The design of the Near Space Optical Survey-alpha (NSOS-α) telescope, encouraged by Korea Astronomy and Space Science Institute (KASI) aims to discover and catalog near-Earth asteroids, especially Potentially Hazardous Asteroids (PHAs). To achieve this goal, an optical telescope with a 1.5m class primary mirror and a 5 square degree field of view will be installed and operated at Cerro Tololo Inter-American Observatory (CTIO) in Chile. The wide field telescope is under development and being designed by a collaboration between KASI and the NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab). A prime focus configuration was adopted and designed with a seven element wide field corrector (WFC). The main mechanical design philosophy was scaled, modified, and revised based on the Korea Microlensing Telescope Network (KMTNet). The NSOS-α telescope will be the first dedicated observation facility for asteroid survey in the southern hemisphere using a 1.5-meter class telescope. In this paper, a summary of the optical and mechanical assemblies designed for the NSOS-α telescope will be addressed.
The Rubin Observatory Commissioning Camera (ComCam) is a scaled down (144 Megapixel) version of the 3.2 Gigapixel LSSTCam which will start the Legacy Survey of Space and Time (LSST), currently scheduled to start in 2024. The purpose of the ComCam is to verify the LSSTCam interfaces with the major subsystems of the observatory as well as evaluate the overall performance of the system prior to the start of the commissioning of the LSSTCam hardware on the telescope. With the delivery of all the telescope components to the summit site by 2020, the team has already started the high-level interface verification, exercising the system in a steady state model similar to that expected during the operations phase of the project. Notable activities include a simulated “slew and expose” sequence that includes moving the optical components, a settling time to account for the dynamical environment when on the telescope, and then taking an actual sequence of images with the ComCam. Another critical effort is to verify the performance of the camera refrigeration system, and testing the operational aspects of running such a system on a moving telescope in 2022. Here we present the status of the interface verification and the planned sequence of activities culminating with on-sky performance testing during the early-commissioning phase.
NEID (NN-explore Exoplanet Investigations with Doppler spectroscopy) is an optical, fiber-fed spectrometer at the WIYN 3.5m Telescope. NEID’s single-measurement radial velocity precision (27 cm/s) requires the stellar image motion (induced by atmospheric turbulence) to be controlled for 90% of the time to within 50 milli-arcseconds in nominal observing conditions. This has been achieved by fast guiding through the NEID Port Adapter, which implements an EMCCD and a tip/tilt piezo stage to capture/stabilize the stellar image. Here, we use on-sky data accumulated over a year to demonstrate the performance of this system under diverse observing conditions.
Here we detail the on-sky performance of the NEID Port Adapter one year into full science operation at the WIYN 3.5m Telescope at Kitt Peak National Observatory. NEID is an optical (380-930 nm), fiber-fed, precision Doppler radial velocity system developed as part of the NASA-NSF Exoplanet Observational Research (NN-EXPLORE) partnership. The NEID Port Adapter mounts directly to a bent-Cassegrain port on the WIYN Telescope and is responsible for precisely and stably placing target light on the science fibers. Precision acquisition and guiding is a critical component of such extreme precision spectrographs. In this work, we describe key on-sky performance results compared to initial design requirements and error budgets. While the current Port Adapter performance is more than sufficient for the NEID system to achieve and indeed exceed its formal instrumental radial velocity precision requirements, we continue to characterize and further optimize its performance and efficiency. This enables us to obtain better NEID datasets and in some cases, improve the performance of key terms in the error budget needed for future extreme precision spectrographs with the goal of observing ExoEarths, requiring ∼ 10 cm/s radial velocity measurements.
The Vera C. Rubin Observatory’s Legacy Survey of Space and Time (LSST) will perform precision photometry of resolved and unresolved objects over the visible sky at a 3-day cadence using an 8.4-meter diameter telescope that forms an image of the sky on a 3.2 Gigapixel focal plane array. Meeting and exceeding the photometric precision requirements is a significant challenge and necessitates the calibration and correction of multiple forms of systematic error. This paper describes multiple novel hardware systems that Rubin is developing to measure and compensate for numerous sources of systematic errors, particularly errors impacting photometry measurements.
The NEID extreme precision radial velocity spectrometer is being commissioned at the WIYN 3.5 meter telescope, Kitt Peak National Observatory, Tucson Arizona. In order to meet the stringent 27 cm per second radial velocity precision, the light to NEID comes from an extremely stable fiber feed, called the NEID Port Adapter, equipped with fast tip-tilt correction. The WIYN telescope vibration environment and the Port Adapter tip-tilt and guiding system are key to achieving the 50 milliarcsecond-level centroiding stability required. Here we describe the servo system performance, along with vibration analysis and mitigation plans. This work would be relevant to upgrade and retrofit efforts as older observatories incorporate low-order wavefront correction to stabilize light to advanced spectrometers and imagers.
The wide field survey telescope (WFST) is a 2.5 meter optical telescope that is currently under construction in China. Designed with a large field of view (FOV) of 3 degrees in diameter and equipped with a 0.75 gigapixel mosaic CCD camera, the telescope will be mainly used for high sensitivity time-domain imaging surveys across the northern sky. The optical design for WFST features an advanced primary-focus assembly (PFA) housing five corrector lenses, an atmospheric dispersion corrector, filters of six bands, and the CCD camera. Stray light rejection performance is crucial for WFST to achieve an optimal sensitivity and maximize its scientific outputs. The primary-focus geometry of WFST helps to reduce the celestial background compared with a Cassegrain geometry, but the wide FOV imposes additional difficulty in stray light control and suppression. In this paper, the stray light behavior of WFST is carefully modeled by establishing a detailed opto-mechanical model of the telescope, assigning proper surface properties, and launching ray tracing simulations for a variety of scenarios. Important stray light paths including ghost effect and first-order scatterings are identified. Stray light mitigation measures including baffle and mask designs are proposed and optimized based on the stray light analysis results, which show promising suppression capability.
Rubin Observatory’s Commissioning Camera (ComCam) is a 9 CCD direct imager providing a testbed for the final telescope system just prior to its integration with the 3.2-Gigapixel LSSTCam. ComCam shares many of the same subsystem components with LSSTCam in order to provide a smaller-scale, but high-fidelity demonstration of the full system operation. In addition, a pathfinder version of the LSSTCam refrigeration system is also incorporated into the design. Here we present an overview of the final as-built design, plus initial results from performance testing in the laboratory. We also provide an update to the planned activities in Chile both prior to and during the initial first-light observations.
