.org/10.1117/12.552003 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract PMAS is a fiber-coupled lens array type of integral field spectrograph, whichwas commissioned at the Calar Alto 3.5m Telescope in May 2001. The opticallayout of the instrument was chosen such as to provide a large wavelengthcoverage, and good transmission from 0.35 to 1 mu. One of the majorobjectives 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 scienceresults obtained during the first two years of operation, we illustratethat 3D spectroscopy is an ideal tool for faint object spectrophotometry.

Select this Article		An Image Motion Compensation System for the Multi-Object Double Spectrograph Jennifer L. Marshall, Bruce Atwood, Paul L. Byard, Darren L. DePoy, Thomas P. O'Brien, and Richard W. Pogge Proc. SPIE 5492, 739 (2004); http://dx.doi.org/10.1117/12.552015 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We describe progress on a closed-loop image motion compensation system (IMCS) for the Multi-Object Double Spectrograph (MODS). The IMCS actively compensates for image motion in the focal plane within the instrument caused by temperature fluctuation, mechanism flexure, and large scale structural bending due to gravity. The system utilizes an infrared laser as a reference beam that shares a light path with the science beam and is detected by an infrared reference detector adjacent to the science detector. The reference detector is read out frequently and detects any image motion in the focal plane. The IMCS compensates for this motion during a science exposure by adjusting the tip and tilt angles of the collimator mirror. A working lab prototype meets specifications and is described.

Select this Article		First light performance of a near-UV spatial heterodyne spectrometer for interstellar emission line studies Edwin J. Mierkiewicz, Fred L. Roesler, John M. Harlander, Ron J. Reynolds, and Kurt P. Jaehnig Proc. SPIE 5492, 751 (2004); http://dx.doi.org/10.1117/12.552326 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract This paper describes the characteristics and performance of a novel spatial heterodyne spectrometer designed to measure the extremely faint [OII] 372.6 nm and 372.9 nm emission lines from the warm (10,000 K) ionized component of our Galaxy's interstellar medium. These [O II] lines are a principal coolant for this wide spread, photoionized gas and are a potential tracer of variations in the gas temperature resulting from unidentified interstellar heating processes that appear to be acting within the Galaxy.In the basic SHS system, Fizeau fringes of wavenumber-dependent spatial frequency are produced by a Michelson interferometer modified by replacing the return mirrors with diffraction gratings; these fringes are recorded on a position sensitive detector and Fourier transformed to recover the spectrum over a limited range centered at the Littrow wavenumber of the gratings. The system combines interferometric and field-widening gains in tandem to achieve 10,000-fold sensitivity gains compared to conventional grating instruments of similar size and resolving power. SHS systems also have relaxed flatness tolerances (20-50 times compared to Fabry-Perots) and do not require precision imaging to achieve diffraction-limited spectroscopic performance. Defects can largely be removed in data processing.Early results from our [OII] SHS system confirm the superb performance of the SHS technique for measurements of spatially extended faint emissions, including the first detection of [O II] emission lines extending out to 20 degrees from the Galactic equator ([OII] intensities ranged from tens of rayleighs near the Galactic plane to less than one rayleigh at high latitudes; the [OII] line profiles show structure indicating emission along the lines of sight from both the local interstellar gas and more distant gas in the Perseus spiral arm).

Select this Article		The 6.5-m MMT's f/5 wide-field optics and instruments Daniel Fabricant, Robert G. Fata, Brian A. McLeod, Andrew H. Szentgyorgyi, J. Barberis, Henry W. Bergner, Jr., Warren R. Brown, Nelson Caldwell, Maureen A. Conroy, Roger Eng, Harland Epps, G. Furesz, Tom M. Gauron, John Geary, Richard E. Goddard, et al. Proc. SPIE 5492, 767 (2004); http://dx.doi.org/10.1117/12.551729 \| Cited 7 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract In 2003, the converted MMT"s wide-field f/5 focus was commissioned. A 1.7-m diameter secondary and a large refractive corrector offer a 1° diameter field of view for spectroscopy and a 0.5° diameter field of view for imaging. Stellar images during excellent seeing are smaller than 0.5" FWHM across the spectroscopic field of view, and smaller than 0.4" across the imaging field of view. Three wide-field f/5 instruments are now in routine operation: Hectospec (an R~1000 optical spectrograph fed by 300 robotically-positioned optical fibers), Hectochelle (an R~40,000 optical spectrograph fed by the same fibers), and Megacam (a 340 megapixel, 36 CCD optical imager covering a 25' by 25' format).

Select this Article		Double Bragg grating tunable filter Sebastien Blais-Ouellette, Edward H. Wishnow, Patrick L. Shopbell, Wil van Breugel, Keith Taylor, and Roger Smith Proc. SPIE 5492, 779 (2004); http://dx.doi.org/10.1117/12.551743 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A novel concept for a very efficient tunable filter for the optical and near infrared is proposed. The filter consistsof two parallel volume phase holographic Bragg gratings used in a dispersion-recombination configuration. Thepassband profile is determined by the first order grating efficiency curve which changes in wavelength accordingto the angle of incidence. The filter can be continuously tuned over ranges of wavelengths larger than 600 nmby adjusting the tilt of the gratings, while bandwidth can be selected between 0.1 and 200 nm. The conceptualdesign is presented, along with predicted performances. Potentially useful instruments for large volume surveysand targeted observations are explored, along with application in areas other than astronomy.

Select this Article		90prime: a prime focus imager for the Steward Observatory 90-in. telescope G. Grant Williams, Ed Olszewski, Michael P. Lesser, and James H. Burge Proc. SPIE 5492, 787 (2004); http://dx.doi.org/10.1117/12.552189 \| Cited 11 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Steward Observatory is currently commissioning a prime focus wide-fieldimager for the 90-inch telescope located at Kitt Peak. The camera'sfocal plane array is populated with a mosaic of four thinnedLockheed 4096 x 4096 pixel CCDs. The f/2.98 system provides aplate scale of 0.45"/pixel and a total field-of-view of1.16 x 1.16 degrees.The optical design includes a four element correctorand six position filter wheel. The first science run was conducted inNovember 2003. We will describe the design of the ``90prime'' instrumentand results from the commissioning runs.

Select this Article		The DEIMOS flexure compensation system: overview and operational results Robert I. Kibrick, Steven L. Allen, De A. Clarke, Sandra M. Faber, Andrew C. Phillips, and Gregory D. Wirth Proc. SPIE 5492, 799 (2004); http://dx.doi.org/10.1117/12.552327 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The DEep Imaging Multi-Object Spectrograph (DEIMOS) was commissioned onKeck II in June 2002. It employs a closed-loop flexure compensationsystem (FCS) to measure and compensate for image motion resulting fromgravitationally-induced flexure of spectrograph elements. The FCSutilizes a set of fiber-fed FCS light sources located at the edges of theinstrument focal plane to produce a corresponding set of spots on a pairof FCS CCD detectors located on either side of the science CCD mosaic.(This FCS light follows the same light path through the instrument as thescience spectra.) During science exposures, the FCS detectors are read outseveral times per minute. These FCS images are analyzed in real time tomeasure any translational motion of the FCS spots and to derive correctionsignals; those signals drive active optical mechanismswhich steer the spots back to their nominal positions, thus stabilizingthe images on the FCS CCDs and the science mosaic.This paper describes the commissioning of the DEIMOS FCS system, itscontinued evolution during its first 18 months of operation on thetelescope, and its operational performance over that period. We describethe various challenges encountered while refining the initial FCS prototype(deployed at commissioning) into a fully-operational and highly-reliablesystem that is now an essential component of the instrument. Thesechallenges include: reducing stray light from FCS light sources to anacceptable level; resolving interactions between FCS acquisition andslit mask alignment; providing robust rejection of cosmic ray events inFCS images; implementing a graphical user interface for FCS control andstatus.

Select this Article		AFOS: probing the UV-visible potential of the Antarctic plateau Jessica T. Dempsey, John W. V. Storey, Michael C. B. Ashley, Michael G. Burton, Paolo G. Calisse, and Mark A. Jarnyk Proc. SPIE 5492, 811 (2004); http://dx.doi.org/10.1117/12.552354 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Antarctic Fiber-Optic Spectrometer (AFOS) is a 30cm Newtonian optical telescope that injects light through six 30m long optical fibers onto a 240-850nm spectrograph with a 1024 x 256 pixel CCD camera. The telescope is mounted on a dual telescope altitude-azimuth mount and has been designed to measure the transperency of the atmosphere above the South Pole for astronomy in the UV and visible wavelength regions. The instrument has observed a series of bright O and B stars during the austral winters of 2002 and 2003 to probe the UV cutoff wavelength, the auroral intensity and water vapour content in the atmosphere above the plateau.AFOS is the first completely automated optical telescope on the Antarctic Plateau. This paper reports on the results of the past two austral winters of remote observing with the telescope as well as the technical and software modifications required to improve the quality and automation of the observations. The atmospheric absorption bands in the 660-900nm regions of the spectra have been fitted with MODTRAN atmospheric models and used to calculate the precipitable water vapour above the South Pole. These data are then compared to those collected concurrently by radiosonde and by a 350 micron submillimeter tipper at South Pole.

Select this Article		Adaptive-optics-assisted integral field spectroscopy with OASIS and NAOMI Richard McDermid, Roland Bacon, Gilles Adam, Chris Benn, and Michele Cappellari Proc. SPIE 5492, 822 (2004); http://dx.doi.org/10.1117/12.552912 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract By incorporating spatial coverage with the spectral dimension,integral-field spectroscopy is uniquely suited for exploiting thecapabilities of adaptive optics (AO) systems. OASIS is a lenslet-basedintegral-field spectrograph designed to perform high-resolutionobservations on AO-corrected sources, operating at visiblewavelengths. This instrument was commissioned at the William HerschelTelescope, La Palma, in July 2003 to work with the ING's AO system,NAOMI. Here we present an overview of the capabilities of theOASIS+NAOMI system, and show results obtained using this technique. Thescience presented here is a small preview of what will be possible fora large number of objects when the GLAS laser guide system isoperational.

Select this Article		Mercator and the P7-2000 photometer Gert Raskin, Gilbert Burki, Michel Burnet, Geert Davignon, Rene Dubosson, Emile Ischi, Michel George, Michel Grenon, Charles Maire, Hans Van Winckel, Christoffel Waelkens, and Luc Weber Proc. SPIE 5492, 830 (2004); http://dx.doi.org/10.1117/12.550191 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present the Mercator Telescope together with the P7-2000 photometer as its first-light instrument. Mercator is a 1.2-meter Ritchey-Chretien telescope, installed at the Roque De Los Muchachos Observatory on La Palma and fully operational since Spring 2001. The Geneva Observatory developed this telescope and a twin, known as the Euler Telescope, was already inaugurated at the La Silla Observatory in 1998. Mercator is an alt-azimuthal telescope designed for semi-automatic operation and high operational robustness.P7 is a high-precision 2-channel differential photometer, built by the Geneva Observatory and in permanent use for over 25 years on various telescopes. It allows quasi-simultaneous observations in the 7 filters of the Geneva photometric system with a variable sampling rate up to 100 samples per second. This vintage instrument was completely refurbished in 2000 to function in an automatic mode on the Mercator Telescope. Electronics were completely renewed and are now based on a digital signal processor (DSP), which controls the instrument and performs basic data reduction. The optical system was left unmodified, apart from the addition of a field camera that is also used for auto-guiding. We also added instrument temperature control and a mechanical derotator. Since the 7 filters are acquired simultaneously and the absolute calibration of the colors is strictly homogeneous, the Mercator-P7 combination is a unique tool to study stellar variability on many different timescales. The current scientific program focuses on multi-periodic phenomena in early-type stars with the goal to identify the frequency spectrum and to constrain stellar models by asteroseismology studies. More than 43000 observations have been performed since 2001 and a precision of few milli-magnitudes is routinely achieved. Our photometric measurements result in the continuous calculation of the atmospheric extinction coefficients and these data are available online for other observers as well. In this paper, we describe the telescope, the photometer and their software, followed by the presentation of some first results. Finally, we discuss an upcoming upgrade and the complete instrumentation plan for Mercator.

Select this Article		Wide-field corrector with ADC compensator and image stabilizer for f/1.7 Gemini telescope prime focus Ming Liang, Samuel C. Barden, and Rick Robles Proc. SPIE 5492, 841 (2004); http://dx.doi.org/10.1117/12.550260 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract KAOS (Kilo-Aperture Optical Spectrograph) is a multi object spectrograph fiber fed from the f/1.7 prime focus of Gemini north telescope. A wide field corrector has been designed for the focus to provide a sub arc-second image over 1.5° FOV. The corrector includes four lenses and ADC (atmospheric dispersion compensator) prisms, which also act as an imager stabilizer. This paper describes the corrector design and presents the optical performance. In the final section, some other design options are discussed.

Select this Article		Data acquisition system for the instruments of Subaru Telescope Hidehiko Nakaya Proc. SPIE 5492, 852 (2004); http://dx.doi.org/10.1117/12.550350 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We have upgraded the data acquisition system for the instruments of Subaru Telescope in these three years. We report the performance of the new data acquisition system Messia5, and the performance of the instruments whose acquisition system have been upgraded to the new system. The most important purpose of the replacement is increasing the observation efficiency. The second purpose is reducing the time and the effort to maintain the data acquisition system. The third purpose is to lead developments of next generation instruments. The new data acquisition system Messia5 is constructed with a commercial DSP board and works with Linux operating system. It has the performance to handle 160MByte/s continuously. It does not only have a capability to be applied to optical instruments, but also has a potential to be applied to infrared instruments. We have successfully upgraded the data acquisition system of the three optical instruments of Subaru Telescope, which are Suprime-Cam, FOCAS, and HDS. We have also upgraded that of an infrared instrument SIRIUS which has three HgCdTe 1k x 1k infrared arrays in April 2004.

Select this Article		Robotic telescope for rapid gamma-ray burst follow-up observations Rie Sato, Nobuyuki Kawai, Motoko Suzuki, Yoichi Yatsu, and Jun Kataoka Proc. SPIE 5492, 859 (2004); http://dx.doi.org/10.1117/12.550890 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Abstract not available

Select this Article		CCD camera and automatic data reduction pipeline for the Mercator telescope on La Palma Geert Davignon, Andre Blecha, Gilbert Burki, Fabien Carrier, Martin Groenewegen, Charles Maire, Gert Raskin, Hans Van Winckel, and Luc Weber Proc. SPIE 5492, 871 (2004); http://dx.doi.org/10.1117/12.550773 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract In this paper we present the development of a CCD imager for the modern 1.2m MERCATOR telescope dedicated to long term monitoring of variable astrophysicalphenomena. This instrument is a result of the collaboration of the Observatory of Geneva with the Institute of Astronomy in Leuven. After a technical description of the main components of the CCD camerasystem, the text will focus on the automatization of the observations andsubsequent data reduction. The telescope itself is an altazimuth mounted1.2 m Ritchey-Chretien telescope and is operated in a semi-automatic mode. The system executes a predefined sequence of observations, that only needoccasional checking of data quality by the astronomer. The observation software is written in a FORTRAN based interpreter language (INTER)running on a UNIX system that communicates with the astronomer via GUIsimplemented in Perl/Tk. The data reduction is integrated into one packageand includes pre-reduction, photometric and astrometric calibration,extraction, catalogue preparation and archiving. This allows to have a GUI driven reduction that is both flexible androbust. The preliminary reduced data give the astronomers an indication ofthe quality of their observations, so that they can adjust their programor camera settings during the same night.