In October 2019, the NEID instrument (PI Suvrath Mahadevan, PSU) was delivered to the WIYN 3.5 m Telescope at Kitt Peak National Observatory. Commissioning began shortly after delivery, but was paused due to a COVID-19 imposed observatory shutdown in March 2020. The observatory has recently reopened and NEID commissioning has resumed. NEID is an optical (380-930 nm), fiber-fed, precision Doppler radial velocity system developed as part of the NN-EXPLORE partnership. While the spectrometer and calibration system are maintained in a highly controlled environment on the basement level of the WIYN, the NEID Port Adapter mounts directly to a bent-Cassegrain port on the telescope and is responsible for precisely and stably placing target light on the science fibers. Here we present a brief overview of the as-built Port Adapter and its sub-components. We then discuss preliminary on-sky performance compared to requirements as well as next steps as we complete commissioning.
The free-vibration modes of an annular mirror (FVMAM), derived from the thin plate theory and reflecting the intrinsic characteristics of the physical phenomenon of resonance, have been applied to compensate the aberrations of the active optics system. As an application example, the compensations of some low-order aberrations of the 2.5-m Wide-Field Survey Telescope with the FVMAM have been presented. In addition, a quantitative comparative study of the aberration corrections between the FVMAM and the annular Zernike polynomials has been carried out. The results have shown that the FVMAM are more effective to correct the aberrations.
The NEID spectrometer is an optical (380-930 nm), fiber-fed, precision Doppler spectrometer currently in de- velopment for the WIYN 3.5 m telescope at Kitt Peak National Observatory as part of the NN-EXPLORE partnership. Designed to achieve a radial velocity precision of < 30 cm/s, NEID will be sensitive enough to detect terrestrial-mass exoplanets around low-mass stars. Light from the target stars is focused by the telescope to a bent Cassegrain port at the edge of the primary mirror mechanical support. The specialized NEID “Port Adapter” system is mounted at this bent Cassegrain port and is responsible for delivering the incident light from the telescope to the NEID fibers. In order to provide stable, high-quality images to the science instrument, the Port Adapter houses several sub-components designed to acquire the target stars, correct for atmospheric dis- persion, stabilize the light onto the science fibers, and calibrate the spectrometer by injecting known wavelength sources such as a laser frequency comb. Here we provide an overview of the overall opto-mechanical design and system requirements of the Port Adapter. We also describe the development of system error budgets and test plans to meet those requirements.
The Fast-steering Secondary Mirror (FSM) of Giant Magellan Telescope (GMT) consists of seven 1.1 m diameter circular segments with an effective diameter of 3.2 m, which are conjugated 1:1 to the seven 8.4 m segments of the primary. Each FSM segment contains a tip-tilt capability for fast guiding to attenuate telescope wind shake and mount control jitter by adapting axial support actuators. Breakaway System (BAS) is installed for protecting FSM from seismic overload or other unknown shocks in the axial support. When an earthquake or other unknown shocks come in, the springs in the BAS should limit the force along the axial support axis not to damage the mirror. We tested a single BAS in the lab by changing the input force to the BAS in a resolution of 10 N and measuring the displacement of the system. In this paper, we present experimental results from changing the input force gradually. We will discuss the detailed characteristics of the BAS in this report.
The Giant Magellan Telescope (GMT) will feature two Gregorian secondary mirrors, an adaptive secondary mirror (ASM) and a fast-steering secondary mirror (FSM). The FSM has an effective diameter of 3.2 m and consists of seven 1.1 m diameter circular segments, which are conjugated 1:1 to the seven 8.4m segments of the primary. Each FSM segment contains a tip-tilt capability for fast guiding to attenuate telescope wind shake and mount control jitter. This tiptilt capability thus enhances performance of the telescope in the seeing limited observation mode. The tip-tilt motion of the mirror is produced by three piezo actuators. In this paper we present a simulation model of the tip-tilt system which focuses on the piezo-actuators. The model includes hysteresis effects in the piezo elements and the position feedback control loop.
KEYWORDS: Mirrors, Telescopes, Actuators, Space telescopes, Off axis mirrors, Integrated modeling, Interfaces, Optical instrument design, Phase transfer function, Control systems
The Fast-Steering Secondary Mirror (FSM) of Giant Magellan Telescope (GMT) consists of seven 1.1m diameter segments with effective diameter of 3.2m. Each segment is held by three axial supports and a central lateral support with a vacuum system for pressure compensation. Both on-axis and off-axis mirror segments are optimized under various design considerations. Each FSM segment contains a tip-tilt capability for guiding to attenuate telescope wind shake and mount control jitter. The design of the FSM mirror and support system configuration was optimized using finite element analyses and optical performance analyses. The design of the mirror cell assembly will be performed including sub-assembly parts consisting of axial supports, lateral support, breakaway mechanism, seismic restraints, and pressure seal. . In this paper, the mechanical results and optical performance results are addressed for the optimized FSM mirror and mirror cell assembly, the design considerations are addressed, and performance prediction results are discussed in detail with respect to the specifications
NEID is a new extreme precision Doppler spectrometer for the WIYN telescope. It is fiber fed and employs a classical white pupil Echelle configuration. NEID has a fiber aperture of only 0.92” on sky in high-resolution mode, and its tight radial velocity error budget resulted in very stringent stability requirements for the input illumination of the spectrograph optics. Consequently, the demands on the fiber injection are challenging. In this paper, we describe the layout and optical design of the injection module, including a broadband, high image quality relay and a high-performance atmospheric dispersion corrector (ADC) across the bandwidth of 380 – 930 nm.
The NEID Port Adapter is the interface between the WIYN 3.5m Telescope and the NEID fiber-fed spectrometer. The spectrometer requires the stellar jitter to be controlled for 90% of the time to within 50 milli-arc seconds for visual magnitudes 12, and 200 milli-arc seconds for V-magnitudes 12-16. The NEID Port Adapter will use an Andor EMCCD with 13 micron pixels, and a tip/tilt piezo stage from nPoint with a lowest resonant mode of 479 Hz. We expect to meet the requirement with a closed-loop rate of 27 Hz. We have data taken at the WIYN telescope consisting of stellar centroids captured at a rate of 108.75 Hz, which we rebin to test the response at lower sampling rates. We present the results of feeding these waveforms into the nPoint controller and measuring the actual response.
The Giant Magellan Telescope (GMT) will be equipped with two Gregorian secondary mirrors; a fast-steering secondary mirror (FSM) for seeing-limited operations and an adaptive secondary mirror (ASM) for adaptive optics observing modes. The FSM has an effective diameter of 3.2 m and is comprised of seven 1.1 m diameter circular segments, which are conjugated 1:1 to the seven 8.4m segments of the primary mirror. Each FSM segment has a tip-tilt capability for fast guiding to attenuate telescope wind shake and jitter. The FSM is mounted on a two-stage positioning system; a macro-cell that positions the entire FSM segments as an assembly and seven hexapod actuators that position and drive the individual FSM segments. In this paper, we present a technical overview of the FSM development status. More details in each area of development will be presented in other papers by the FSM team.
Except for the spectroscopic survey telescope LAMOST, there are only two 2m class general purpose telescopes for precision observation in China (2.16m in Xinglong and 2.4m in Lijiang). Chinese astronomical community unanimously agrees that a 10m class large diameter general purpose optical/infrared telescope is urgently needed in China for a wide range of scientific research. The configuration for LOT with primary aperture 12m has been selected by Chinese government for the Thirteen-five-years plan in July, 2016. The concept design introduced here has been approved by Chinese astronomical community and Chinese Academy of Sciences in Dec. 2017, and submitted into the formal funding procedure of Chinese government. For quite a long time, China will very likely have only one 10m class telescope, therefore LOT should be a general-purpose telescope including multi-foci. The Nasmyth focus, prime focus, Cassegrain focus and coudé focus have been considered or reserved. Also, LOT will closely combine with the development of new technologies, such as AO, GLAO, fiber and instrument related new technologies, to make it has powerful capability for the frontier sciences. The four-mirror Nasmyth system, optimized according to the GLAO requirements, has a f-ratio about 14 and field of view 14 arecmin with excellent image quality. Some off-axis four-mirror Nasmyth optical systems are also presented in this paper. The primary focus system has a f-ratio 2 and 1.5degree field of view with 80% light energy encircled in 0.5 arecsec, which will let LOT complementary with the coming 30m-class telescopes. A double–layer Nasmyth platforms are proposed to accommodate more instruments, such as the wide field imaging spectrograph, broad band medium resolution spectrograph, high resolution spectrograph and multi-object fiber spectrographs and so on. Not all optical systems will be constructed in the same time, which will be in stages depending on the science and funding situation.
The Fast Steering Secondary Mirror (FSM) for the Giant Magellan Telescope (GMT) will have seven 1.05 m diameter circular segments and rapid tip-tilt capability to stabilize images under wind loading. In this paper, we report on the assembly, integration, and test (AIT) plan for this complex opto-mechanical system. Each fast-steering mirror segment has optical, mechanical, and electrical components that support tip-tilt capability for fine coalignment and fast guiding to attenuate wind shake and jitter. The components include polished and lightweighted mirror, lateral support, axial support assembly, seismic restraints, and mirror cell. All components will be assembled, integrated and tested to the required mechanical and optical tolerances following a concrete plan. Prior to assembly, fiducial references on all components and subassemblies will be located by three-dimensional coordinate measurement machines to assist with assembly and initial alignment. All electronics components are also installed at designed locations. We will integrate subassemblies within the required tolerances using precision tooling and jigs. Performance tests of both static and dynamic properties will be conducted in different orientations, including facing down, horizontal pointing, and intermediate angles using custom tools. In addition, the FSM must be capable of being easily and safely removed from the top-end assemble and recoated during maintenance. In this paper, we describe preliminary AIT plan including our test approach, equipment list, and test configuration for the FSM segments.
The Large Synoptic Survey Telescope (LSST) Commissioning Camera (ComCam) is a smaller, simpler version of the full LSST camera (LSSTCam). It uses a single raft of 9 (instead of twenty-one rafts of 9) 4K x 4K LSST Science CCDs, has the same plate scale, and uses the same interfaces to the greatest extent possible. ComCam will be used during the Project’s 6-month Early Integration and Test period beginning in 2020. Its purpose is to facilitate testing and verification of system interfaces, initial on-sky testing of the telescope, and testing and validation of Data Management data transfer, infrastructure and algorithms prior to the delivery of the full science camera.
WFST is a proposed 2.5m wide field survey telescope intended for dedicated wide field sciences. The telescope is to operate at six wavelength bands (u, g, r, i, z, and w), spanning from 320 to 1028 nm. Designed with a field of view diameter of 3 degree and an effective aperture diameter of 2.29 m, the WFST acquires a total optical throughput over 29.3 m2deg2. With such a large throughput, WFST will survey up to 6000deg2 of the northern sky in multiple colors each night, reaching 23th magnitude for high-precision photometry and astrometry. The optical design is based on an advanced primary-focus system made up of a 2.5 m f/2.48 concave primary mirror and a primary-focus assembly (PFA) consisting of five corrector lenses, atmospheric dispersion corrector (ADC), filters, and the focal-plane instrument. For zenith angles from 0 to 60 degrees, 80% of the polychromatic diffracted energy falls within a 0.35 arcsec diameter. The optical design also highlights an enhanced transmission in the UV bands. The total optical transmission reaches 23.5% at 320 nm, allowing unique science goals in the U band. Other features include low distortion and ease of baffling against stray lights, etc. The focal-plane instrument is a 0.9 gigapixel mosaic CCD camera comprising 9 pieces of 10K×10K CCD chips. An active optics system (AOS) is used to maintain runtime image quality. Various design aspects of the WFST including the optical design, active optics, mirror supports, and the focal-plane instrument are discussed in detail.
KEYWORDS: Telescopes, Finite element methods, Systems modeling, Solid modeling, Mirrors, Actuators, 3D modeling, Large Synoptic Survey Telescope, Computer aided design, Large Synoptic Survey Telescope, Space telescopes
During this early stage of construction of the Large Synoptic Survey Telescope (LSST), modeling has become a crucial system engineering process to ensure that the final detailed design of all the sub-systems that compose the telescope meet requirements and interfaces. Modeling includes multiple tools and types of analyses that are performed to address specific technical issues. Three-dimensional (3D) Computeraided Design (CAD) modeling has become central for controlling interfaces between subsystems and identifying potential interferences. The LSST Telescope dynamic requirements are challenging because of the nature of the LSST survey which requires a high cadence of rapid slews and short settling times. The combination of finite element methods (FEM), coupled with control system dynamic analysis, provides a method to validate these specifications. An overview of these modeling activities is reported in this paper including specific cases that illustrate its impact.
The Dark Energy Spectroscopic Instrument, to be located at the prime focus of the Mayall telescope, includes a wide field corrector, a 5000 fiber positioner system, and a fiber view camera. The mapping of the sky to the focal plane, needed to position the fibers accurately, is described in detail. A major challenge is dealing with the large amount of distortion introduced by the optics (of order 10% scale change), including time-dependent non-axisymmetric distortions introduced by the atmospheric dispersion compensator. Solutions are presented to measure or mitigate these effects.
The Dark Energy Spectroscopic Instrument (DESI), currently under construction, is designed to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 40 million galaxies over 14000 sq deg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. This paper describes the overall design and construction status of the prime focus corrector. The size and complexity of the system poses significant design and production challenges. The optics of the corrector consists of six lenses, ranging from 0.8 - 1.14m in diameter, two of which can be rotated to act as an atmospheric dispersion corrector. These lenses are mounted in custom cells that themselves are mounted in a barrel assembly the alignment of which can be actively controlled by a hexapod system to micrometer precision. The whole assembly will be mounted at the prime focus of the Mayall 4m telescope at Kitt Peak observatory and will be one of the largest lens systems ever built for an optical telescope. Construction of the corrector began in 2014 and is well advanced. The system is due to be delivered to the telescope for installation in early 2018.