Select this Article		OSIRIS camera barrel optomechanical design Alejandro Farah, Carlos Tejada, Jesus Gonzalez, Francisco J. Cobos, Beatriz Sanchez, Javier Fuentes, and Elfego Ruiz Proc. SPIE 5492, 880 (2004); http://dx.doi.org/10.1117/12.550658 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A Camera Barrel, located in the OSIRIS imager/spectrograph for the Gran Telescopio Canarias (GTC), is described in this article. The barrel design has been developed by the Institute for Astronomy of the University of Mexico (IA-UNAM), in collaboration with the Institute for Astrophysics of Canarias (IAC), Spain. The barrel is being manufactured by the Engineering Center for Industrial Development (CIDESI) at Queretaro, Mexico. The Camera Barrel includes a set of eight lenses (three doublets and two singlets), with their respective supports and cells, as well as two subsystems: the Focusing Unit, which is a mechanism that modifies the first doublet relative position; and the Passive Displacement Unit (PDU), which uses the third doublet as thermal compensator to maintain the camera focal length and image quality when the ambient temperature changes.This article includes a brief description of the scientific instrument; describes the design criteria related with performance justification; and summarizes the specifications related with misalignment errors and generated stresses. The Camera Barrel components are described and analytical calculations, FEA simulations and error budgets are also included.

Select this Article		Instrument remote control project at TNG: SARG implementation Rosario Cosentino, Pietro Bruno, Manuel Gonzalez, Manuel Huertas, and Salvatore Scuderi Proc. SPIE 5492, 891 (2004); http://dx.doi.org/10.1117/12.551464 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The high resolution spectrograph at TNG (SARG), mounted at the telescope in 2000, is based on the 'first generation CCD controller1, transputers and VME real time computer that control the instrument and the detectors. The evolution of the CCD controller, with high performance in speed acquisition and transfer rate, has changed the architecture of the instrument control. Due to the high performances of modern LAN, it has become possible to have direct access to CCD controller and instruments features. The architecture is based on a remote system, connected to a local system through standard network facilities and communicating with it using an XML-like syntax. The remote system receives from the local system commands and, in turn, sends back telemetry and images. This control system will be tested for the first time with the SARG spectrograph, in the framework of the Instruments remote control project at the Telescopio Nazionale Galileo (TNG)

Select this Article		Large Binocular Camera: the final acceptance tests of the blue channel Roberto Speziali, Fernando Pedichini, Andrea Di Paola, Adriano Fontana, and Emanuele Giallongo Proc. SPIE 5492, 900 (2004); http://dx.doi.org/10.1117/12.553772 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Large Binocular Camera (LBC) is the double optical imager whose blue channel is going to start the commissioning phase at the Large Binocular Telescope (2x8.4 m). We present the updated characteristics of the CCD camera and its characterization performed in the laboratory of the Rome Observatory and in the integration room of the Arcetri Observatory.

Select this Article		MUSE optomechanical design and performance Francois Henault, Roland Bacon, Hans Dekker, Bernard Delabre, Slimane Djidel, Jean-Pierre Dubois, Norbert Hubin, Blandine Lantz, Wing Lau, Miska Le Louarn, Ian J. Lewis, Jean-Louis Lizon, James Lynn, Luca Pasquini, Roland Reiss, et al. Proc. SPIE 5492, 909 (2004); http://dx.doi.org/10.1117/12.554096 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Abstract not available

Select this Article		Optical and optomechanical design of the WIYN High Resolution Infrared Camera Robert H. Barkhouser, Stephen A. Smee, and Margaret Meixner Proc. SPIE 5492, 921 (2004); http://dx.doi.org/10.1117/12.578365 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The WIYN High Resolution Infrared Camera (WHIRC) is being developed for use on the WIYN 3.5 m telescope at Kitt Peak. It will mount on a Nasmyth port behind the recently commissioned WIYN Tip-Tilt Module (WTTM). WTTM is expected to routinely deliver 0.25" FWHM images in the near infrared (0.8-2.5 μm), with occasional periods of 0.12" diffraction-limited performance in the K band. WHIRC will take advantage of this superb imaging capability, offering a plate scale of 0.09" per pixel and a 3'x3' field-of-view (FOV) with the planned 2K² detector. Stringent moment loading requirements at the WTTM interface necessitate a compact, low mass design, which has been achieved using an all-refractive optical path. Tight centering tolerances on the lenses call for precision cryogenic lens assemblies. In this paper we present details of the optical and optomechanical designs, and engineering analyses completed to date.

Select this Article		A fiber-fed VPHG-based high-resolution spectrograph for moderate-aperture robotic telescopes Giorgio Toso, Ruben Mazzoleni, Filippo M. Zerbi, Paolo Conconi, and Emilio Molinari Proc. SPIE 5492, 932 (2004); http://dx.doi.org/10.1117/12.580327 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The use of high diffraction efficiency Volume Phase Holographic grating as central element in a spectrograph allows to consistently increase the instrumental throughput. Moreover the geometry they use allow them to be located in simplified optical designs and their manufacturing characteristics make them ideal also for the high resolution (R > 20,000) domain. VPHG are the perfect solution for high resolution spectrograph coupled with moderate collecting areas such as those of robotic telescopes nowadays distributed worldwide. We present in this paper the spectrograph, currently under construction, that will equip the REM telescope at la Silla Observatory, Chile.

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Solar Instrumentation

Select this Article		Instrumentation for the Advanced Technology Solar Telescope Thomas R. Rimmele, Robert P. Hubbard, K. S. Balasubramaniam, Tom Berger, David Elmore, G. Allen Gary, Don Jennings, Christoph Keller, Jeff Kuhn, Haosheng Lin, Don Mickey, Gilberto Moretto, Hector Socas-Navarro, Jan O. Stenflo, and Haimin Wang Proc. SPIE 5492, 944 (2004); http://dx.doi.org/10.1117/12.551853 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The 4-m aperture Advanced Technology Solar Telescope (ATST) is the next generation ground based solar telescope. In this paper we provide an overview of the ATST post-focus instrumentation. The majority of ATST instrumentation is located in an instrument Coude lab facility, where a rotating platform provides image de-rotation. A high order adaptive optics system delivers a corrected beam to the Coude lab facility. Alternatively, instruments can be mounted at Nasmyth or a small Gregorian area. For example, instruments for observing the faint corona preferably will be mounted at Nasmyth focus where maximum throughput is achieved. In addition, the Nasmyth focus has minimum telescope polarization and minimum stray light. We describe the set of first generation instruments, which include a Visible-Light Broadband Imager (VLBI), Visible and Near-Infrared (NIR) Spectropolarimeters, Visible and NIR Tunable Filters, a Thermal-Infrared Polarimeter & Spectrometer and a UV-Polarimeter. We also discuss unique and efficient approaches to the ATST instrumentation, which builds on the use of common components such as detector systems, polarimetry packages and various opto-mechanical components.

Select this Article		The development of filter vector magnetographs for the Solar Magnetic Activity Research Telescope (SMART) Satoru UeNo, Shin-ichi Nagata, Reizaburo Kitai, Hiroki Kurokawa, and Kiyoshi Ichimoto Proc. SPIE 5492, 958 (2004); http://dx.doi.org/10.1117/12.550304 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract In recent years, it is beginning to be shown observationally and theoretically that the existence of the magnetic field isindispensable for active phenomena on the solar surface. In particular, the rotation or helicity of the magnetic field andtheir temporal variation are considered to be important factors which influence solar activity. In order to confirm this, itis necessary to compute vector components of the magnetic field with a higher accuracy than before. Therefore, wedeveloped two kinds of filter-type magnetographs for the Solar Magnetic Activity Research Telescope (SMART) at Hidaobservatory, which allow us to observe the polarization components in sunlight with high accuracy. We use a Lyot filterin one of two sets of magnetographs. On the other hand, a tandem-typed Fabry-Perot filter is used in one more set. Forthese two instruments, we made the following concrete advances.1. The method of coating of the pre-filters.2. Special fine-anneal on the main lenses.3. Highly accurate rotating wave-plate.4. Simultaneous observation of two kinds of filtergrams which have orthogonally polarized light mutually by using Fabry-Perot channel.5. Observation in four wavelengths which can suppress various errors.6. Low apparent Doppler shift in the FOV due to the oblique incidence of the rays to the filters.7. Large format CCD (large-sized chip, large full-well).8. High speed data transfer interface between the CCD and PC.In this paper, we report the details of these points, the expected effect of them, and the results of initial measurements.

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Infrared Imaging I

Select this Article		A novel simultaneous differential imager for the direct imaging of giant planets Rainer Lenzen, Laird Close, Wolfgang Brandner, Beth Biller, and Markus Hartung Proc. SPIE 5492, 970 (2004); http://dx.doi.org/10.1117/12.549406 \| Cited 17 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Adaptive Optics System NACO at the VLT has been equipped with a Simultaneous Differential Imager (SDI) designed to provide direct imaging of giant extra-solar planets. Exploiting the fact that all cool (Teff < 1200K) extra-solar giant planets have strong CH4 (methane) absorption beyond 1.62 μm in the H band NIR atmospheric window, diffraction limited narrow-band images centred on this absorption edge are obtained with NACO simultaneously to reduce the speckle-noise floor and increase the sensitivity for Jupiter-like planets around nearby young stars. We present the technical realization of this device and first results obtained during the commissioning run.

Select this Article		WIRCam: the infrared wide-field camera for the Canada-France-Hawaii Telescope Pascal Puget, Eric Stadler, Rene Doyon, Pierre Gigan, Simon Thibault, Gerard Luppino, Gregory Barrick, Tom Benedict, Thierry Forveille, William Rambold, James Thomas, Tom Vermeulen, Jeff Ward, Jean-Luc Beuzit, Philippe Feautrier, et al. Proc. SPIE 5492, 978 (2004); http://dx.doi.org/10.1117/12.551097 \| Cited 9 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract WIRCam (Wide-field InfraRed Camera) is a near-infrared (0.9-2.4 microns) camera developed for the prime focus of the Canada France Hawaii Telescope (CFHT), a 3.6-m telescope located on Mauna Kea, Hawaii. WIRCam is based on 4 x 2048x2048 HAWAII2RG arrays, developed by Rockwell. The camera provides a 0.3"/pixel sampling, and the close packaging of the detectors allows to cover an almost contiguous field-of-view of 20.5' x 20.5'. All optical elements are assembled in a cryovessel and cooled down to 85K by a He closed cycle cryogenerator. The two filter wheels have capacity for 8 filters (110 mm in diameter), cooled at low temperature together with the Lyot stop. These wheelsare mounted on sapphire ball bearings and powered by external motors. Passive spring indexers define their positioning. A fused-silica tip/tilt plate powered by voice coil type motors provides image stabilization in front of the cryovessel. It compensates for flexures as well as for low frequency telescope oscillations from wind shake.This paper describes the overall architecture of the camera, giving the optical estimated performances and details some specific points of the design such as filter wheels, thermal connections, etc..

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Infrared Imaging II

Select this Article		The VISTA IR camera Gavin B. Dalton, Martin Caldwell, Kim Ward, Martin S. Whalley, Kevin Burke, John M. Lucas, Tony Richards, Marc Ferlet, Ruben L. Edeson, Daniel Tye, Bryan M. Shaughnessy, Mel Strachan, Eli Atad-Ettedgui, Melanie R. Leclerc, Angus Gallie, et al. Proc. SPIE 5492, 988 (2004); http://dx.doi.org/10.1117/12.551378 \| Cited 7 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The VISTA IR Camera has now completed its detailed design phase and is on schedule for delivery to ESO"s Cerro Paranal Observatory in 2006. The camera consists of 16 Raytheon VIRGO 2048x2048 HgCdTe arrays in a sparse focal plane sampling a 1.65 degree field of view. A 1.4m diameter filter wheel provides slots for 7 distinct science filters, each comprising 16 individual filter panes. The camera also provides autoguiding and curvature sensing information for the VISTA telescope, and relies on tight tolerancing to meet the demanding requirements of the f/1 telescope design.The VISTA IR camera is unusual in that it contains no cold pupil-stop, but rather relies on a series of nested cold baffles to constrain the light reaching the focal plane to the science beam. In this paper we present a complete overview of the status of the final IR Camera design, its interaction with the VISTA telescope, and a summary of the predicted performance of the system.

Select this Article		IRIS2: a working infrared multi-object spectrograph and camera Chris G. Tinney, Stuart D. Ryder, Simon C. Ellis, Vladimir Churilov, John Dawson, Greg A. Smith, Lew Waller, John D. Whittard, Roger Haynes, Allan Lankshear, John R. Barton, C. J. Evans, Keith Shortridge, Tony Farrell, and Jeremy Bailey Proc. SPIE 5492, 998 (2004); http://dx.doi.org/10.1117/12.550980 \| Cited 4 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract IRIS2 is a near-infrared imager and spectrograph based on a HAWAII1 HgCdTe detector. It provides wide-field (7.7"×7.7") imaging capabilities at 0.4486"/pixel sampling, long-slit spectroscopy at R~2400 in each of the J, H and K passbands, and the ability to do multi-object spectroscopy in up to three masks. These multi-slit masks are laser cut, and have been manufactured for both traditional multiple slit work (~20-40 objects in a 3"×7.4" field-of-view), multiple slit work in narrow-band filters (~100 objects in a 5"×7.4" field-of-view), and micro-hole spectroscopy in narrow-band filters allowing the observation of ?200 objects in a 5"×7.4" field.

Select this Article		The science case of the CHEOPS planet finder for VLT Raffaele Gratton, Markus Feldt, Hans Martin Schmid, Wolfgang Brandner, Stefan Hippler, R. Neuhauser, Andreas Quirrenbach, Silvano Desidera, Massimo Turatto, and Daphne M. Stam Proc. SPIE 5492, 1010 (2004); http://dx.doi.org/10.1117/12.551417 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The CHEOPS Planet Finder is one of the proposed second generation instrumentsfor the VLT. Its purpose is to image and characterize giant extrasolar planetsin different phases of their evolution: young, warm planets as well as old,cold ones. Imaging the last ones is the most challenging task because of thevery large (>10⁸) flux contrast with their star. Detection of such faintsources close to the stars from the ground requires a very high Strehl ratioand efficient suppression of the speckle noise. Two complementary strategies,based on imaging polarimetry using fast modulation and on integral fieldspectroscopy, are included as scientific channels of CHEOPS, after the highorder adaptive optics module. The outputs of the two channels will allow aclose insight into the main properties of detected extrasolar planets. Inaddition, the CHEOPS instrument is well suited for a number of astrophysicalprojects, which are briefly described.

Select this Article		DAzLE: the dark ages z (redshift) Lyman-α Explorer Anthony Horton, Ian Parry, Joss Bland-Hawthorn, Sonia Cianci, David King, Richard McMahon, and Steve Medlen Proc. SPIE 5492, 1022 (2004); http://dx.doi.org/10.1117/12.551591 \| Cited 11 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract DAzLE is an near infrared narrowband differential imager being built by the Institute of Astronomy, Cambridge, in collaboration with the Anglo-Australian observatory. It is a special purpose instrument designed with a sole aim; the detection of redshifted Lyman-alpha emission from star forming galaxies at z>7. DAzLE will use pairs of high resolution (R=1000) narrowband filters to exploit low background `windows' in the near infrared sky emission spectrum. This will enable it to reach sensitivities of ~2E-21 W/m^2, thereby allowing the detection of z>7 galaxies with star formation rates as low as a few solar masses per year. The design of the instrument, and in particular the crucial narrowband filters, are presented. The predicted performance of DAzLE, including the sensitivity, volume coverage and expected number counts, is discussed. The current status of the DAzLE project, and its projected timeline, are also presented.