The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe, using the Baryon Acoustic Oscillation technique and the growth of structure using redshift-space distortions (RSD). The spectra of 40 million galaxies over 14000 square degrees will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. We will describe modeling and mitigation of stray light within the front end of DESI, consisting of the Mayall telescope and the corrector assembly. This includes the creation of a stray light model, quantitative analysis of the unwanted light at the corrector focal surface, identification of the main scattering sources, and a description of mitigation strategies to remove the sources.
The Dark Energy Spectroscopic Instrument (DESI), which is currently under construction, is designed to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 40 million galaxies over 14000 sq deg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fibre optic positioners. The fibres in turn feed ten broad-band spectrographs. The prime focus corrector for DESI consists of six lenses that range in diameter from 0.80 - 1.14 meters and from 83 - 237 kg in weight. The alignment of the large lenses of the optical corrector poses a significant challenge as in order to meet the fibre throughput requirements they have to be aligned to within a tolerance of ~50 micrometres. This paper details the design for the cells that will hold the lenses and the alignment and assembly procedure for the mounting of the lenses into the cells and into the complete barrel assembly. This is based on the experience obtained from the alignment of the Dark Energy Camera (DECam) instrument which was successfully assembled and aligned by the same team and we include in the paper the lessons learnt and design modifications that will be implemented on the DESI system.
The Large Synoptic Survey Telescope (LSST) is currently under construction and upon completion will perform precision photometry over the visible sky at a 3-day cadence. To meet the stringent relative photometry goals, LSST will employ multiple calibration systems to measure and compensate for systematic errors. This paper describes the design and development of these systems including: a dedicated calibration telescope and spectrograph to measure the atmospheric transmission function, a collimated beam projector to characterize the spatial dependence of the LSST transmission function and an at-field screen illumination system to measure the high-frequency variations in the global system response function.
At the core of the Large Synoptic Survey Telescope (LSST) three-mirror optical design is the primary/tertiary (M1M3) mirror that combines these two large mirrors onto one monolithic substrate. The M1M3 mirror was spin cast and polished at the Steward Observatory Mirror Lab at The University of Arizona (formerly SOML, now the Richard F. Caris Mirror Lab at the University of Arizona (RFCML)). Final acceptance of the mirror occurred during the year 2015 and the mirror is now in storage while the mirror cell assembly is being fabricated. The M1M3 mirror will be tested at RFCML after integration with its mirror cell before being shipped to Chile.
In the construction phase since 2014, the Large Synoptic Survey Telescope (LSST) is an 8.4 meter diameter wide-field (3.5 degrees) survey telescope located on the summit of Cerro Pachón in Chile. The reflective telescope uses an 8.4 m f/1.06 concave primary, an annular 3.4 m meniscus convex aspheric secondary and a 5.2 m concave tertiary. The primary and tertiary mirrors are aspheric surfaces figured from a monolithic substrate and referred to as the M1M3 mirror. This unique design offers significant advantages in the reduction of degrees of freedom, improved structural stiffness for the otherwise annular surfaces, and enables a very compact design. The three-mirror system feeds a threeelement refractive corrector to produce a 3.5 degree diameter field of view on a 64 cm diameter flat focal surface. This paper describes the current status of the mirror system components and provides an overview of the upcoming milestones including the mirror coating and the mirror system integrated tests prior to summit integration.
The LSST M1/M3 combines an 8.4 m primary mirror and a 5.1 m tertiary mirror on one glass substrate. The combined mirror was completed at the Richard F. Caris Mirror Lab at the University of Arizona in October 2014. Interferometric measurements show that both mirrors have surface accuracy better than 20 nm rms over their clear apertures, in nearsimultaneous tests, and that both mirrors meet their stringent structure function specifications. Acceptance tests showed that the radii of curvature, conic constants, and alignment of the 2 optical axes are within the specified tolerances. The mirror figures are obtained by combining the lab measurements with a model of the telescope’s active optics system that uses the 156 support actuators to bend the glass substrate. This correction affects both mirror surfaces simultaneously. We showed that both mirrors have excellent figures and meet their specifications with a single bending of the substrate and correction forces that are well within the allowed magnitude. The interferometers do not resolve some small surface features with high slope errors. We used a new instrument based on deflectometry to measure many of these features with sub-millimeter spatial resolution, and nanometer accuracy for small features, over 12.5 cm apertures. Mirror Lab and LSST staff created synthetic models of both mirrors by combining the interferometric maps and the small highresolution maps, and used these to show the impact of the small features on images is acceptably small.
The Dark Energy Spectroscopic instrument (DESI) is a 5000 fiber multi-object spectrometer system under development
for installation on the National Optical Astronomy Observatory (NOAO) Kitt Peak 4m telescope (the Mayall telescope).
DESI is designed to perform a 14,000° (square) galaxy and Quasi-Stellar Object (QSO) redshift survey to improve
estimates of the dark energy equation of state. The survey design imposes numerous constraints on a prime focus
corrector design, including field of view, geometrical blur, stability, fiber injection efficiency, zenith angle, mass and
cost. The DESI baseline wide-field optical design described herein provides a 3.2° diameter field of view with six 0.8-
1.14m diameter lenses and an integral atmospheric dispersion compensator.
The Large Synoptic Survey Telescope (LSST) relies on a set of calibration systems to achieve the survey photometric performances over a wide range of observing conditions. Its purpose is to consistently and accurately measure the observatory instrumental response and the atmospheric transparency during LSST observing. The instrumental response calibration will be performed regularly to monitor any variation of the transmission during the duration of the survey. The atmospheric data will be acquired nightly and processed to atmospheric models. In this paper, we describe the calibration screen system that will be used to perform the instrumental response calibration and the atmospheric calibration system including the auxiliary telescope dedicated to the acquisition of spectral data to determine the atmospheric transmission.
The closed-loop correction must be carry out before observation of Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) to eliminate the low-frequency errors. A natural guide star S-H sensor in the focal plane of LAMOST is used to conduct wave-front sensing. The designed limiting magnitude of the S-H sensor is 10th magnitude, and the beacon must be located in the center of field of view, or slightly deviated from the center. The survey time of LAMOST is 2 hours before and after transit, wherefore the active optical correction should be completed within half of an hour, so it is necessary to make the wave-front sensing time as short as possible. Since the magnitude of guide star and atmospheric seeing have important effect on the efficiency of wave-front sensing, 9th magnitude or brighter stars are adopted in operation. For 9th magnitude stars, sky coverage will be about 100%, but at most of time, the beacons are not located in the center of field of view, so we propose to design a laser guide system based on Rayleigh scattering to provide a beacon whose brightness is equivalent to a 7th or 8th magnitude star and to launch the beacon in the center of field of view at any observational sky. In this paper, we describe the optical design of the implementation involved a laser system with 532nm in wavelength, beam diagnostics, a launch telescope with 350mm in diameter, and receiving system.
High-resolution near-infrared echelle spectrographs require coarse rulings in order to match the free spectral range to the
detector size. Standard near-IR detector arrays typically are 2 K x 2 K or 4 K x 4 K. Detectors of this size combined
with resolutions in the range 30000 to 100000 require grating groove spacings in the range 5 to 20 lines/mm.
Moderately high blaze angles are desirable to reduce instrument size. Echelle gratings with these characteristics have
potential wide application in both ambient temperature and cryogenic astronomical echelle spectrographs. We discuss
optical designs for spectrographs employing immersed and reflective echelle gratings. The optical designs set constraints
on grating characteristics. We report on market choices for obtaining these gratings and review our experiments with
custom diamond turned rulings.
Microfluidic devices have been widely used in manipulation and analysis of individual cells in small-volume solutions. It
could be potentially used for studies of the interaction of THz radiation with biomolecules and cells in aqueous media.
We present a prototype microfluidic device that can be used for controlled cellular exposures to THz radiation. The
device is made of a PDMS microfluidic channel on glass substrate and consists of electrodes for cell concentration.
Initial cell concentration and THz transmission measurements have been performed on various prototype samples. Our
results demonstrate the feasibility of using microfluidic chips for potential “Lab-on-a-Chip” THz applications.
The Large Synoptic Survey Telescope (LSST) uses an Active Optics System (AOS) to maintain system alignment and surface figure on its three large mirrors. Corrective actions fed to the LSST AOS are determined from 4 curvature based wavefront sensors located on the corners of the inscribed square within the 3.5 degree field of view. Each wavefront sensor is a split detector such that the halves are 1mm on either side of focus. In this paper we describe the development of the Active Optics Pipeline prototype that simulates processing the raw image data from the wavefront sensors through to wavefront estimation on to the active optics corrective actions. We also describe various wavefront estimation algorithms under development for the LSST active optics system. The algorithms proposed are comprised of the Zernike compensation routine which improve the accuracy of the wavefront estimate. Algorithm development has been aided by a bench top optical simulator which we also describe. The current software prototype combines MATLAB modules for image processing, tomographic reconstruction, atmospheric turbulence and Zemax for optical ray-tracing to simulate the closed loop behavior of the LSST AOS. We describe the overall simulation model and results for image processing using simulated images and initial results of the wavefront estimation algorithms.
BigBOSS is a Stage IV dark energy experiment based on proven techniques to study baryon acoustic oscillations and the growth of large scale structure. The 2010 Astronomy and Astrophysics Decadal Survey labeled dark energy as a key area of exploration. BigBOSS is designed to perform a 14,000 square degree survey of 20 million galaxies and quasi-stellar objects. The project involves installation of a new instrument on the Mayall 4m telescope, operated by the National Optical
Astronomy Observatory. The instrument includes a new optical widefield corrector, a 5,000 fiber actuator system, and a multi-object spectrometer. Systems engineering flowdown from data set requirements to instrument requirements are discussed, along with the trade considerations and a pre-conceptual baseline design of the widefield optical corrector, spectrometer and fiber positioner systems.
The Large Synoptic Survey Telescope (LSST) has a 3.5º field of view and F/1.2 focus that makes the performance quite
sensitive to the perturbations of misalignments and mirror surface deformations. In order to maintain the image quality,
LSST has an active optics system (AOS) to measure and correct those perturbations in a closed loop. The perturbed
wavefront errors are measured by the wavefront sensors (WFS) located at the four corners of the focal plane. The
perturbations are solved by the non-linear least square algorithm by minimizing the rms variation of the measured and
baseline designed wavefront errors. Then the correction is realized by applying the inverse of the perturbations to the
optical system. In this paper, we will describe the correction processing in the LSST AOS. We also will discuss the
application of the algorithm, the properties of the sensitivity matrix and the stabilities of the correction. A simulation
model, using ZEMAX as a ray tracing engine and MATLAB as an analysis platform, is set up to simulate the testing and
correction loop of the LSST AOS. Several simulation examples and results are presented.
BigBOSS is a proposed DOE-NSF Stage IV ground-based dark energy experiment designed to study
baryon acoustic oscillations (BAO) and the growth of large scale structure with a 14,000 square
degree survey of the redshifts of galaxies and quasi-stellar objects. The project involves
modification of existing facilities operated by the National Optical Astronomy Observatory
(NOAO). Design and systems engineering of a preliminary 3 degree field of view refractive
corrector, atmospheric dispersion corrector (ADC), and 5000 actuator fiber positioning system are
presented.
KEYWORDS: Monochromatic aberrations, Mirrors, Off axis mirrors, Infrared telescopes, Radio optics, Infrared radiation, Signal to noise ratio, Radio telescopes, Telescopes, Astronomy
Off-axis systems in radio and infrared wavelengths have obvious advantages in suppressing aperture blockage and
background noise. Therefore, the signal-to-noise ratio as well as system gain is improved. However, an off-axis optical
system involves complex aberrations which limit its field of view. This paper provides an overview of aberrations in
axial symmetric and off-axis optical systems. As the system deviates from an axial symmetric one, system aberrations
become more and more complicated. In a general two mirror off-axis focusing system, the field of view is nearly zero.
Even for off-axis system with an equivalent parabola, the field of view is still very small as the linear astigmatism
dominates the system. An optimized off-axis system is one in which the linear astigmatism and cross polarization-free
conditions are met. In this optimized system, coma aberration is dominant, so that the field of view is still limited. The
field of view of an optimized off-axis system can be improved using a simple coma corrector system.
The Large Synoptic Survey Telescope (LSST) will continuously image the entire sky visible from Cerro Pachon
in northern Chile every 3-4 nights throughout the year. The LSST will provide data for a broad range of science
investigations that require better than 1% photometric precision across the sky (repeatability and uniformity)
and a similar accuracy of measured broadband color. The fast and persistent cadence of the LSST survey
will significantly improve the temporal sampling rate with which celestial events and motions are tracked. To
achieve these goals, and to optimally utilize the observing calendar, it will be necessary to obtain excellent
photometric calibration of data taken over a wide range of observing conditions - even those not normally
considered "photometric". To achieve this it will be necessary to routinely and accurately measure the full
optical passband that includes the atmosphere as well as the instrumental telescope and camera system. The
LSST mountain facility will include a new monochromatic dome illumination projector system to measure the
detailed wavelength dependence of the instrumental passband for each channel in the system. The facility will
also include an auxiliary spectroscopic telescope dedicated to measurement of atmospheric transparency at all
locations in the sky during LSST observing. In this paper, we describe these systems and present laboratory
and observational data that illustrate their performance.