Select this Article		Gemini South Adaptive Optics Imager (GSAOI) Peter McGregor, John Hart, Dejan Stevanovic, Gabe Bloxham, Damien Jones, Jan Van Harmelen, Jason Griesbach, Murray Dawson, Peter Young, and Mark A. Jarnyk Proc. SPIE 5492, 1033 (2004); http://dx.doi.org/10.1117/12.550288 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Gemini South Adaptive Optics Imager (GSAOI) is the science camera and commissioning instrument for the Multi-Conjugate Adaptive Optics (MCAO) system on the Gemini South telescope. GSAOI is required to deliver diffraction-limited performance at near-infrared wavelengths over a 85"×85" field of view. It must be delivered on a short timescale commensurate with MCAO delivery. GSAOI will use a high throughput, all-refractive optical design and a mosaic of four HAWAII-2RG detectors to form an imager focal plane of 4080x4080 pixels with a fixed scale of 0.02"/pixel. The On-Detector Guide Window (ODGW) capability of the HAWAII-2RG detectors will be used for flexure monitoring and as near-infrared substitutes for MCAO natural guide star wave front sensors. The imager will include a pupil viewer for accurate alignment to MCAO and defocus lenses to measure wave front phase errors at the science detector using the curvature technique. Non-common path wave front errors will be nulled by setting the base shapes of the three MCAO deformable mirrors. The science drivers, performance predictions, optical design issues, and detector system for the instrument are described.

Select this Article		The LINC-NIRVANA interferometric imager for the Large Binocular Telescope Tom M. Herbst, Roberto Ragazzoni, Andreas Eckart, and Gerd Weigelt Proc. SPIE 5492, 1045 (2004); http://dx.doi.org/10.1117/12.551516 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We describe LINC-NIRVANA, a 1-2.5 micron interferometric imaging instrument for the Large Binocular Telescope. Operating in Fizeau beam combination mode, LINC-NIRVANA will deliver the sensitivity of a 12-meter telescope and the angular resolution of a 23-meter telescope. Unlike traditional interferometers, LINC-NIRVANA will be a true imaging device, with a field of view of ten arcseconds on a single HAWAII-2 detector array.LINC-NIRVANA employs a number of state-of-the-art technologies, including multi-conjugated adaptive optics (MCAO), innovative cooling systems, and complex software for instrument control and data analysis. We report on overall project progress and highlight some unique aspects of LINC-NIRVANA that should be of wider interest to the near-infrared instrument-building community.

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Airborne Instrumentation

Select this Article		The SOFIA science instrument program: lessons learned Sean C. Casey, Maureen L. Savage, and Eric E. Becklin Proc. SPIE 5492, 1053 (2004); http://dx.doi.org/10.1117/12.552350 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present an overview of the science instrument program for the Stratospheric Observatory for Infrared Astronomy (SOFIA). Funded for an initial suite of facility and PI instruments, the SOFIA instrument development program includes imagers and spectrometers from both U.S. and German development teams. With an emphasis on lessons learned, we review the development of the facility instrument suite. We conclude with the anticipated role for SOFIA as a new technology test bed for the latest far-infrared detectors.

Select this Article		Development of the HAWC far-infrared camera for SOFIA Doyal A. Harper, Arlin E. Bartels, Sean C. Casey, David T. Chuss, Jessie L. Dotson, Rhodri Evans, Steve Heimsath, Robert A. Hirsch, Scott Knudsen, Robert F. Loewenstein, S. Harvey Moseley, Matt Newcomb, Robert J. Pernic, Tim S. Rennick, Eric Sandberg, et al. Proc. SPIE 5492, 1064 (2004); http://dx.doi.org/10.1117/12.552151 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract HAWC (High-resolution Airborne Wideband Camera) is a facility science instrument for SOFIA (Stratospheric Observatory for Infrared Astronomy). It is a far-infrared camera designed for diffraction-limited imaging in four spectral passbands centered at wavelengths of 53, 89, 155, and 216 μm. Its detector is a 12x32 array of bolometers cooled to 0.2 K by an adiabatic demagnetization refrigerator. In this paper, we report on the development and testing of the instrument and its subsystems.

Select this Article		FIFI LS: the far-infrared integral field spectrometer for SOFIA Walfried Raab, Albrecht Poglitsch, Leslie W. Looney, Randolf Klein, Norbert Geis, Rainer Hoenle, Werner Viehhauser, Reinhard Genzel, Murad Hamidouche, Thomas Henning, and Eugene E. Haller Proc. SPIE 5492, 1074 (2004); http://dx.doi.org/10.1117/12.550435 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract FIFI LS is a far-infrared integral field spectrometer for the SOFIA airborne observatory. The instrument is designed to maximize the observing efficiency by simultaneous and nearly independent imaging of the field of view in two medium spectral resolution bands. Both spectral channels - covering a wavelength range of 42 to 110 microns and 110 to 210 microns respectively - allow diffraction limited spectral imaging. Reflective image slicers rearrange the 5x5 pixel field of view into the 1x25 pixel entrance slit of a grating spectrograph. Littrow mounted gratings with anamorphic collimators are used for spectral multiplexing with a spectral resolution between R = 1400 - 6500, depending on observing wavelength. Each spectral band employs two large format 25x16 pixel Ge:Ga detector arrays, axially stressed for the long wavelength band to achieve a longer wavelength response and slightly stressed for the short wavelength band. For each of the 25 spatial pixels, we are able to cover a velocity range of approximately 1500 km/s around a selected far-infrared line. This arrangement provides good spectral coverage with high responsivity. We present a summary of the FIFI LS design and the current status of instrument integration.

Select this Article		First test results from FORCAST: the facility mid-IR camera for SOFIA Luke D. Keller, Terry Herter, Gordon Stacey, George Gull, Justin Schoenwald, Bruce Pirger, Joseph Adams, Marc Berthoud, and Thomas Nikola Proc. SPIE 5492, 1086 (2004); http://dx.doi.org/10.1117/12.552333 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Abstract not available

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Infrared Spectroscopy I

Select this Article		First light for LIRIS (long-slit intermediate-resolution infrared spectrograph) Arturo Manchado, Mary Barreto, Jose Acosta-Pulido, Ezequeil Ballesteros, Roberto Barreto, Emilio Cadavid, Judit Carrillo, Miguel Charcos, Santiago Correa, Jose M. Delgado, Carlos Dominguez-Tagle, Omaira Gonzalez, Elvio Hernandez, Roberto Lopez, Heidy Moreno, et al. Proc. SPIE 5492, 1094 (2004); http://dx.doi.org/10.1117/12.549188 \| Cited 4 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Abstract not available

Select this Article		Design and performance of a MEMS-based infrared multi-object spectrometer John W. MacKenty, Richard F. Green, Matthew A. Greenhouse, and Raymond G. Ohl Proc. SPIE 5492, 1105 (2004); http://dx.doi.org/10.1117/12.551913 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Infrared Multi-Object Spectrometer (IRMOS) is an innovative near-IR instrument employing an array of MEMS micro mirrors for focal plane target selection. IRMOS is a joint project of the Space Telescope Science Institute, the NASA James Webb Space Telescope, and the Kitt Peak National Observatory and will shortly become available to the community at Kitt Peak. IRMOS uses a Texas Instruments 848x600 element DMD as a micro mirror array to synthesize slits to obtain up to 100 simultaneous spectra. It provides R~300, 1000, and 3000 spectroscopy in the J, H, and K bands plus R~1000 in Z together with imaging in all bands. Designed for the KPNO 4 and 2.1-meter telescopes, IRMOS will provide 3x2 and 6x4 arc minute fields of view on these telescopes. We describe the design and status of IRMOS, summarize its expected performance, and present early test data from system level lab tests.

Select this Article		Integration, testing, and performance of the Infrared Multi-Object Spectrometer Raymond G. Ohl, Joseph A. Connelly, Robert F. Boyle, Rebecca J. Derro, Danette L. Fitzgerald, Matthew A. Greenhouse, Timothy J. Madison, John E. Mentzell, Brian Nord, Leroy M. Sparr, Jason E. Hylan, Knute Ray, and John W. MacKenty Proc. SPIE 5492, 1114 (2004); http://dx.doi.org/10.1117/12.551494 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Infrared Multi-Object Spectrometer (IRMOS) is a principle investigator-class instrument for the Kitt Peak National Observatory 2.1 m and Mayall 3.8 m telescopes. IRMOS is a near-IR (0.8--2.5 micron) spectrometer with low- to mid-resolving power (R = λ/Δλ = 300-3000). On the 3.8 m telescope, IRMOS produces simultaneous spectra of ~100 objects in its 2.8 ' 2.0 arcmin field of view using a commercial micro electro-mechanical systems (MEMS) digital micro-mirror device (DMD) from Texas Instruments. The multi-mirror array DMD operates as a real-time programmable slit mask. The all-reflective optical design consists of two imaging subsystems. The focal reducer images the focal plane of the telescope onto the DMD field stop, and the spectrograph images the DMD onto a large-format detector. The instrument operates at ~90 K, cooled by a single electro-mechanical cryocooler. The bench and all components are made from aluminum 6061. There are three cryogenic mechanisms.We describe laboratory integration and test of IRMOS before shipment to Kitt Peak National Observatory. We give an overview of the optical alignment technique and integration of optical, mechanical, electrical and cryogenic subsystems. We compare optical test results to model predictions of point spread function size. We discuss some lessons learned and conclude with a prediction for performance on the telescope.

Select this Article		On-sky performance of SPIFFI: the integral field spectrometer for SINFONI at the VLT Christof Iserlohe, Matthias Tecza, Frank Eisenhauer, Reinhard Genzel, Niranjan A. Thatte, Roberto Abuter, Matthew J. Horrobin, Alexander Schegerer, Juergen Schreiber, and Henri Bonnet Proc. SPIE 5492, 1123 (2004); http://dx.doi.org/10.1117/12.552197 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract SPIFFI (SPectrometer for Infrared Faint Field Imaging) is a fully cryogenic, near-infrared imaging spectrograph built atthe Max-Planck-Institute for Extraterrestrial Physics (MPE) and upgraded with a new detector and spectrograph camera by ASTRON/NOVA, ESO and MPE. The upgraded instrument will become a facility instrument for the ESO VLT in summer 2004 as part of the SINFONI (SINgle Faint Object Near-IR Investigation) project, which is the combination of SPIFFI and ESOs adaptive optics module MACAO (Multiple Application Curvature Adaptive Optics), at the Cassegrain focus of Yepun (UT4). In spring 2003 we had the opportunity to observe with SPIFFI as a guest instrument without the AO-module at the Cassegrain focus of UT2 of the VLT. In this paper we discuss the performance of SPIFFI during theguest-instrument phase. First we summarize the technical performance of SPIFFI like the spatialand spectral resolution, the detector performance and the instruments throughput. Afterwards we illustrate the power of integral field spectroscopy by presenting data and results of the Galactic Center.

Select this Article		CIRPASS: description, performance, and astronomical results Ian Parry, Andrew Bunker, Andrew Dean, Michelle Doherty, Anthony Horton, David King, Marie Lemoine-Busserole, Craig D. Mackay, Richard McMahon, Steve Medlen, Robert G. Sharp, and Joanna Smith Proc. SPIE 5492, 1135 (2004); http://dx.doi.org/10.1117/12.552012 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Cambridge Infra-red Panoramic Survey Spectrograph (CIRPASS) is described. This near-infrared (NIR) spectrograph has been used on the 8m Gemini-South Telescope, the 3.9m Anglo-Australian Telescope (AAT) and the 4.2m William Herschel Telescope (WHT). Its performance in both integral field mode and multi-object mode is discussed and some scientific highlights are presented. A multi-IFU system, which is currently under construction, is also described.

Select this Article		The second-generation VLT instrument MUSE: science drivers and instrument design Roland Bacon, Svend-Marian Bauer, Richard Bower, Sylvie Cabrit, Michele Cappellari, Marcella Carollo, Francoise Combes, Roger L. Davies, Bernard Delabre, Hans Dekker, Julien Devriendt, Slimane Djidel, Michel Duchateau, Jean-Pierre Dubois, Eric Emsellem, et al. Proc. SPIE 5492, 1145 (2004); http://dx.doi.org/10.1117/12.549009 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Abstract not available

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Infrared Spectroscopy II

Select this Article		LRS-J: instrument design and characterization Joseph R. Tufts, Gary J. Hill, Phillip J. MacQueen, and Marsha J. Wolf Proc. SPIE 5492, 1150 (2004); http://dx.doi.org/10.1117/12.552212 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract LRS-J is a 142 mm f / 1 near infrared (J-Band) camera designed as a drop in replacement for the optical camera installed on the Hobby--Eberly Telescope (HET) multi-object low resolution spectrograph (LRS). The Hawaii-1RG (H1RG) based instrument is liquid nitrogen cooled, but it mates to the warm LRS making use of the existing longslit and multi-object (MOS) units as well as the existing optical collimator. LRS-J utilizes a molecular beam epitaxy (MBE) based Hawaii-1RG (H1RG) detector. The design is a fully cryogenic catadioptric Maksutov-type, with the detector at the internal focus. This configuration produces excellent images, but presents particular challenges in the mounting of the detector. This is the first time that such an arrangement has been used in an astronomical instrument with an infrared detector. By replacing the conventional optical grisms with two 170 mm diameter near-IR VPH grisms, LRS-J covers the 0.9-1.3 μm bandpass with R ~ 1750-2000. We present the opto-mechanical design of LRS-J including the thermally self-compensating corrector doublet mount, and 100 μm/turn cryogenic mirror adjusters, FEA optimized vacuum housing, and custom Dewar. We also characterize the electrical and thermal connections necessary to mount the detector head in this unusually small inverted arrangement.

Select this Article		The commissioning of and first results from the UIST imager spectrometer Suzanne K. Ramsay Howat, Stephen Todd, Sandy Leggett, Chris Davis, Mel Strachan, Alastair Borrowman, Maureen Ellis, Jim Elliot, David Gostick, Russell Kackley, and Matthew Rippa Proc. SPIE 5492, 1160 (2004); http://dx.doi.org/10.1117/12.551673 \| Cited 11 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract UIST is a facility class near-infrared instrument recently commissioned at the UK Infrared Telescope (UKIRT). UIST provides a comprehensive imaging and spectroscopic facility with spatial resolution limited only by the delivered tip-tilt corrected seeing. In addition to long slit spectroscopic modes, UIST includes the first deployable cryogenic integral field unit in a common user instrument. We will present results obtained during the commissioning period in late 2002. These include measurements of the image quality and the sensitivities of the different observing modes of the instrument. We also discuss the use of an instrument-specific telescope pointing-model developed for UIST to allow the instrument to meet the stringent flexure requirements arising from the choice of 0.06arcsec/pixel and 0.12arcsec/pixel plate scales. We pay particular attention to the performance of the image slicing integral field unit (IFU). We will present astronomical results from the first year of UIST operations, during which time UIST carried out diverse programmes, from mineralogical studies of Mars to measuring the mass of the black hole at the centre of the most distant quasar.

Select this Article		Near infrared cryogenic tunable solid Fabry-Perot spectrometer Alexander S. Kutyrev, Charles L. Bennett, S. Harvey Moseley, David Rapchun, and Kenneth P. Stewart Proc. SPIE 5492, 1172 (2004); http://dx.doi.org/10.1117/12.551911 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We have developed a high resolution near-infrared temperature tunable cryogenic spectrometer with solid Fabry-Perot etalons. It is designed and built for diffuse emission of ionized hydrogen Brackett-gamma line studies, although with the appropriate pre-filter it can be configured for any near infrared lines. The etalons made from silicon and germanium operate near 77K. The high refractive index of these etalons allows for the construction of a very compact spectrometer. Germanium etalon with 20mm clear aperture is equivalent to a gas spaced Fabry-Perot interferometer of about 80 mm in diameter. A strong temperature dependence of the refractive index for these two materials makes it easy to tune etalons. Combination of these factors allowed to build a compact, high resolution (R=12000) high throughput instrument.

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Infrared Spectroscopy III

Select this Article		KMOS: an infrared multiple-object integral field spectrograph for the ESO VLT Ray M. Sharples, Ralf Bender, Matthew D. Lehnert, Suzanne K. Ramsay Howat, M. N. Bremer, Roger L. Davies, Reinhard Genzel, Reiner Hofmann, Rob J. Ivison, R. Saglia, and Niranjan A. Thatte Proc. SPIE 5492, 1179 (2004); http://dx.doi.org/10.1117/12.550495 \| Cited 6 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We describe the design of a 2nd generation instrument for the ESO VLT which will deliver a unique multiple deployable integral field capability in the near-infrared (1-2.5μm). The science drivers for the instrument are presented and linked to the functional specification. The baseline instrument concept is described with emphasis on technological innovations. Detailed discussions of specific technologies, and ongoing prototype studies, are described in separate papers.

Select this Article		EMIR: the GTC NIR multi-object imager-spectrograph Francisco Garzon, David Abreu, Sonia Barrera, Santiago Correa, Jose J. Diaz, Ana B. Fragoso, F. J. Fuentes, Fernando Gago, Carlos Gonzalez, Pablo Lopez, Antonio Manescau, Jesus Patron, Jaime Perez, Pablo Redondo, Rene Restrepo, et al. Proc. SPIE 5492, 1187 (2004); http://dx.doi.org/10.1117/12.550961 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present the final global design and performances of EMIR, the NIR multi-object spectrograph of the GTC, as well as the plan for its early scientific exploitation. EMIR, currently in the middle of its final phase, will be one of the first common user instruments for the GTC, the 10 meter telescope under construction by GRANTECAN at the Roque de los Muchachos Observatory (Canary Islands, Spain). EMIR is being built by a Consortium of Spanish and French institutes led by the IAC. EMIR is designed to realize one of the central goals of 10m class telescopes, allowing observers to obtain spectra for large numbers of faint sources in an time-efficient manner. EMIR is primarily designed to be operated as a MOS in the K band, but offers a wide range of observing modes, which include imaging and spectroscopy, both long slit and multi-object, in the wavelength range 0.9 to 2.5 mm. It is equipped with two innovative subsystems: a robotic reconfigurable multi-slit mask and dispersive elements formed by the combination of high quality diffraction grating and conventional prisms, both at the heart of the instrument. The present status of development, expected performances, schedule and plans for scientific exploitation are described and discussed. This project is mostly funded by GRANTECAN and the Plan Nacional de Astronomia y Astrofisica (National Plan for Astronomy and Astrophysics, Spain).

Select this Article		FLAMINGOS-2: the facility near-infrared wide-field imager and multi-object spectrograph for Gemini Stephen S. Eikenberry, Richard Elston, S. Nicholas Raines, Jeff Julian, Richard J. Corley, Kevin Hanna, David Hon, Roger Julian, David Rashkin, Brian Leckie, W. Rusty Gardhouse, Murray Fletcher, Jennifer Dunn, and Robert Wooff Proc. SPIE 5492, 1196 (2004); http://dx.doi.org/10.1117/12.549796 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We report on the design and status of the FLAMINGOS-2 instrument - a fully-cryogenic facility near-infrared imager and multi-object spectrograph for the Gemini 8-meter telescopes. FLAMINGOS-2 has a refractive all-spherical optical system providing 0.18-arcsecond pixels and a 6.2-arcminute circular field-of-view on a 2048x2048-pixel HAWAII-2 0.9-2.4 mm detector array. A slit/Dekker wheel mechanism allows the selection of up to 9 multi-object laser-machined plates or 3 long slits for spectroscopy over a 6x2-arcminute field of view, and selectable grisms provide resolutions from ~1300 to ~3000 over the entire spectrograph bandpass. FLAMINGOS-2 is also compatible with the Gemini Multi-Conjugate Adaptive Optics system, providing multi-object spectroscopic capabilities over a 3x1-arcminute field with high spatial resolution (0.09-arcsec/pixel). We review the designs of optical, mechanical, electronics, software, and On-Instrument WaveFront Sensor subsystems. We also present the current status of the project, midway through its construction phase in June 2004.

Select this Article		LUCIFER status report, summer 2004 Holger Mandel, Immo Appenzeller, Walter Seifert, Harald Baumeister, Peter Bizenberger, Ralf-Juergen Dettmar, Hans Gemperlein, Bernhard Grimm, Tom M. Herbst, Reiner Hofmann, Marcus Jutte, Werner Laun, Michael Lehmitz, Sebastiano Ligori, Rainer Lenzen, et al. Proc. SPIE 5492, 1208 (2004); http://dx.doi.org/10.1117/12.551302 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract LUCIFER (LBT NIR Spectrograph Utility with Camera and Integral-FieldUnit for Extragalactic Research) is a NIR spectrograph and imager forthe LBT (Large Binocular Telescope) working in the wavelength range from 0.9 to 2.5 microns. The instrument is to be built by a consortium of five german institutes (Landessternwarte Heidelberg (LSW), Max Planck Institut for Astronomy (MPIA), Max Planck Institut for Extraterrestric Physics (MPE), Astronomical Institut of the Ruhr-University Bochum (AIRUB) and Fachhochschule for Technics and Design Mannheim (FHTG)). LUCIFER will be one of the first light instruments of the LBT and will be available to the community at the end of 2005. A copy of the instrument for the second LBT mirror follows about one year later. The paper presents a brief status report of the procured and builthardware, of the workpackages already carried out and summarizes the ongoing work in progress.

Select this Article		CRIRES: a high-resolution infrared spectrograph for ESO's VLT Hans-Ulrich Kaeufl, Pascal Ballester, Peter Biereichel, Bernard Delabre, Rob Donaldson, Reinhold Dorn, Enrico Fedrigo, Gert Finger, Gerhard Fischer, Francis Franza, Domingo Gojak, Gotthard Huster, Yves Jung, Jean-Louis Lizon, Leander Mehrgan, et al. Proc. SPIE 5492, 1218 (2004); http://dx.doi.org/10.1117/12.551480 \| Cited 14 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract CRIRES is a cryogenic, pre-dispersed, infrared echelle spectrograph designed to provide a resolving power lambda/(Delta lambda) of 10⁵ between 1 and 5mu m at the Nasmyth focus B of the 8m VLT unit telescope #1 (Antu). A curvature sensing adaptive optics system feed is used to minimize slit losses and to provide diffraction limited spatial resolution along the slit. A mosaic of 4 Aladdin~III InSb-arrays packaged on custom-fabricated ceramics boards has been developed. This provides for an effective 4096x512 pixel focal plane array, to maximize the free spectral range covered in each exposure. Insertion of gas cells to measure high precision radial velocities is foreseen. For measurement of circular polarization a Fresnel rhomb in combination with a Wollaston prism for magnetic Doppler imaging is foreseen. The implementation of full spectropolarimetry is under study. This is one result of a scientific workshop held at ESO in late 2003 to refine the science-case of CRIRES. Installation at the VLT is scheduled during the first half of 2005. Here we briefly recall the major design features of CRIRES and describe its current development status including a report of laboratory testing.

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Poster Presentations: Infrared Instrumentation

Select this Article		Echidna: the engineering challenges Jurek K. Brzeski, Peter Gillingham, David Correll, John Dawson, Anna M. Moore, Rolf Muller, Scott Smedley, and Greg A. Smith Proc. SPIE 5492, 1228 (2004); http://dx.doi.org/10.1117/12.550963 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Anglo-Australian Observatory's (AAO's) FMOS-Echidna project is for the Fiber Multi-Object Spectroscopy system for the Subaru Telescope. It includes three parts: the 400-fiber positioning system, the focal plane imager (FPI) and the prime focus corrector. The Echidna positioner concept and the role of the AAO in the FMOS project have been described in previous SPIE proceedings. The many components for the system are now being manufactured, after prototype tests have demonstrated that the required performance will be achieved. In this paper, the techniques developed to overcome key mechanical and electronic engineering challenges for the positioner and the FPI are described. The major performance requirement is that all 400 science fiber cores and up to 14 guide fiber bundles are to be re-positioned to an accuracy of 10μm within 10 minutes. With the fast prime focus focal ratio, a close tolerance on the axial position of the fiber tips must also be held so efficiency does not suffer from de-focus. Positioning accuracy is controlled with the help of the FPI, which measures the positions of the fiber tips to an accuracy of a few μm and allows iterative positioning. Maintaining fiber tips sufficiently co-planar requires accurate control in the assembly of the several components that contribute to such errors. Assembly jigs have been developed and proven adequate for this purpose. Attaining high reliability in an assembly with many small components of disparate materials bonded together, including piezo ceramics, carbon fiber reinforced plastic, hardened steel, and electrical circuit boards, has entailed careful selection and application of cements and tightly controlled soldering for electrical connections.

Select this Article		The cryogenic MOS unit for LUCIFER Reiner Hofmann, Hans Gemperlein, Bernhard Grimm, Marcus Jutte, Holger Mandel, Kai Polsterer, and Harald Weisz Proc. SPIE 5492, 1243 (2004); http://dx.doi.org/10.1117/12.551137 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The LUCIFER MOS unit has been designed to exchange long-slit and multi-slit masks between two mask storage cabinets and the focal plane area. In combination with auxiliary cryostats, the MOS unit also permits the exchange of cold mask cabinets between LUCIFER and the auxiliary cryostats. Main functional components of the MOS unit are: a focal plane interface accepting the active mask, a mask handling unit transporting the masks between the focal plane mount and their storage locations, a stationary and an exchangeable cabinet holding 10 longslit and 23 multi-slit masks respectively, the translation drives for the exchangeable cabinet and the mask handling unit, and the mask locking unit securing the masks in their cabinets. For mask cabinet exchange, the LUCIFER cryostat as well as the auxiliary cryostats are equipped with 32 cm clear diameter gate valves. A test cryostat has been built to test all MOS unit functions at LN2 temperature. Most of the MOS unit components have been completed. System tests at ambient have started. First results are presented.

Select this Article		Design, fabrication, assembly, and testing of the Florida image slicer for infrared cosmology and astrophysics (FISICA) integral field unit Paul E. Glenn, C. Gregory Hull-Allen, Jeff Hoffman, Michael Rodgers, Kevin Thompson, Bruce Myrick, Lovell Comstock, Scott Flint, Glenn Boreman, Stephen S. Eikenberry, Richard Elston, Rafael Guzman, Jeff Julian, and S. Nicholas Raines Proc. SPIE 5492, 1254 (2004); http://dx.doi.org/10.1117/12.551661 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We discuss the design, fabrication, assembly, and testing of the prototype Florida Image Slicer for Infrared Cosmology and Astrophysics (FISICA) Integral Field Unit (IFU). FISICA is intended for large telescopes with f/numbers close to f/15, such as the KPNO 4-m and GTC 10.4-m telescopes. It implements an image slicing approach, wherein the initial image plane is optically sliced into thin strips and the strips are optically rearranged end-to-end, whereupon the composite slit image is fed into a conventional spectrograph. We divide the field of view into 22 slices, while accommodating the entire f/15 viewing solid angle. The all-reflective instrument resides in a cryogenic dewar at the initial focal plane, and places the composite slit image output precisely at the initial focus, allowing it to interface to the existing FLAMINGOS spectrograph. The mirrors were diamond turned using various tool geometries and state-of-the-art, multi-axis tool control. The mirrors are made from a single billet of aluminum, and the optical bench and mounts are made of the same alloy as the mirrors for optimum performance during cryogenic cooling. We discuss the key design efforts, emphasizing tradeoffs among performance, volume, fabrication difficulty, and alignment requirements. We describe the fabrication, and present preliminary laboratory test results.

Select this Article		FISICA: the Florida image slicer for infrared cosmology and astrophysics Stephen S. Eikenberry, Richard Elston, Rafael Guzman, Jeff Julian, S. Nicholas Raines, Nicolas Gruel, Glenn Boreman, Paul E. Glenn, C. Gregory Hull-Allen, Jeff Hoffman, Michael Rodgers, Kevin Thompson, Scott Flint, Lovell Comstock, and Bruce Myrick Proc. SPIE 5492, 1264 (2004); http://dx.doi.org/10.1117/12.549150 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We report on the design and status of the Florida Image Slicer for Infrared Cosmology and Astrophysics (FISICA) - a fully-cryogenic all-reflective image-slicing integral field unit for the FLAMINGOS near-infrared spectrograph. Designed to accept input beams near f/15, FISICA with FLAMINGOS provides R~1300 spectra over a 16x33-arcsec field-of-view on the Cassegrain f/15 focus of the KPNO 4-meter telescope, or a 6x12-arcsec field-of-view on the Nasmyth or Bent Cassegrain foci of the Gran Telescopio Canarias 10.4-meter telescope. FISICA accomplishes this using three sets of "monolithic" powered mirror arrays, each with 22 mirrored surfaces cut into a single piece of aluminum. We review the optical and opto-mechanical design and fabrication of FISICA, as well as laboratory test results for FISICA integrated with the FLAMINGOS instrument. We also discuss plans for first-light observations on the KPNO 4-meter telescope in July 2004.

Select this Article		GIANO: an ultrastable IR echelle spectrometer optimized for high-precision radial velocity measurements and for high-throughput low-resolution spectroscopy Ernesto Oliva, Livia Origlia, Roberto Maiolino, Sandro Gennari, Valdemaro Biliotti, Emanuel Rossetti, Carlo Baffa, F. Leone, Paolo Montegriffo, Marco Lolli, Francesco D'Amato, Pietro Bruno, Salvatore Scuderi, Francesca Ghinassi, Manuel Gonzalez, et al. Proc. SPIE 5492, 1274 (2004); http://dx.doi.org/10.1117/12.550050 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract GIANO is an infrared (0.9-2.5 μm) cross-dispersed echelle spectrometer designed to achieve high throughput, high resolving power, wide band coverage and high accuracy radial velocity measurements. It also includes polarimetric capabilities and a low resolution mode that make it a very versatile, common user instrument which will be permanently mounted and available at one of the Nasmyth foci of the Telescopio Nazionale Galileo (TNG) located at Roque de Los Muchachos Observatory (ORM), La Palma, Spain. GIANO was selected by INAF as the top priority instrument among those proposed within the Second Generation Instrumentation Plan of the TNG. More information on this project can be found at the web page http://www.bo.astro.it/giano

Select this Article		EMIR electronics and mechanism control Fernando Gago, Jose J. Diaz, Pablo Redondo, Carlos Gonzalez, Francis Beigbeder, Yvan Chapon, Francisco Garzon, and Jesus Patron Proc. SPIE 5492, 1280 (2004); http://dx.doi.org/10.1117/12.550506 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract EMIR is a multiobject intermediate resolution near infrared (1.0-2.5 microns) spectrograph with image capabilities to be mounted on the 10m Gran Telescopio de Canarias (GTC), located on the Spanish island of La Palma. This paper shows an overview of the EMIR electronics and mechanism control. First, a description of the detector (a Hawaii-2 array) electronics is given, which involves the use of commercial components (resistors, capacitors and operational amplifiers) working under cryogenic conditions (around 77K). This paper describes the particularities of the cold electronics, showing the problems found and the way to solve them. Preliminary results of the detector characterization are also presented in this paper.Secondly, an overview of the different mechanisms of the instrument is presented. They are cryogenic mechanisms with pretty stringent positioning requirements. The technological solutions used to meet the tight control requirements will be described.

Select this Article		A new wide-field spectrograph Eamonn Ansbro Proc. SPIE 5492, 1290 (2004); http://dx.doi.org/10.1117/12.550887 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A spectrograph was designed and constructed to provide a new capability for measuring spectrum of extended emission line sources, but it has the versatility to work well on stellar bright moving sources for example emission nebulae and comets.The spectrograph uses high-speed lens system. It projects the incoming wide field light through a horizontal moving slit assembly onto a reflective grating based on a rotary platform that is synchronised with the slit mechanism. The slit width is adjustable, as is the case in conventional spectrographs.An important part of the design is the lateral movement of the entire slit assembly (in addition to the movement of the slit itself), so that the narrow beam passing through the slit will reflect off different parts of the diffraction grating and be received by the camera in a scanning mode. As a result, this single device can cover a wide field of view across the range of spectra in a short duration of time. In fact it can obtain a spectrum of sky 3 x 3 degrees in a short timescale depending on the quantum efficiency and format size of the CCD detector.