The Large Synoptic Survey Telescope (LSST) flat-fields must repeatedly trace not only the spatial response variations,
but also the chromatic response through the entire optical system, with an accuracy driven by the photometric
requirements for the LSST survey data. This places challenging requirements on the LSST Calibration Dome Screen,
which must uniformly illuminate the 8.4-meter diameter telescope pupil over its 3.5-degree field of view at desired
monochromatic wavelengths in a way that allows the measurement of the total system throughput from entrance pupil to
the digitization of charge in the camera electronics. This includes the reflectivity of the mirrors, transmission of the
refractive optics and filters, the quantum efficiency of the sensors in the camera, and the gain and linearity of the sensor
read-out electronics. The baseline design uses a single tunable laser and includes an array of discrete projectors. The
projected flux of light produced by the screen must fill the entire telescope pupil and provide uniform illumination to 1%
at the focal plane and to within 0.25% over any optical trajectory within 0.5 degrees of each other. The wavelength of
light is tunable across the LSST bandpass from 320 nm to 1080 nm. The screen also includes a broad-band ("white")
light source with known Spectral Energy Density (SED) that spans the same range of wavelengths.
We present the as-built design overview and post-installation performance of the upgraded WIYN Bench Spectrograph.
This Bench is currently fed by either of the general-use multi-fiber instruments at the WIYN 3.5m telescope on Kitt
Peak, the Hydra multi-object positioner, and the SparsePak integral field unit (IFU). It is very versatile, and can be
configured to accommodate low-order, echelle, and volume phase holographic gratings. The overarching goal of the
upgrade was to increase the average spectrograph throughput by ~60% while minimizing resolution loss (< 20%). In
order to accomplish these goals, the project has had three major thrusts: (1) a new CCD was provided with a nearly
constant 30% increase is throughput over 320-1000 nm; (2) two Volume Phase Holographic (VPH) gratings were
delivered; and (3) installed a new all-refractive collimator that properly matches the output fiber irradiance (EE90) and
optimizes pupil placement. Initial analysis of commissioning data indicates that the total throughput of the system has
increased 50-70% using the 600 l/mm surface ruled grating, indicating that the upgrade has achieved its goal.
Furthermore, it has been demonstrated that overall image resolution meets the requirement of <20% loss.
The Large Synoptic Survey Telescope (LSST) is an 8.4 meter telescope with a field of view of 10 square
degrees. This telescope will be capable of mapping the entire visible sky every few nights via sequential 15-second exposures, opening new windows on the universe from dark energy to time variable objects. The
LSST optics calls for an annular 3.5 m diameter Secondary Mirror (M2), which is a large meniscus convex
asphere (ellipse). The M2 converts the beam reflected from the f/1.2 primary mirror into a beam for the f/0.83
Tertiary Mirror (M3). The M2 has a mass of approximately 1.5 metric tons and the mirror support system will
need to maintain the mirror figure at different gravity orientations. The optical performance evaluations were
made based on the optimized support systems consisting of 72 axial supports, mounted at the mirror back
surface, and 6 tangent link lateral supports mounted around the outer edge. The predicted print-though errors
of the M2 supports are 8nm RMS surface for axial gravity and 10nm RMS surface for lateral gravity. The
natural frequencies were calculated for the M2 dynamic performance. In addition, thermo-elastic analyses of
M2 for thermal gradient cases were conducted. The LSST M2 support system has an active optics capability
to maintain optical figure and its performance to correct low-order aberrations has been demonstrated. The
optical image qualities and structure functions for the axial and lateral gravity print-through cases, and
thermal gradient effects were calculated.
KEYWORDS: Telescopes, Space telescopes, Mirrors, Diagnostics, Adaptive optics, Electronics, Near field optics, Laser safety, Optical benches, Thirty Meter Telescope
The Thirty Meter Telescope (TMT) will implement a Laser Guide Star Facility (LGSF), which will generate up to nine
Na laser beams in at least four distinct asterisms. The TMT LGSF conceptual design is based upon three 50W solid state,
continuous wave, sum frequency 589 nm lasers and conventional beam transport optics. In this paper, we provide an
update to the TMT LGSF conceptual design. The LGSF top end and the beam transfer optics have been significantly
redesigned to compensate for the TMT telescope top end flexure, to adapt for the new TMT Ritchey-Chretien optical
design, to reduce the number of optical surfaces and to reduce the mass and volume. Finally, the laser service enclosure
has been relocated within the telescope azimuth structure. This will permit the lasers to operate with a fixed gravity
vector, but also requires further changes in the beam transport optical path.
The combination of immersion grating and infrared array detector technologies now allows the construction
of high-resolution spectrographs in the near-infrared that have capabilities approaching those of optical
spectrographs. It is possible, for instance, to design multi-object spectrographs with very large wavelength
coverage and high throughput. However, infrared spectrographs must be cryogenic and the cost of
complexity can be large. We investigate lower cost design options for single-object high-resolution
spectrographs. The trade-off in these designs is between the size/number of infrared arrays and the
inclusion of moving parts. We present a design for a no moving parts spectrograph with either 1.1-2.5 or 3-
5 μm simultaneous wavelength coverage. The design was undertaken with attention to cost as well as
scientific merit. Here we review the science drivers and key functional requirements. We present a general
overview of the instrument and estimate the limiting performance. The performance is compared with that
of medium-resolution infrared spectrographs as well as other high-resolution infrared spectrographs.
We describe the redesign and upgrade of the versatile fiber-fed Bench Spectrograph on the WIYN 3.5m telescope. The
spectrograph is fed by either the Hydra multi-object positioner or integral-field units (IFUs) at two other ports, and can
be configured with an adjustable camera-collimator angle to use low-order and echelle gratings. The upgrade, including
a new collimator, charge-coupled device (CCD) and modern controller, and volume-phase holographic gratings
(VPHG), has high performance-to-cost ratio by combining new technology with a system reconfiguration that optimizes
throughput while utilizing as much of the existing instrument as possible. A faster, all-refractive collimator enhances
throughput by 60%, nearly eliminates the slit-function due to vignetting, and improves image quality to maintain
instrumental resolution. Two VPH gratings deliver twice the diffraction efficiency of existing surface-relief gratings: A
740 l/mm grating (float-glass and post-polished) used in 1st and 2nd-order, and a large 3300 l/mm grating (spectral
resolution comparable to the R2 echelle). The combination of collimator, high-quantum efficiency (QE) CCD, and VPH
gratings yields throughput gain-factors of up to 3.5.