Select this Article		Mass producing an efficient NIR spectrograph John C. Wilson, Charles P. Henderson, Terry L. Herter, Keith Matthews, Michael F. Skrutskie, Joseph D. Adams, Dae-Sik Moon, Roger Smith, Nick Gautier, Michael Ressler, B. T. Soifer, Sean Lin, James Howard, John LaMarr, Todd M. Stolberg, et al. Proc. SPIE 5492, 1295 (2004); http://dx.doi.org/10.1117/12.550925 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Four institutions are collaborating to design and build three near identical R ~2700 cross-dispersed near-infrared spectrographs for use on various 5-10 meter telescopes. The instrument design addresses the common observatory need for efficient, reliable near-infrared spectrographs through such features as broad wavelength coverage across 6 simultaneous orders (0.8 - 2.4 microns) in echelle format, real-time slit viewing through separate optics and detector, and minimal moving parts. Lastly, the collaborators are saving money and increasing the likelihood of success through economies of scale and sharing intellectual capital.

Select this Article		MMT and Magellan infrared spectrograph Brian A. McLeod, Daniel Fabricant, John Geary, Paul Martini, George Nystrom, Richard Elston, Stephen S. Eikenberry, and Harland Epps Proc. SPIE 5492, 1306 (2004); http://dx.doi.org/10.1117/12.551049 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present the preliminary design for the MMT and Magellan InfraredSpectrograph (MMIRS). MMIRS is a fully refractive imager and multi-object spectrograph that uses a 2048x2048 pixel Hawaii2 HgCdTe array. It offers a 7'x7' imaging field of view and a 4'x7' field of view for multi-object spectroscopy. Dispersion is provided by a set of 5 grisms providing R=3000 at J, H, or K, or R=1300 in J+H or H+K.

Select this Article		The fiber multi-object spectrograph (FMOS) for the Subaru Telescope III Shigeru Eto, Toshinori Maihara, Kouji Ohta, Fumihide Iwamuro, Masahiko Kimura, Daisaku Mochida, Shinpei Wada, Satoko Imai, Yusuke Narita, Yu Nakajima, Hiroshi Karoji, Jun'ichi Noumaru, Masayuki Akiyama, Peter Gillingham, Scott Smedley, et al. Proc. SPIE 5492, 1314 (2004); http://dx.doi.org/10.1117/12.551087 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Fibre Multi-Object Spectrograph (FMOS) for the primary focusof Subaru Telescope is one of the second generationinstruments, aiming at acquiring spectra of faint objects withtarget multiplicity of up to 400. The optimised wavelengths spanfrom 0.9 to 1.8 microns so as to extend our knowledge of galaxyformations and evolutions at higher redshifts in a systematic way,as well as of variety of intriguing near-infrared objects.On the basis of detailed design of FMOS, actual processes offabrication are in progress, and some of critical hardwarecomponents have successfully been developed. In this report,we present the status of the FMOS project, the results ofdeveloped components, and also instrument control systems suchas the new detector electronics as well the related contolsoftwares.

Select this Article		EMIR mechanical design status F. J. Fuentes, Vicente Sanchez, Sonia Barrera, Santiago Correa, Jaime Perez, Pablo Redondo, Rene Restrepo, Fabio Tenegi, Alejandro Villegas, Jesus Patron, and Francisco Garzon Proc. SPIE 5492, 1319 (2004); http://dx.doi.org/10.1117/12.551122 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract EMIR is the NIR multi-object imager and spectrograph for the GTC (Gran Telescopio Canarias). The instrument PDR phase was held successfully in March 2003, and we are at present in the middle of the ADR (Advanced Design Phase) during which a number of mechanical concepts will be tested on development prototypes to ensure the feasibility of the PDR proposed design. This presentation contains a technical description of the mechanical design of the instrument, as well as the prototypes development. The mechanical design is essentially built around the optical layout by providing an optical bench for mounting the optomechanics, the mechanisms and the detector, all this inside a custom-designed vacuum vessel and with the corresponding cooling system. One of its main design features is the use of a cryogenic reconfigurable slit mechanism to generate a multi-slit configuration, a long slit or an imaging aperture at the telescope focal plane. This feature will permit to maintain the instrument in operation conditions for a long time and take advantages in both a classically scheduled and a queued service observing schemes

Select this Article		Structural and thermal analysis of EMIR Santiago Correa, Rene Restrepo, Fabio Tenegi, F. J. Fuentes, Vicente Sanchez, Sonia Barrera, Jaime Perez, Pablo Redondo, Alejandro Villegas, Francisco Garzon, and Jesus Patron Proc. SPIE 5492, 1331 (2004); http://dx.doi.org/10.1117/12.551255 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract This paper shows the different design concepts and techniques employed in the structural and thermal analysis of EMIR (Espectrografo Multiobjeto Infrarrojo), nowadays under development at the Instituto de Astrofisica de Canarias.

Select this Article		LUCIFER: status and results of the hardware testing Walter Seifert, Werner Laun, Michael Lehmitz, Holger Mandel, Andreas Schuetze, and Andreas Seltmann Proc. SPIE 5492, 1343 (2004); http://dx.doi.org/10.1117/12.551288 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract LUCIFER (LBT NIR-Spectroscopic Utility with Camera and Integral-Field Unit for Extragalactic Research) is a NIR spectrograph and imager (wavelength range 0.9 to 2.5 micron) for the Large Binocular Telescope (LBT) on Mt. Graham, Arizona. It is built by a consortium of five German institutes and will be one of the first light instruments for the LBT. Later, a second copy for the second mirror of the telescope will follow. Both instruments will be mounted at the bent Gregorian foci of the two individual telescope mirrors. The instrument is equipped with three exchangeable cameras for imaging and spectroscopy: two of them are optimized for seeing-limited conditions, the third camera for the diffraction-limited case with the LBT adaptive secondary mirror working. The spectral resolution will allow for OH suppression. Up to 33 exchangeable masks will be available for longslit and multi-object spectroscopy (MOS) over the full field of view (FOV). The detector will be a Rockwell HAWAII-2 HgCdTe-array. Extensive tests were done for all the electro-mechanical functions. Those include the grating selection and the grating tilt unit and the drive for the fold mirror to compensate for image movement due to flexure. Furthermore several optical and opto-mechanical units were tested. The procedures and results of the tests are presented in detail and compared with the specifications.

Select this Article		CHEOPS NIR IFS: exploring stars neighborhood spectroscopically Riccardo U. Claudi, Massimo Turatto, Raffaele Gratton, Jacopo Antichi, Silvio Buson, Claudio Pernechele, Silvano Desidera, Andrea Baruffolo, Jorge Lima, Juan Alcal, Enrico Cascone, Gainpaolo Piotto, Sergio Ortolani, Hans Martin Schmid, Markus Feldt, et al. Proc. SPIE 5492, 1351 (2004); http://dx.doi.org/10.1117/12.551427 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract CHEOPS is a 2^nd generation VLT instrument for the direct detection of extrasolar planets. The project is currently in its Phase A. It consists of an high order adaptive optics system which provides the necessary Strehl ratio for the differential polarimetric imager (ZIMPOL) and an Integral Field Spectrograph (IFS). The IFS is a very low resolution spectrograph (R~15) which works in the near IR (0.95-1.7 μm), an ideal wavelength range for the ground based detection of planetary features. In our baseline design, the Integral Field Unit (IFU) is a microlens array of about 250x250 elements which will cover a field of view of about 3.5x3.5 arcsecs² in proximity of the target star. In this paper we describe the instrument, its preliminary optical design and the basic requirements about detectors. In a separate contribution to this conference, we present the very low resolution disperser.

Select this Article		The current status of the UK-FMOS spectrograph Ian A. Tosh, Guy F. Woodhouse, Tim Froud, Allan Dowell, Mukesh Patel, Mattias Wallner, Ian J. Lewis, Gavin B. Dalton, Alan Holmes, Barney Brooks, Cyril Band, David G. Bonfield, Graham J. Murray, David J. Robertson, and Nigel A. Dipper Proc. SPIE 5492, 1362 (2004); http://dx.doi.org/10.1117/12.551454 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract FMOS is a near-IR OH-suppressed multi-fibre fed spectrograph for the Subaru telescope. The spectrograph will accept 200 optical fibres from the ECHIDNA positioner system at the 30arcmin Prime focus of the telescope. We will describe the recent activities here in the UK in progressing the instrument from its conceptual phase through detailed design and into manufacture. A variety of technical areas will be described including: the opto-mechanical system design and construction, development of the HAWAII-II detector control system, the thermal system design & control and OH suppression techniques.

Select this Article		A prototype cryogenic pick-off arm for multi-IFU spectrometers Suzanne K. Ramsay Howat, David J. Robertson, Andrew Haslehurst, Juergen Schmoll, Philip Parr Burman, Ray M. Sharples, Colin Dickson, Peter Hastings, David Lee, Peter Luke, Paul McMahon, Nigel Phillips, Martyn Wells, Colin Cunnigham, Nigel A. Dipper, et al. Proc. SPIE 5492, 1371 (2004); http://dx.doi.org/10.1117/12.551545 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A prototype cryogenic 'pick-off' arm for selecting a small field from the focal plane of a large telescope has been built and tested against a set of scientific requirements representative of those for proposed multi-integral-field spectrographs. In this paper, we present the design of the arm and the results of the cryogenic testing. Since the proposed instruments will require tens of arms, perhaps hundreds, we have also considered the industrialisation of the manufacture and assembly of the arms. We briefly discuss this aspect of the design and the possibilities for future instrumentation on Extremely Large Telescopes.

Select this Article		An ultraprecision fiber connector for FMOS Graham J. Murray, George N. Dodsworth, Robert Content, Naoyuki Tamura, David J. Robertson, Daniel Gedge, and Barney Brooks Proc. SPIE 5492, 1383 (2004); http://dx.doi.org/10.1117/12.551559 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A fibre-fed near IR (J & H band) multi-object spectrograph (FMOS) is being constructed by a consortium of UK, Australian and Japanese groups for the SUBARU telescope on Mauna Kea, Hawaii. The prime focus of the telescope will support ECHIDNA, a 400-fibre multi-object positioning system. However, the IR spectrographs are located close to the Nasmyth platform, so an optical feed is required to deliver light from ECHIDNA to the spectrographs. The Astronomical Instrumentation Group at the University of Durham is undertaking the design and construction of a suitable fibre-optic downlink. To allow the prime focus unit that houses ECHIDNA to be removed, the fibre cabling is to include a connectorised break. The optical design of the fibre system also calls for a change in focal ratio from that delivered by ECHIDNA in order to couple light to the spectrographs with the greatest efficiency. This will be achieved in a custom designed connector head by means of a tailored lens array. The connector design will in addition incorporate a back-illumination system for fibre position determination at the prime focus. This paper describes the overall design of the connector that is to be employed. The modularity of the scheme and various innovative features are highlighted. A more advanced connector concept capable of dual bandwidth (visible & NIR) operation is also shown. Such a system could significantly enhance the science return from future ECHIDNA-type fibre instruments.

Select this Article		Design study for the KMOS spectrograph module Matthias Tecza, Niranjan A. Thatte, Ian J. Lewis, James Lynn, Wing Lau, Stephanie Yang, Ian A. Tosh, and Martyn Wells Proc. SPIE 5492, 1395 (2004); http://dx.doi.org/10.1117/12.552235 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present the results of a design study for the spectrograph module for KMOS - a cryogenic near-infrared multi-object spectrograph being developed as a second generation instrument for the VLT by a consortium of UK and German institutes. KMOS will consist of 24 deployable integral field units feeding three identical spectrograph units via image slicers. The spectrographs are designed to provide a resolving power greater than 3000, so as to provide adequate OH avoidance, whilst covering one of the J, H or K bands within a single exposure. We present the opto-mechanical layout of the spectrographs, together with an analysis of the impact of the image quality (and PSF uniformity) on the accuracy of sky background subtraction within each IFU's field of view.

Select this Article		Data reduction pipeline for OSIRIS, the new NIR diffraction-limited imaging field spectrograph for the Keck adaptive optics system Alfred Krabbe, Tom Gasaway, Inseok Song, Christof Iserlohe, Jason Weiss, James E. Larkin, Matthew Barczys, and David Lafreniere Proc. SPIE 5492, 1403 (2004); http://dx.doi.org/10.1117/12.552592 \| Cited 7 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract OSIRIS is a near infrared diffraction limited imaging field spectrograph under development for the Keck observatory adaptive optics system and scheduled for commissioning in fall 2004. Based upon lenslet pupil imaging, diffraction grating, and a 2Kx2K Hawaii2 HgCdTe array, OSIRIS is a highly efficient instrument at the forefront of today's technology. OSIRIS will deliver per readout up to 4096 diffraction limited spectra in a complex interleaved format, requiring new challenges to be met regarding user interaction and data reduction. A data reduction software package is under development, aiming to provide the observer with a facility instrument allowing him to concentrate on science rather than dealing with instrumental as well as telescope and atmosphere related effects. Together with OSIRIS, a pipeline for basic data reduction will be provided for a new Keck instrument for the first time. A status report is presented here together with some aspects of the data reduction pipeline.

Select this Article		A high-efficiency near-infrared spectrograph for the Apache Point 3.5 m telescope Alan Uomoto, Stephen A. Smee, and Robert H. Barkhouser Proc. SPIE 5492, 1411 (2004); http://dx.doi.org/10.1117/12.552841 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A point-source spectrograph under development for the APO 3.5 m telescope offers resolving powers (R = λ/Δλ) of 1000 and 4000 in the near-IR (0.85-2.5 μm) while using wide slits matched to the seeing disk. The use of diamond-turned aluminum and crystal optics in a straightforward optical path coupled with a Hawaii-1RG detector provides excellent end-to-end efficiency of 32%-39% (including the telescope optics). Designed primarily for follow-up studies of brown dwarf and high redshift quasar candidates identified by wide-field surveys such as SDSS and 2MASS, this instrument will afford the 3.5 m telescope superb capability for a wide variety of science programs. In this paper we present the goals and design of the spectrograph and its expected performance.

Select this Article		AMBER instrument control software Etienne P. leCoarer, Gerard Zins, Laurence Gluck, Gilles Duvert, Thomas Driebe, Keiichi Ohnaka, Matthias Heininger, Claus Connot, Jan Behrend, Michel Dugue, Jean Michel Clausse, and Florentin Millour Proc. SPIE 5492, 1423 (2004); http://dx.doi.org/10.1117/12.551301 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract AMBER (Astronomical Multiple BEam Recombiner) is a 3 aperture interferometric recombiner operating between 1 and 2.5 um, for the Very Large Telescope Interferometer (VLTI). The control software of the instrument, based on the VLT Common Software, has been written to comply with specific features of the AMBER hardware, such as the Infrared detector read out modes or piezo stage drivers, as well as with the very specific operation modes of an interferomtric instrument.In this respect, the AMBER control software was designed to insure that all operations, from the preparation of the observations to the control/command of the instrument during the observations, would be kept as simple as possible for the users and operators, opening the use of an interferometric instrument to the largest community of astronomers. Peculiar attention was given to internal checks and calibration procedures both to evaluate data quality in real time, and improve the successes of long term UV plane coverage observations.

Select this Article		Very low resolution disperser of CHEOPS NIR integral field spectrograph Riccardo U. Claudi, Silvio Buson, Silvano Desidera, Massimo Turatto, Raffaele Gratton, and Jacopo Antichi Proc. SPIE 5492, 1431 (2004); http://dx.doi.org/10.1117/12.552566 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Integral Field Spectrograph (IFS) of CHEOPS, the 2^nd generation VLT instrument for planet finding, will attain a very low resolution (R=15) in order to search for cold (and warm) planets in stellar neighbourhood. This will allow to exploit wide band integral field spectroscopy to perform differential photometry. The complete description of CHEOPS IFS is given as a separate contribution to this conference; in this paper the analysis and the project of the very low disperser are outlined.

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Poster Presentations: Infrared, Solar and ELT Instrumentation

Select this Article		Design study for the WIYN high-resolution infrared camera Margaret Meixner, Patricia Knezek, Edward Churchwell, Ryan Doering, Remy Indebetouw, Donald Figer, John W. MacKenty, Andrew Fruchter, Robert H. Barkhouser, and Stephen A. Smee Proc. SPIE 5492, 1440 (2004); http://dx.doi.org/10.1117/12.550868 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present the science case, design overview and sensitivity estimate for the design study for the WIYN High Resolution Infrared Camera (WHIRC). The WIYN telescope is an active 3.5 m telescope located at an excellent seeing site on Kitt Peak and operated by University of Wisconsin, Indiana University, Yale University and National Optical Astronomical Observatory (NOAO). As a dedicated near-infrared (0.8-2.5 micron) camera on the WIYN Tip-Tilt Module (WTTM), WHIRC will provide near diffraction limited imaging, i.e. FWHM~0.25" typically and 0.12" on exceptional nights. The optical design goal is to use a 2048x2048 HgCdTe array with a plate scale of 0.09" per pixel, resulting in a field of view (FOV), 3'x3', which is a compromise between the highest angular resolution achievable and the largest FOV correctable by WTTM. WHIRC will be used for high definition near-infrared imaging studies such as star formation, proto-planetary disks, galactic dust enshrouded B clusters, dust enshrouded stellar populations in nearby galaxies, and supernova and gamma-ray burst searches.

Select this Article		A 350-μm array polarimeter using translational modulators David T. Chuss, Dominic J. Benford, Chris Walker, S. Harvey Moseley, Giles Novak, Johannes G. Staguhn, and Edward J. Wollack Proc. SPIE 5492, 1450 (2004); http://dx.doi.org/10.1117/12.551382 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We describe a polarimeter that will be a testbed for a novel polarization modulator. This modulator is composed of two modified Martin-Puplett interferometers in which the input polarization state is transformed by adjusting the phase delays between linear orthogonal polarizations in each of the two stages. This type ofmodulator represents a potential improvement over existing technology in the following three ways. First, these modulators can fully characterize the polarization state by measuring Stokes Q, U, and V. The characterization of V is especially useful as a diagnostic for systematic errors. Second, the Martin-Puplett modulators can be easily retuned to observe at multiple frequencies. Finally, the small translations required for modulation can be accomplished with fewer moving parts than the rotational motions in wave plate modulators, thus potentially leading to modulators with longer lifetimes than those currently employed in polarimeters. The next generation of polarimeters, designed for both the study of Galactic magnetic fields in the far-infrared and submillimeter and the measurement of the polarized component of the Cosmic Microwave Background, will need to incorporate modulators with these attributes.This prototype polarimeter will be a modified version of the Hertz polarimeter that had until recently been operating on the Caltech Submillimeter Observatory. After modification, Hertz will be moved to the Heinrich Hertz Telescope in Arizona. We will utilize dynamic scheduling to efficiently observe during the best fraction of weather at this site.

Select this Article		The LINC-NIRVANA cryogenic interferometric camera Peter Bizenberger, Dave Andersen, Harald Baumeister, Udo Beckmann, Emiliano Diolaiti, Tom M. Herbst, Werner Laun, Lars Mohr, Vianak Naranjo, and Christian Straubmeier Proc. SPIE 5492, 1461 (2004); http://dx.doi.org/10.1117/12.551400 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The LINC-NIRVANA instrument is a 1-2.5 micron Fizeau interferometric imager, which combines the light of the two 8.4 m mirrors of the Large Binocular Telescope on Mt. Graham in Arizona. The cryogenic camera forms the heart of the science channel of this instrument, delivering a 1 arcmin diameter field of view with 5 mas spatial resolution. The center 10x10 arcseconds, initially limited by the size of the 2048x2048 Hawaii-2 detector, are used for science observations. For simplicity, the camera has a fixed, F/32 optical path of the combined beams, leading to wavelength-dependent sampling. We describe the main components of the camera, as well as present the calculations of interferometric performance and the required opto-mechanical tolerances. We demonstrate that specially designed components can reach these specifications.

Select this Article		A prime focus camera for the Discovery Channel Telescope Edward W. Dunham and Thomas A. Sebring Proc. SPIE 5492, 1471 (2004); http://dx.doi.org/10.1117/12.552230 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Discovery Channel Telescope (DCT) is a 4.2 meter telescope that will provide a two degree diameter well-corrected field of view at prime focus with wavelength coverage across the groundbased ultraviolet and optical range. The design of the telescope and the prime focus corrector are described in other papers at this conference. The prime focus of the DCT will be occupied by a CCD camera similar in scope to the SAO Megacam for the MMT, the CFHT MegaCam, and the Kepler focal plane, but with differences in detail. It will be used for a variety of planetary science and astrophysics observing programs, the most demanding technically being searches for near-Earth and Kuiper Belt objects. This paper describes the design requirements, major systems issues, current design, and expected performance of the prime focus camera for the DCT.

Select this Article		CPAPIR: a wide-field infrared camera for the Observatoire du Mont Megantic Etienne Artigau, Rene Doyon, Philippe Vallee, Martin Riopel, and Daniel Nadeau Proc. SPIE 5492, 1479 (2004); http://dx.doi.org/10.1117/12.551920 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract CPAPIR is a wide-field infrared camera for use at the Observatoire du mont Megantic and CTIO 1.5 m telescopes. The camera will be primarily a survey instrument with a half-degree field of view, making it one of the most efficient of its kind. CPAPIR will provide broad and narrow band filters within its 0.8 to 2.5 μm bandpass. The camera is based on a Hawaii-2 2048x2048 HgCdTe detector.

Select this Article		A Martin-Puplett architecture for polarization modulation and calibration David T. Chuss, S. Harvey Moseley, Giles Novak, and Edward J. Wollack Proc. SPIE 5492, 1487 (2004); http://dx.doi.org/10.1117/12.552103 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We introduce an architecture for changing the polarization state of far-infrared through submillimeter radiation that employs two Martin-Puplett interferometers. One interferometer is oriented with its beam-splitting grid at an angle of 22.5 degrees with respect to the Stokes Q axis. The second is oriented with its beam-splitting grid at an angle of 45 degrees. By modulating one of the arms of each interferometer, it is possible to arbitrarily adjust the polarization state that a polarization-sensitive detector measures when placed at the output of the device. Because of this flexibility, one application of this device is as a calibrator for a polarimeter. In addition, it is conceivable to use such a device as a modulator for a far-infrared/submillimeter polarimeter. As such, this system has several advantages over a half-wave plate. First, the capability to measure circular polarization will provide the instrument with a novel method for checking systematic errors, as the circular polarization of most astronomical continuum sources is expected to be near zero. Second, such a device is easily adapted to work at different wavelengths, thus facilitating the construction of far-infrared and submillimeter polarimeters with multiple passbands. Finally, the small linear throws necessary for modulation eliminate the need for complicated systems of gears and low temperature bearings that are common in wave plate systems and often prone to failure. We present a Jones matrix analysis of this modulator architecture and compare the performance of this device with that of a half-wave plate.

Select this Article		Four years of good SpeX John T. Rayner, Peter M. Onaka, Michael C. Cushing, and William D. Vacca Proc. SPIE 5492, 1498 (2004); http://dx.doi.org/10.1117/12.551107 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract SpeX is a cross-dispersed medium-resolution 0.8-5.5 micron spectrograph in operation at the NASA Infrared Telescope Facility(IRTF) on Mauna Kea, Hawaii. The instrument uses prism cross-dispersers and gratings to provide resolving powers of up toR~2000 simultaneously across 0.8-2.4 micron or ~2-5.4 micron. An autonomous infrared slit-viewer is used for object acquisition,guiding, and scientific imaging. The spectrograph employs a 1024x1024 Aladdin 3 InSb array and the imager a 512x512 Aladdin 2 InSb array. Since it was commissioned in June 2000, SpeX has been used for about 45% of all telescope time. We give an overview of the design, followed by details of the use and performance of the Aladdin arrays,observing techniques, maintenance issues and lessons learned.

Select this Article		Mechanics of LIRIS (long-slit intermediate-resolution infrared spectrograph) at first commissioning Elvio Hernandez, Jose Acosta-Pulido, Emilio Cadavid, Santiago Correa, Lorenzo Peraza, Pablo Redondo, Vicente Sanchez, Fabio Tenegi, Arturo Manchado, and Mary Barreto Proc. SPIE 5492, 1510 (2004); http://dx.doi.org/10.1117/12.551286 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract LIRIS is a near-infrared intermediate resolution spectrograph with added capabilities for multi-slit, imaging, coronography, and polarimetry, developed by the Instituto de Astrofisica de Canarias (IAC). It will be a common user instrument for the Cassegrain focus of the William Herschel Telescope (WHT) at the Roque de los Muchachos Observatory in La Palma. At its first commissioning, that was held in February 2003, the functionality of the mechanisms (entrance wheel, central wheels and camera wheel) under variable orientation of the telescope was verified, and no thermal nor structural problems arose. The functionality of the mechanical interface with telescope (allows for up to 5 mm of lateral displacements in the attachment plane), of the LIRIS handling trolley, of the transport equipment and of all the equipments used in the integration was also checked. For the second commissioning of LIRIS, which has been held in March 2004, some modifications have been done. The results of both commissionings were satisfactory.

Select this Article		Preparation and testing of a fiber MOS unit feeding a near-infrared spectrograph Roberto Speziali, Daniele Liberi, Fausto Cortecchia, Francesco D'Alessio, Gianluca Li Causi, Dario Lorenzetti, Fernando Pedichini, and Fabrizio Vitali Proc. SPIE 5492, 1520 (2004); http://dx.doi.org/10.1117/12.551294 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We describe the procedures adopted to realize the fiber unit for feeding the near IR multi-object spectrometer GOHSS. Since a scarce literature is available on this subject, all the steps of the fabrication processes are explained and documented through a detailed illustrative material: in particular the polishing methods of the fiber ends are addressed along with the criteria for evaluating the achieved results; the preparation and application of the ferrules; the matching with the input micro-lens; finally, the laboratory tests to measure the focal ratio degradation of each fiber are presented aiming also to certify the quality of the realized device.

Select this Article		Commissioning of the NACO Fabry-Perot interferometer at the VLT Markus Hartung, Chris Lidman, Nancy Ageorges, Olivier Marco, Markus E. Kasper, and Yann Clenet Proc. SPIE 5492, 1531 (2004); http://dx.doi.org/10.1117/12.552048 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract In October 2002 the VLT Adaptive Optics (AO) facility instrument NAOS-CONICA (NACO) was offered for the first time to the astronomical community and has been operated successfully ever since. NACO is capable of performing AO assisted imaging, spectroscopy, polarimetry, and coronography. One exciting and unique observing capability of NACO is its cold tunable Fabry-Perot Interferometer, that will be offered in October 2004. The 3-dimensional structure analysis of extended objects, such as planetary nebulae, is one interesting application of this device that combines imaging and medium resolution spectroscopy in the K-band. Using VLT day and night time commissioning data, the performance of the Fabry-Perot is evaluated and a strategy to handle the complex calibration and data reduction has been developed.

Select this Article		Performance update of the infrared camera and spectrograph for the Subaru Telescope (IRCS) Hiroshi Terada, Naoto Kobayashi, Alan T. Tokunaga, Tae-Soo Pyo, Ko Nedachi, Mark Weber, Robert Potter, and Peter M. Onaka Proc. SPIE 5492, 1542 (2004); http://dx.doi.org/10.1117/12.552516 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present the upgraded performance of the Infrared Camera and Spectrograph for the Subaru Telescope (IRCS). The IRCS has been very successfully operating on cassegrain focus of the telescope about four years after the first light in February 2000. Initially the capability of the IRCS was limited due to the quite low sensitivity of the camera side array (Q.E.~50%) and the high dark current(~0.6e^-/sec) of the spectrograph side array. To improve the performance, two major upgrades were carried out for the IRCS in these four years. The first major upgrade was the replacement of the previous engineering grade Aladdin-II array on the camera side used for imaging and grism spectroscopy into the new Aladdin-III array with significantly improved sensitivity (Q.E.~95%) in August 2001. Then, we also replaced the previous Aladdin-II array on the spectrograph side for high dispersion echelle spectroscopy into the new Aladdin-III array with good sensitivity (Q.E.~95%) and low dark current (~0.05e^-/s) in the second major upgrade in June 2003. In this report, we will show the updated characteristics for the new Aladdin-III on the spectrograph side and also summarise the total performance of the IRCS after the upgrades together with actually achieved scientific results.

Select this Article		Astronomical observation through the NIR atmospheric emissive layer Guy Moreels, Michael Faivre, Olivier Lorin, Dominique Pautet, Francois Colas, and Jacques Clairemidi Proc. SPIE 5492, 1551 (2004); http://dx.doi.org/10.1117/12.550838 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The emission of the upper atmosphere introduces an additional component into photometric observations of astronomical objects. In the I band for instance, the intensity of the atmospheric emission is of the order of 1 to 2 Imag20 per square arcsecond. The subtraction of this component is not easy because it varies during the night by as much as 50% and it is not homogeneous over the sky. A program aimed at understanding the main characteristics of the atmospheric emission was undertaken. A set of CCD images of the OH emission in the I band covering the sky was assembled in a panorama, it shows wide converging arches. An algorithm was developed in order to invert the perspective projection of the photographs. The result is a 2200 km wide view over Europe and Mediterranean Sea of the emission as seen from a virtual satellite. This image shows the presence of an extended wave field. A Fourier analysis allows to infer mean horizontal wavelength, mean temporal period and horizontal phase velocity. The atmospheric emission varies under the influence of atmospheric waves. A stereoscopic imaging program is currently under development to measure the amplitude and the energy of the atmospheric waves.

Select this Article		Clio: a 5-μm camera for the detection of giant exoplanets Melanie Freed, Philip M. Hinz, Michael R. Meyer, N. Mark Milton, and Michael Lloyd-Hart Proc. SPIE 5492, 1561 (2004); http://dx.doi.org/10.1117/12.550940 \| Cited 6 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We plan to take advantage of the unprecedented combination of low thermal background and high resolution provided by the 6.5m MMT's adaptive secondary mirror, to target the 3-5 micron atmospheric window where giant exoplanets are expected to be anomalously bright. We are in the process of building a 3-5 micron camera that we will use to carry out a survey to characterize the prevalence and distribution of giant planets around nearby, Sun-like stars. Sensitivity estimates show that for a 1 Gyr old G0V primary at 10 pc, we expect to detect 5 M_Jupiter and 15 M_Jupiter exoplanets at angular separations greater than 0.45-2.1" and 0.2-1.2" respectively. Monte Carlo simulations based on these sensitivity estimates and a sample of 80 young (<1 Gyr), nearby (<20 pc) M0V-F0V stars, predict the detection of 15±3 exoplanets with masses of 4-15 M_Jupiter and separations of 17-50 AU. Construction of the camera is currently underway and on-telescope testing is expected in the Fall 2004-Winter 2005.