Atmospheric turbulence compensation via adaptive optics (AO) will be essential for achieving most objectives of the
TMT science case. The performance requirements for the initial implementation of the observatory's facility AO system
include diffraction-limited performance in the near IR with 50 per cent sky coverage at the galactic pole. This capability
will be achieved via an order 60x60 multi-conjugate AO system (NFIRAOS) with two deformable mirrors optically
conjugate to ranges of 0 and 12 km, six high-order wavefront sensors observing laser guide stars in the mesospheric
sodium layer, and up to three low-order, IR, natural guide star wavefront sensors located within each client instrument.
The associated laser guide star facility (LGSF) will consist of 3 50W class, solid state, sum frequency lasers,
conventional beam transport optics, and a launch telescope located behind the TMT secondary mirror.
In this paper, we report on the progress made in designing, modeling, and validating these systems and their components
over the last two years. This includes work on the overall layout and detailed opto-mechanical designs of NFIRAOS and
the LGSF; reliable wavefront sensing methods for use with elongated and time-varying sodium laser guide stars;
developing and validating a robust tip/tilt control architecture and its components; computationally efficient algorithms
for very high order wavefront control; detailed AO system modeling and performance optimization incorporating all of
these effects; and a range of supporting lab/field tests and component prototyping activities at TMT partners. Further
details may be found in the additional papers on each of the above topics.
The High-resolution Near-infrared Spectrograph (HRNIRS) concept for the Gemini telescopes combines a seeing-limited R ~ 70000 cross-dispersed mode and a MCAO-fed near diffraction-limited R ~ 20000 multi-object mode into a single compact instrument operating over the 0.9-5.5μm range. We describe the mechanical design, emphasizing the challenging design requirements and how they were met. The approach of developing the optical and mechanical designs in concert and utilizing proven working concepts from the Gemini Near Infra-Red Spectrograph were key elements of the design philosophy. Liang, et al. provides a detailed discussion of the optical design, Hinkle, et al. describes the science cases and requirements as well as a general overview, and Eikenberry, et al. describes the systems engineering and performance aspects of HRNIRS.
KEYWORDS: Mirrors, Actuators, Telescopes, Active optics, Control systems, Computer programming, Systems modeling, Adaptive optics, Monochromatic aberrations, Thirty Meter Telescope
The Thirty Meter Telescope (TMT) project is a partnership between ACURA, AURA, Caltech, and the University of California. The design calls for a 3.6 m diameter secondary mirror and an elliptical tertiary mirror measuring more than 4 m along its major axis. Each mirror will weigh more than two metric tons and must be articulated to compensate for deformation of the telescope structure. The support and control of these "smaller optics" pose significant challenges for
the designers. We present conceptual designs for active and passive figure control and articulation of these optics.
The Gemini Near-Infrared Spectrograph (GNIRS) supports a variety of observing modes over the 1-5 μm wavelength
region, matched to the infrared-optimized performance of the Gemini 8-m telescopes. We describe the optical,
mechanical, and thermal design of the instrument, with an emphasis on challenging design requirements and how they
were met. We also discuss the integration and test procedures used.
We present a preliminary optical design for a mid-infrared, high-resolution spectrograph (MIRES), together with an
integrated adaptive optics system optimized for the mid-infrared, intended for use on a 30-meter telescope. The design
includes laser guide star wavefront sensors, a near-infrared natural guide star wavefront sensor with a patrol field of 60
arcseconds, and near-infrared and mid-infrared imaging channels, in addition to the cross-dispersed spectrograph itself.
The spectrograph provides resolution of up to 120,000 and continuous spectral coverage over multiple cross-dispersed
orders, with high efficiency between 4.5 and 25 microns.
HRNIRS is an extremely versatile high-resolution infrared facility spectrograph designed for the Gemini South telescope. Operating over the 1.05 - 5.5 micron wavelength range, it has the capability to carry out a wide range of scientific programs by incorporating two separate modes of operation. The first is a conventional single slit cross-dispersed mode providing spectral resolution R ~ 70000 with a 0.4 arcsec slit over as much as an octave in wavelength, thus covering most of the JHK or LM windows in a single observation. In this mode the spectrograph accepts the Gemini seeing-limited f/16 input over a small field. A built-in modulator and polarizer allow HRNIRS to measure both linear and circular polarization. The second mode is a moderately-high resolution (R ~ 30000) spectrograph observing multiple objects simultaneously within a 2 arcmin field fed by the f/33.2 Gemini MCAO beam. In this paper, we discuss the optical design considerations, present the resulting design and show that the predicted performance meets the design requirements.
We present a discussion of the science drivers and design approach for a high-resolution, mid-infrared spectrograph for
the Thirty-Meter Telescope. The instrument will be integrated with an adaptive optics system optimized for the midinfrared;
as a consequence it is not significantly larger or more complex than similar instruments designed for use on
smaller telescopes. The high spatial and spectral resolution possible with such a design provides a unique scientific
capability. The design provides spectral resolution of up to 120,000 for the 4.5-25 μm region in a cross-dispersed format
that provides continuous spectral coverage of up to 2% to 14 μm. The basic concept is derived from the successful
TEXES mid-infrared spectrograph. To facilitate operation, there are separate imaging channels for the near-infrared and
the mid-infrared; both can be used for acquisition and the mid-infrared imaging mode can be used for science imaging
and for guiding. Because the spectrograph is matched to the diffraction limit of a 30-m telescope, gains in sensitivity are
roughly proportional to the square of the telescope diameter, opening up a volume within the Galaxy a thousand times
greater than existing instruments.
A feasibility design study was undertaken to assess the requirements of a mid-infrared echelle spectrograph (MIRES)
with a resolving power of 120,000 and its associated mid-infrared adaptive optics (MIRAO) system on the Thirty-Meter
Telescope. Our baseline design incorporates a 2K×2K Si:As array or array mosaic for the spectrograph and a 1K×1K
Si:As array for the slit viewer. Various tradeoffs were studied to minimize risk and to optimize the sensitivity of the
instrument. Major challenges are to integrate the spectrograph to the MIRAO system and, later, to an adaptive
secondary, the procurement of a suitable window and large KRS-5 lenses, and the acquisition of large format mid-IR
detector arrays suitable for the range of background conditions. We conclude that the overall risk is relatively low and
there is no technical reason that should prevent this instrument from being ready for use at first light on the Thirty-
Meter Telescope.
The High-Resolution Near-InfraRed Spectrograph (HRNIRS) concept for the Gemini telescopes combines a seeing limited R ~ 70000 cross-dispersed mode and an MCAO-fed near diffraction-limited R ~ 30000 multi-object mode into a single compact instrument operating over the 1 - 5 μm range. The HRNIRS concept was developed in response to proposals issued through the Aspen instrument process by Gemini. Here we review the science drivers and key functional requirements. We present a general overview of the instrument and estimate the limiting performance.