Select this Article		Engineering performance of IRIS2 infrared imaging camera and spectrograph Vladimir Churilov, John Dawson, Greg A. Smith, Lew Waller, John D. Whittard, Roger Haynes, Allan Lankshear, Stuart D. Ryder, and Chris G. Tinney Proc. SPIE 5492, 1572 (2004); http://dx.doi.org/10.1117/12.550965 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract IRIS2, the infrared imager and spectrograph for the Cassegrain focus of the Anglo Australian Telescope, has been in service since October 2001.IRIS2 incorporated many novel features, including multiple cryogenic multislit masks, a dual chambered vacuum vessel (the smaller chamber used to reduce thermal cycle time required to change sets of multislit masks), encoded cryogenic wheel drives with controlled backlash, a deflection compensating structure, and use of teflon impregnated hard anodizing for gear lubrication at low temperatures. Other noteworthy features were: swaged foil thermal link terminations, the pupil imager, the detector focus mechanism, phased getter cycling to prevent detector contamination, and a flow-through LN2 precooling system. The instrument control electronics was designed to allow accurate positioning of the internal mechanisms with minimal generation of heat. The detector controller was based on the AAO2 CCD controller, adapted for use on the HAWAII1 detector (1024 x 1024 pixels) and is achieving low noise and high performance.We describe features of the instrument design, the problems encountered and the development work required to bring them into operation, and their performance in service.

Select this Article		ISPI: a wide-field NIR imager for the CTIO Blanco 4-m telescope Nicole S. van der Bliek, Dara Norman, Robert D. Blum, Ronald G. Probst, Andres Montane, Ramon Galvez, Michael Warner, Roberto Tighe, Francisco Delgado, and Manuel Martinez Proc. SPIE 5492, 1582 (2004); http://dx.doi.org/10.1117/12.550973 \| Cited 4 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Infrared Side Port Imager ISPI is a facility infrared imager forthe CTIO Blanco 4-meter telescope. ISPI has the following capabilities: 1-2.4 micron imaging with an 2K x 2K HgCdTe array, 0.3arcsec/pixel sampling matched to typical f/8 IR image quality of ~0.6arcsec and a 10.5 x 10.5 arcmin field of view. First light with ISPIwas obtained on September 24 2002, and since January 2003 ISPI hasbeen in operation as a common user instrument. In this paper we discuss operational aspects of ISPI, the behavior of the array and we report on the performance of ISPI during the first one and half year of operation.

Select this Article		The REM telescope: a robotic multiwavelength facility Filippo M. Zerbi, Guido Chincarini, Gabriele Ghisellini, Marcello Rodono, Gino Tosti, Lucio A. Antonelli, Paolo Conconi, Stefano Covino, Giuseppe Cutispoto, Emilio Molinari, Luciano Nicastro, and Eliana Palazzi Proc. SPIE 5492, 1590 (2004); http://dx.doi.org/10.1117/12.551145 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The REM Observatory, recently installed and commissioned at la Silla Observatory Chile, is the first moderate aperture robotic telescope able to cover simultaneously the visible-NIR (0.45-2.3 microns) wavelength range. His very fast pointing and his full robotization makes it an ideal observing facility for fast transients. The high throughput Infrared Camera and the Visible imaging spectrograph simultaneously fed by a dichroic allows to collect high S/N data in an unprecedented large spectral range on a telescope of this size. The REM observatory is an example of a versatile and agile facility necessary complement to large telescopes in fileds in which rapid response and/or target pre-screening are necessary. We give in this paper an overview of the Observatory and its performances with emphasis to the innovative technical solution adopted to reach such performances.

Select this Article		The commissioning of the REM-IR camera at La Silla Paolo Conconi, Ronan Cunniffe, Francesco D'Alessio, Luca Calzoletti, Brendan Jordan, Ruben Mazzoleni, Andrea Melandri, Emilio Molinari, Vincenzo Testa, Fabrizio Vitali, Filippo M. Zerbi, Guido Chincarini, Stefano Covino, Gabriele Ghisellini, Marcello Rodono, et al. Proc. SPIE 5492, 1602 (2004); http://dx.doi.org/10.1117/12.551289 \| Cited 5 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract During the early Summer 2003, the REM telescope has been installed at La Silla, together with the near infrared camera REM-IR and the optical spectrograph. ROSS. The REM project is a fully automated instrument to follow-up Gamma Ray Burst, triggered mainly by satellites, such as HETE II, INTEGRAL, AGILE and SWIFT. REM-IR will perform high efficiency imaging of the prompt infrared afterglow of GRB and, together with the optical spectrograph ROSS, will cover simultaneously a wide wavelength range, allowing a better understanding of the intriguing scientific case of GRB. In this paper we present the result of the commissioning phase of the near infrared camera REM-IR, lasted for an extended period of time and currently under the final fine tuning.

Select this Article		REM: a fully robotic telescope for GRB observations Stefano Covino, Mauro Stefanon, Giorgio Sciuto, Alberto Fernandez-Soto, Gino Tosti, Filippo M. Zerbi, Guido Chincarini, Lucio A. Antonelli, Paolo Conconi, Giuseppe Cutispoto, Emilio Molinari, Luciano Nicastro, and Marcello Rodono Proc. SPIE 5492, 1613 (2004); http://dx.doi.org/10.1117/12.551532 \| Cited 3 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Rapid Eye Mount (REM) telescope is an ambitious project devoted to the prompt observations, in the optical and Near Infrared (NIR), of Gamma-Ray Bursts (GRBs) whose high energy emission is mainly detected by the Swift satellite. The system is able to immediately react to a GRB alert and perform observations, data reduction and analyses, distributing GRB counterparts in a timescale of tens of seconds. Apart from GRB observations, REM can also drive autonomous observations of a variety of targets as X-ray transients, flare stars, etc. We describe here how REM can manage all these tasks robotically, taking into account environmental and scientific parameters as seeing, visibility, target priority, etc.

Select this Article		Near-infrared camera and Fabry-Perot spectrometer (NIC-FPS) Fred R. Hearty, Jon Morse, Stephane Beland, James Green, Nathaniel J. Cunningham, Robert Valentine, Meredith Drosback, Cynthia S. Froning, Patrick Hartigan, and J. C. Barentine Proc. SPIE 5492, 1623 (2004); http://dx.doi.org/10.1117/12.551703 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A near-infrared instrument is being built for the ARC 3.5 meter telescope that will operate in both an imaging and a narrow band, full field spectroscopic mode. The 4.5' x 4.5' fild-of-view is imaged onto a new-generation, low-noise Rockwell Hawaii-1RG 1024x1024 HgCdTe detector. High resolution (R~10,000) spectroscopy is accomplished by employing a Queensgate (now IC Optical) cryogenic Fabry-Perot etalon. The instrument is housed in a large Dewar of innovative, light-weight design. This report describes the as-built opto-mechanical system for the instrument and the work remaining before deployment at Apache Point Observatory in New Mexico.

Select this Article		INCA: a light 1- to 5-μm camera for ground and space applications Alberto Riva, Vincenzo De Caprio, Florio Dalla Vedova, Alessandro Battocchio, Giorgio Colombo, Filippo M. Zerbi, Corrado Bosco, Marco Canetti, Paolo Cerabolini, Andrea Casale, Paolo Conconi, Vincenzo Di Marco, Mauro Ghigo, Ruben Mazzoleni, Emilio Molinari, et al. Proc. SPIE 5492, 1633 (2004); http://dx.doi.org/10.1117/12.551719 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We present INCA, a prototype of a light and versatile camera covering the 1-5 microns wavelength range designed for ground based and space application. INCA has innovative optical solution such as aspherical mirrors obtained via ion-beam ablation, a new light cryogenic concept and a new philosophy of chip controller. Co-financed at the bread board level by the Italian Space Agency (ASI) INCA has been recently characterized and is now ready for a phase 2 development.

Select this Article		Spartan infrared camera: high-resolution imaging for the SOAR Telescope Edwin D. Loh, Jason D. Biel, Jian-Jun Chen, Michael Davis, Rene Laporte, and Owen Y. Loh Proc. SPIE 5492, 1644 (2004); http://dx.doi.org/10.1117/12.551808 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Spartan Infrared Camera provides tip-tilt corrected imaging for the SOAR Telescope in the 1-2.5μm spectral range with four 2048x2048 HAWAII2 detectors. The median image size is expected to be less than 0.25 arcsec (FWHM), and in the H and K bands a significant amount of the light is expected to be in a core having the diffraction-limited width. The camera has two plate scales: 0.04 arcsec/pixel (f/21) for diffraction-limited sampling in the H and K bands and 0.07 arcsec/pixel (f/12) to cover a 5×5 arcmin² field, over which tip-tilt correction is substantial. Except for CaF2 field-flattening lenses, the optics is all reflective to achieve the large field size and achromaticity, and all aluminum to match thermally the aluminum cryogenic-optical box in which the optics mount. The Strehl ratio of the camera itself is 0.95-1.00 for the f/21 channel. The optics (including the off-axis aspherical mirrors) will be aligned with precise metrology rather than adjusted using interferometry.

Select this Article		PANIC: a near-infrared camera for the Magellan telescopes Paul Martini, S. E. Persson, David C. Murphy, Christoph Birk, Stephen A. Shectman, Steve M. Gunnels, and Erich Koch Proc. SPIE 5492, 1653 (2004); http://dx.doi.org/10.1117/12.551828 \| Cited 25 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract PANIC (Persson's Auxiliary Nasmyth Infrared Camera) is a near-infraredcamera designed to operate at any one of the f/11 folded ports of the 6.5m Magellan telescopes at Las Campanas Observatory, Chile. The instrument is built around a simple, all-refractive design that reimages the Magellan focal plane to a plate scale of 0.125"/pixel onto a Rockwell 1024x1024 HgCdTe detector. The design goals for PANIC included excellent image quality to sample the superb seeing measured with the Magellan telescopes, high throughput, a relatively short construction time, and low cost. PANIC has now been in regular operation for over one year and has proved to be highly reliable and produce excellent images. The best recorded image quality has been ~0.2" FWHM.

Select this Article		Thermal reflector to reduce thermal radiation in the entrance of cryogenic instruments Edwin D. Loh Proc. SPIE 5492, 1661 (2004); http://dx.doi.org/10.1117/12.551831 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The entrance of a cryogenic instrument is often a major heat load, since the opening in the cold instrument has a large solid angle. We present a novel thermal reflector that, placed between two openings, reduces the load by reflecting radiation emitted in the hot opening and not directed toward the cold opening. In the Spartan IR Camera, this thermal reflector, placed between the vacuum window and the field stop, reduces the load by a factor of 2.5, which is 1.5 times the limit defined by the size of the field stop, the minimum window size, and the separation between the two.

Select this Article		INGRID: retrofitting an improved mechanism control system to an operational cryogenic instrument Simon G. Rees, Paul Jolley, Michiel van der Hoeven, Andy Ridings, and Maarten Blanken Proc. SPIE 5492, 1665 (2004); http://dx.doi.org/10.1117/12.552214 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract This paper describes an engineering programme to retrofit an improved mechanism control system to the Isaac Newton Group Red Imaging Device (INGRID), the infrared camera at the William Herschel Telescope. INGRID is an operational instrument and engineering upgrades need to be considered carefully with a view to minimising risks to the instrument and ensuring that it is back in service on the due date. A number of alternative mechanical arrangements were considered; different stepper motor candidates were assessed together with the electronics to drive them. Motor drive parameters were optimised to increase the speed of optical setup. Finally, different technologies were considered for improving the arrangements for sensing the position of the instrument's mechanism wheels. The paper reports on the results of this programme and lessons learned.

Select this Article		Instrument science at the Anglo-Australian Observatory Joss Bland-Hawthorn Proc. SPIE 5492, 1678 (2004); http://dx.doi.org/10.1117/12.550295 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Anglo-Australian Observatory (AAO) has two groups which work closely to develop the next generation of astronomical instruments: the Instrumentation group, headed by Sam Barden, and the Instrument Science group. The Instrument Science group plays a key role in identifying and prototyping new technologies and concepts, and in establishing links with universities and industrial partners. Recent developments include the following: "echidna" fibre positioning technology, "starbug" robotic positioners; designer optical fibres and photonics; inertial drives and new concepts for large telescopes; new designs for gratings, tunable filters and interference coatings; a programmable "honeycomb" integral field spectrograph; a compact spectrograph for a Mars rover; and a new scheme for an optical laser receiver.

Select this Article		Helium cryostat vent sizing For SOFIA science instruments Maureen L. Savage, Siriluk Limmongkol, Richard E. Bacher, Theodore M. Brown, Christopher T. Koerber, Eric Smith, and Patrick G. Waddell Proc. SPIE 5492, 1689 (2004); http://dx.doi.org/10.1117/12.552622 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract In the event of a cryostat vacuum failure, the subsequent liquid helium boil off can produce a significant pressure rise in the helium reservoir potentially causing damage to the cryostat. To preclude cryostat damage during such a failure, an analysis has been developed to predict the maximum internal pressure for the corresponding vent neck size and helium reservoir surface area at failure condition. To demonstrate that the analysis predicts correct pressure values, a series of experiments have been carried out at NASA Ames Research Center to measure the pressure profile during an induced failure. The maximum measured helium reservoir pressure is then used in the analysis to derive the heat load. The experiments have been conducted using a cylindrical helium and nitrogen cryostat with a variable size constriction insert in the helium neck to enable measuring the pressure rise across a range of effective neck areas. The experimentally derived heat flux on the uninsulated helium reservoir during an induced vacuum failure is 3.1 ± 0.2 W/cm². Some preliminary test results are presented describing the effects of superinsulation, but this aspect of cryostat design is not extensively explored, as the design and materials selected may have highly variable results.

Select this Article		The CAMCAO infrared camera Antonio Amorim, Antonio Melo, Joao Alves, Jose Rebordao, Jose Pinhao, Gregoire Bonfait, Jorge Lima, Rui Barros, Rui Fernandes, Isabel Catarino, Marta Carvalho, Rui Marques, Jean-Marc Poncet, Filipe Duarte Santos, Gert Finger, et al. Proc. SPIE 5492, 1699 (2004); http://dx.doi.org/10.1117/12.549008 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The CAMCAO instrument is a high resolution near infrared (NIR) camera conceived to operate together with the new ESO Multi-conjugate Adaptive optics Demonstrator (MAD) with the goal of evaluating the feasibility of Multi-Conjugate Adaptive Optics techniques (MCAO) on the sky. It is a high-resolution wide field of view (FoV) camera that is optimized to use the extended correction of the atmospheric turbulence provided by MCAO. While the first purpose of this camera is the sky observation, in the MAD setup, to validate the MCAO technology, in a second phase, the CAMCAO camera is planned to attach directly to the VLT for scientific astrophysical studies. The camera is based on the 2kx2k HAWAII2 infrared detector controlled by an ESO external IRACE system and includes standard IR band filters mounted on a positional filter wheel. The CAMCAO design requires that the optical components and the IR detector should be kept at low temperatures in order to avoid emitting radiation and lower detector noise in the region analysis. The cryogenic system inclues a LN2 tank and a sptially developed pulse tube cryocooler. Field and pupil cold stops are implemented to reduce the infrared background and the stray-light. The CAMCAO optics provide diffraction limited performance down to J Band, but the detector sampling fulfills the Nyquist criterion for the K band (2.2mm).

Select this Article		Overview and design of the Canarias infrared camera experiment (CIRCE) Michelle L. Edwards, Antonio Marin-Franch, Stephen S. Eikenberry, Michael Rodgers, Jeff Julian, Kevin Hanna, and Chris Packham Proc. SPIE 5492, 1710 (2004); http://dx.doi.org/10.1117/12.550514 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We report on the design status of the Canarias InfraRed Camera Experiment (CIRCE), a near-infrared visitor instrument for the 10.4-meter Gran Telescopio Canarias (GTC). Besides functioning as a 1-2.5 micron imager, CIRCE will have the capacity for narrow-band imaging, low- and moderate- resolution grism spectroscopy, and imaging polarimetry. Other design features include fully cryogenic filter, slit, and grism wheels, high-speed photometry modes, and broad-band imaging in J, H, and Ks filters. We anticipate that a myriad of scientific projects will benefit from CIRCE's unique combination of capabilities.

Select this Article		Program status of NEWFIRM, the wide-field infrared camera system for the NOAO 4-m telescopes Ronald G. Probst, Neil Gaughan, Marianne Abraham, John Andrew, Phil Daly, Edward Hileman, Mark Hunten, Ming Liang, K. M. Merrill, Roger Repp, and Richard Shaw Proc. SPIE 5492, 1716 (2004); http://dx.doi.org/10.1117/12.550801 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The NEWFIRM program will provide a widefield IR imaging system optimized for survey programs on the NOAO 4-m telescopes in Arizona and Chile. The camera images a 28 x 28 arcminute field of view over 1-2.4 microns wavelength range with a 4K x 4K pixel array mosaic. We present an overview of camera design features including optics design, manufacture, and mounting; control of internal flexure between input and output focal planes; mosaic array mount design; and thermal design. We also discuss the status of other projects within the program: array control electronics, observation and pipeline reduction software, and production of the science grade array complement. The program is progressing satisfactorily and we expect to deliver the system to the northern 4-m telescope in 2005.

Select this Article		Cooling of ground-based telescope instrumentation: the LINC-NIRVANA cryostat Werner Laun, Harald Baumeister, and Peter Bizenberger Proc. SPIE 5492, 1725 (2004); http://dx.doi.org/10.1117/12.551497 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The MPIA in Heidelberg has built many instruments for IR observation over the years. While the previous instruments were moderate in size and could easily be enclosed in a liquid nitrogen dewar, future instruments will require different cooling concepts. The use of Gifford McMahon coolers was chosen for some instruments, but has the disadvantage of low frequency vibrations. The recently-developed pulse tube coolers have lower vibrations but other disadvantages. For the LINC-NIRVANA cryostat, we plan to build a cooling system with a constant flow of Helium through a heat exchanger inside the cryostat. This cooling concept could also be expanded to future instrumentation for the next generation of telescopes.

Select this Article		Status report on the EMIR optical system Antonio Manescau, Ana B. Fragoso-Lopez, Francisco Garzon, and Jesus Patron Proc. SPIE 5492, 1735 (2004); http://dx.doi.org/10.1117/12.550428 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract EMIR is a multiobject intermediate resolution near infrared (1.0 - 2.5 microns) spectrograph with imaging capabilities, to be mounted on the Gran Telescopio Canarias. After the successful results of the preliminary design review, EMIR optical system is being fixed. Detailed status of the solutions adopted for the optical system as well as the developments made and their results are presented. Management and technical issues related to the procurement of the different optical components are shown.

Select this Article		The cryo-mechanical design of SCUBA-2: a wide-field imager for the James Clerk Maxwell Telescope David Gostick, Dave Montgomery, Bob Wall, Helen McGregor, Mark Cliffe, Adam Woodcraft, and Fred Gannaway Proc. SPIE 5492, 1743 (2004); http://dx.doi.org/10.1117/12.551749 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The SCUBA-2 instrument is a new wide-field imager under development for the James Clerk Maxwell Telescope on Mauna Kea in Hawaii and due to be operational in 2006. The instrument has two separate focal planes and is designed to observe simultaneously at wavelengths of 450 and 850μm. The instrument cryostat will weigh around 2500kg and has a volume of approximately 2.4x1.8x2.0m. The two detector arrays are operated at ~100mK and are surrounded by a cold enclosure at ~1K. Both the arrays and cold enclosure are cooled by a novel, liquid cryogen-free dilution refrigerator. To reduce the thermal background on the arrays to a minimum the main optics structure, weighing in excess of 450kg, must be cooled to less than 15K. A pair of low vibration pulse tube coolers are used to cool this structure and a radiation shield at ~60K. This paper describes the cryo-mechanical design of SCUBA-2 and discusses some of the issues and techniques needed to both cool the instrument within a reasonable timescale, and operate it in the required temperature regime

Select this Article		Tunable etalons and other applications of multi-application low-voltage piezoelectric instrument control electronics (MALICE) Alan D. Scott, Rodney Norman, and Liping Zhou Proc. SPIE 5492, 1755 (2004); http://dx.doi.org/10.1117/12.552005 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract EMS have developed low voltage piezoelectric (LVPZT) tunable filters for the James Webb Space Telescope (JWST), and a wide field tunable Michelson for the Canadian Space Agency"s (CSA) Stratospheric Wind Interferometer For Transport studies (SWIFT) instrument. As a spin-off from this work, we have developed a prototype control system for ground-based interferometric optics using LVPZTs and capacitive displacement sensor feedback. The system is designed to control three channels in parallel with a measurement resolution target of <0.1 Å/√Hz, and thermal drift bandwidth limit of ~1 Hz over a dynamic motion range of ~8 μm. The prototype Multi-Application LVPZT Instrument Control Electronics (MALICE) system will be delivered in fall 2004 with a field-widened Michelson to perform observations of atmospheric wave phenomena at remote weather stations. We describe the performance of the MALICE prototype and its applications to astronomical imaging and remote sensing.

Select this Article		HAWK-I: A new wide-field 1- to 2.5-μm imager for the VLT Jean-Francois Pirard, Markus Kissler-Patig, Alan Moorwood, Peter Biereichel, Bernard Delabre, Reinhold Dorn, Gert Finger, Domingo Gojak, Gotthard Huster, Yves Jung, Franz Koch, Miska Le Louarn, Jean-Louis Lizon, Leander Mehrgan, Esther Pozna, et al. Proc. SPIE 5492, 1763 (2004); http://dx.doi.org/10.1117/12.578293 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract HAWK-I (High Acuity, Wide field K-band Imaging) is a 0.9 μm - 2.5 μm wide field near infrared imager designed to sample the best images delivered over a large field of 7.5 arcmin x 7.5 arcmin. HAWK-I is a cryogenic instrument to be installed on one of the Very Large Telescope Nasmyth foci. It employs a catadioptric design and the focal plane is equipped with a mosaic of four HAWAII 2 RG arrays. Two filter wheels allow to insert broad band and narrow band filters. The instrument is designed to remain compatible with an adaptive secondary system under study for the VLT.

Select this Article		Optical design for a Fabry-Perot image interferometer for solar observations Gilberto Moretto, G. Allen Gary, K. S. Balasubramaniam, and Thomas R. Rimmele Proc. SPIE 5492, 1773 (2004); http://dx.doi.org/10.1117/12.548913 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract We outline here a preliminary optical design study for a telecentric tunable Fabry-Perot etalon system. The first result of the optical optimization into a design, which delivers performance image quality and telecentricity, is presented here. Bearing in mind the possible use of such a study design - as a possible instrument for the Advanced Technology Solar Telescope (ATST) - we also show that a hybrid design strategy delivers a compact design that will fit inside the ATST's Coude optical tables.

Select this Article		Calibration of the instrumental polarization of the Domeless Solar Telescope at the Hida Observatory Junko Kiyohara, Satoru Ueno, Reizaburo Kitai, Hiroki Kurokawa, Mitsugu Makita, and Kiyoshi Ichimoto Proc. SPIE 5492, 1778 (2004); http://dx.doi.org/10.1117/12.551222 \| Cited 1 time Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A new spectropolarimeter is developed at the Domeless Solar Telescope (DST) in Hida Observatory. It consists of a rotating waveplate, Wollaston prisms, and a high-dispersion spectrograph which is vertically installed at the focus of the DST. In order to realize a high-precision measurement, it is inevitable to compensate the instrumental polarization due to the DST. We observed the quiet region of the Sun, which is considered to be highly unpolarized, with and without a sheet linear polarizer or circular polarizer set at the entrance window of the telescope. The theoretical model which represents the total instrumental polarization of the DST with some characteristic parameters was calculated and compared with the observation. The model that two flat mirrors have different properties can explain the observation in 0.5% accuracy for the unpolarized light, and in 7% for the polarized light.

Select this Article		Near infrared waveplate Dongguang Wang, Yuanyong Deng, and Wenda Cao Proc. SPIE 5492, 1786 (2004); http://dx.doi.org/10.1117/12.553165 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The waveplate made of Polyvinyl Alcohol (PVA) plastic film has several advantages compared with that of birefringent crystal in visible region, such as its lower cost and insensitivity to temperature and incidence angle. What are the performances when they are used in the near infrared spectral region? In this paper, we provide some experimental results of infrared PVA waveplates. To do this, we make some samples and measure their polarization characteristics at several aspects. Firstly, we measure the performance of these PVA waveplates by precise instruments in laboratory. Secondly, we put the waveplates into a Stokes polarimeter to observe the solar magnetic field at near infrared line FeI1.56μm. By use of this polarimeter mounted on the vertical spectrograph of 2m McMath telescope at Kitt Peak, the two-dimensional Stokes parameters, I, Q, U, and V, of a sunspot were observed. From the results of laboratory and observation, we get the conclusion that PVA waveplate has the fair polarization performance to be used to observe the solar magnetic fields in the near infrared spectral region. By these experiments, we provide a design of an achromatic waveplate in infrared region, which consists of five-element, to illustrate the PVA waveplate is the best choice to it.

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Instrumentation for Future Extremely Large Telescopes

Select this Article		Instruments for a European Extremely Large Telescope: the challenges of designing instruments for 30- to 100-m telescopes Adrian P. Russell, Guy Monnet, Andreas Quirrenbach, Roland Bacon, Michael Redfern, Torben Andersen, Arne Ardeberg, Eli Atad-Ettedgui, and Timothy G. Hawarden Proc. SPIE 5492, 1796 (2004); http://dx.doi.org/10.1117/12.551473 \| Cited 2 times Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Designs for Extremely Large Telescopes (ELTs) are quite well advanced, but the requirements of instruments have had limited impact. Since provision of a suitable environment for instruments is a critical aspect of all telescopes, we outline some well-known and some less-appreciated challenges of designing instruments for ELTs. A wide-field spectrometer (WFSPEC) with ~10 arcmin field-of-view, probably with AO correction of ground-layer seeing, illustrates the well-known difficulty of matching modern detector pixels to large (~0."3) images. The challenges of exploiting wide-field (1'-2' FOV) high-performance AO systems on ELTs are illustrated by a Multi-Object Multi-field Spectrometer and Imager (MOMSI), which provides imaging and integral-field spectroscopy, at near-diffraction-limited pixel scales, of targets in approximately 300 subfields each. This instrument, roughly equivalent to all the astronomical spectrometers yet built, extracts ~200 times less of the available information from the ELT's FOV than near-future instruments on 8-m class telescopes will do for their hosts. We emphasise the great size of such instruments (40-100 tonnes, 100-200 m3) and the need to accommodate this size in telescope plans. A third area of challenge is the exploitation of the potential capabilities of ELTs in the mid-IR, where they would offer powerful complements to JWST and ALMA; low-emissivity telescope designs and, possibly, cryogenic AO, may be needed. Finally, we outline the potential challenges of correcting atmospheric dispersion effects.

Select this Article		Toward instrumentation for ELTs: the OWL case Guy Monnet and Sandro D'Odorico Proc. SPIE 5492, 1810 (2004); http://dx.doi.org/10.1117/12.562330 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract Based on expected Science Drivers for a 60 to 100-m diameter OWL-class telescope, we derive the basic instrumental capabilities that are needed to address them effectively. They come in three flavors -viz. an extremely high-contrast fully diffraction-limited spectro-imager, a cryogenic AO-assisted imager and multi-integral field spectrometer. Their highest priority wavelength range lies in the near-IR. In terms of size and technical requirements, these instruments belong to a quite similar class than instruments currently being developed for the 8-10 m telescopes. This places them hopefully in the feasible category, even if already rather challenging. A big caveat however is that enlarging the imaging field or the spectrometer multiplex would require large clusters of these basic "bricks". The requirements on the adaptive optics correction are stringent and call for a close and careful integration between the telescope adaptive optics systems and the instruments. We also introduce here, as a relevant example of a new observational strategy, an instrument focused on a specific scientific program - the direct measurement of the acceleration of the Universe at different epochs via the Lyα forest in QSO spectra. Being able to host dedicated facilities of this type, used for a specific observing programs in a CERN experiment-like fashion, is deemed essential to ensure that the giant telescopes of the future get and stay at the cutting edge of research in the next decade and beyond. Finally, we comment briefly on the articulation between the development of generic instrument concepts for ELTs in the frame of the European ELT Design Study and their adaptation to the OWL case.

Select this Article		Instrumentation for the Thirty Meter Telescope Keith Taylor Proc. SPIE 5492, 1818 (2004); http://dx.doi.org/10.1117/12.556885 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Science Advisory Committee (SAC) of the Thirty Meter Telescope Project (TMT) is nearing completion in its deliberations on defining a set of instrumentation capabilities for the first decade of operation. These are encapsulated in the SAC"s Science Requirements Document (SRD). We focus here on issues related to the challenges posed by the proposed first generation requirements for both seeing-limited, wide-field spectroscopy for the UV/optical and for integral field unit (IFU) spectroscopy for the near infra-red (NIR).

Select this Article		A Canadian wide-field optical spectrograph for a 30-m telescope Bev Oke, Denis Laurin, Ian Powell, David Crampton, John Pazder, Kei Szeto, Marc Baril, Leslie Saddlemyer, James Stilburn, and Scott Roberts Proc. SPIE 5492, 1824 (2004); http://dx.doi.org/10.1117/12.552436 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract A wide-field low-resolution multi-object optical spectrograph suitable for a 30-m F/15 telescope is described. The effort to build a 30-m class telescope is gaining momentum. Many science cases for such a telescope make the need for a wide-field seeing-limited spectrograph a high priority. Our concept comprises four identical instruments placed symmetrically around the optical axis of the telescope, this allows smaller dimensions for the spectrographs and their components. Each instrument is placed in one quadrant of the telescope focal plane; a space at the center of the field is free for other instrumentation. Using a dichroic beam-splitter each instrument feeds a "red" and "blue" camera. The total field is 81 square arcmin, the wavelength range covers simultaneously 310 nm to 1000 nm and the spectral resolution (R) is 300 to 5000. The instruments are designed for vertical mounting at a Nasmyth focus to avoid gravity vector changes and reducing mechanical flexure problems during observation. The layout also allows access to internal components for maintenance. The design offers advantages for the location of a slit mask and filters. The instruments can also be used for imaging. Optical and opto-mechanical models and analyses are presented with specifications and expected performance.

Select this Article		The MOMFOS fiber positioner Anna M. Moore and Andrew J. McGrath Proc. SPIE 5492, 1835 (2004); http://dx.doi.org/10.1117/12.550294 Online Publication Date: Oct 05, 2004 Full Text: \| Download PDF
	+ -	Show Abstract The Anglo-Australian Observatory has undertaken a design study for a ≈1000 fibre positioner for the prime focus of the Giant Segmented Mirror Telescope (GSMT) as part of the MOMFOS (Multi-Object Multi-Fibre Optical Spectrograph) instrument. To our knowledge this is the first design study funded for a prime focus instrument for an ELT. It offers a particularly elegant and efficient solution for wide-field multiobject spectroscopy on extremely large telescopes (>30m) for the acquisition of large scale high-redshift surveys (1<z<10) with sufficient area (25 deg²), density coverage (≈2.5 million galaxies) and limiting magnitude (R≤26.5).Closely based on the innovative Echidna positioner under construction for Subaru's FMOS system, the MOMFOS positioner uses piezoelectric microrobotic actuators able to position accurately all 1000 fibres simultaneously. The FMOS-Echidna design is extended to include a novel position feedback system offering radical benefits in cost and speed. We present positioning results for a design capable of a higher packing density than that developed for FMOS-Echidna, providing ≈1000 fibres across the 175 mm diameter field of view (20 arcmin).

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