The Thirty Meter Telescope (TMT) will utilize adaptive optics to achieve near diffraction-limited images in the near-infrared using both natural and laser guide stars. The Laser Guide Star Facility (LGSF) will project up to eight Na laser beacons to generate guide stars in the Earth's Na layer at 90 - 110 km altitude. The LGSF will generate at least four distinct laser guide star patterns (asterisms) of different geometry and angular diameter to meet the requirements of the specific adaptive optics modules for the TMT instruments. We describe the baseline concept for this facility, which draws on the heritage from the systems being installed at the Gemini telescopes. Major subsystems include the laser itself and its enclosure, the optics for transferring the laser beams up the telescope structure and the asterism generator and launch telescope, both mounted behind the TMT secondary mirror. We also discuss operational issues, particularly the required safety interlocks, and potential future upgrades to higher laser powers and precompensation of the projected laser beacons using an uplink adaptive optics system.
KEYWORDS: Point spread functions, Absorption, Sensors, Spectrographs, Stars, Optical components, Velocity measurements, Gemini Observatory, Device simulation, Signal to noise ratio
The High-resolution Near-infrared Spectrograph (HRNIRS) concept for the Gemini telescopes combines a seeing-limited R ~ 7000 cross-dispersed mode and an MCAO-fed near diffraction-limited R ~ 20000 multi-object mode into a single compact instrument operating over the 0.9 - 5.5 μm range. We describe the systems engineering and performance modeling aspects of this study, emphasizing simulations of high-precision radial verlocity measurements in the Gemini Cassegrain-focus instrument environment.
We present a design of a thermal-infrared optimized adaptive optics system for the TMT 30-meter telescope. The
approach makes use of an adaptive secondary but during an initial implementation contains a more conventional
ambient-temperature optical relay and deformable mirror. The conventional optical relay is used without sacrificing the
thermal background by using multiple off-axis laser guide stars to avoid a warm dichroic in the common path. Three
laser guide stars, equally spaced 75" off axis, and a "conventional" 30×30 deformable mirror provide a Strehl > 0.9 at
wavelengths longer than 10 microns and the LGS beams can be passed to the LGS wavefront sensors with pickoff
mirrors while a one-arcminute field is passed unvignetted to the science instrument and NGS WFSs. The overall design
is relatively simple with a wavefront correction similar to existing high-order systems (e.g. 30×30) but still provides
competitive performance over the higher-order TMT NIR AO design at wavelengths as short as 3 microns due to its
reduced thermal emissivity. We present our figures of merit and design considerations within the context of the science
drivers for high-spectral resolution NIR/MIR spectroscopy at 5-28 microns on a 30-meter ground-based telescope.
In this paper, we provide an overview of the adaptive optics (AO) program for the Thirty Meter Telescope (TMT) project, including an update on requirements; the philosophical approach to developing an overall AO system architecture; the recently completed conceptual designs for facility and instrument AO systems; anticipated first light capabilities and upgrade options; and the hardware, software, and controls interfaces with the remainder of the observatory. Supporting work in AO component development, lab and field tests, and simulation and analysis is also discussed. Further detail on all of these subjects may be found in additional papers in this conference.
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.
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.
We present case studies on the application of passive compensation in two large astronomical instruments: the Gemini Near Infrared Spectrograph (GNIRS), including actual performance, and the NOAO Extremely Wide Field Infrared Mosaic (NEWFIRM) camera. Image motion due to gravity flexure is a problem in large astronomical instruments. We present solutions for two different cases using passive mechanical compensation of the optical train. For the Gemini Near Infrared Spectrograph (GNIRS), articulation of a single sensitive optic is used. Adjustable cantilevered weights, designed to respond to specific gravity components, are employed to drive tilt flexures connected to the collimator mirror. An additional requirement is that cryocooler vibration must not dynamically excite this mirror. Performance testing of the complete instrument shows that image motion has been satisfactorily compensated. Some image blur due to dynamic excitation by the cryocoolers was noted. A successful damping scheme has been developed experimentally. For the NOAO Extremely Wide Field Infrared Mosaic camera (NEWFIRM), the entire optical support structure is mechanically tuned to deflect and rotate precisely as a rigid body relative to the telescope focal plane. This causes the optical train to remain pointed at a fixed position in the focal plane, minimizing image motion on the science detector. This instrument is still in fabrication.
Wide field-of-view, high-resolution near-infrared cameras on 4-m class telescopes have been identified by the astronomical community as critical instrumentation needs in the era of 8-m and larger telescopes. Acting as survey instruments, they will provide the input source discoveries for large-telescope follow-up observations. The NOAO Extremely Wide Field Infrared Mosaic (NEWFIRM) imaging instrument will serve this need within the US system of facilities. NEWFIRM is being designed for the National Optical Astronomy Observatory (NOAO) 4-m telescopes (Mayall at KPNO and Blanco at CTIO). NEWFIRM covers a 28 x 28 arcmin field of view over the 1-2.4 μm wavelength range with a 4k x 4k pixel detector mosaic assembled from 2k x 2k modules. Pixel scale is 0.4 arcsec/pixel. Data pipelining and archiving are integral elements of the instrument system. We present the science drivers for NEWFIRM, and describe its optical, mechanical, electronic, and software components. By the time this paper is presented, NEWFIRM will be in the preliminary design stage, with first light expected on the Mayall telescope in 2005.
The Kitt Peak Mayall 4-m telescope required a new prime focus corrector having a flat focal plane covering 36 arcmin on a side (51 arcmin diagonal) to accommodate the Mosaic 8K X 8K CCD system. The scientific requirements for the new corrector included atmospheric dispersion compensation (ADC), excellent near-UV efficiency, excellent image quality, and extremely low scattered light and ghosting. The optical system designed to meet these demands exhibits excellent and stable performance through its first year of operation. This paper describes the innovative design and engineering aspects of the corrector. Science verification data are presented to demonstrate some of the attributes of the new corrector.
Recently, design examples of wide field three mirror Mersenne-Schmidt system had been presented by R.V. Willstrop. The work presented in this paper is an extension of Willstrop's early work. By applying overall system optimization, the maximum image size within a 4-degree field of a well-designed Mersenne-Schmidt system can be as small as 0.16 arc sec. If small edge vignetting is allowed, within a five-degree wider field of view, the maximum image size of the Mersenne-Schmidt system would be as small as 0.34 arc sec. In the second part of this paper, the Mersenne-Schmidt telescope is discussed in comparison with a Schmidt camera. Discussion shows that both systems can achieve a wider field of view. However, from astronomical requirements, the Mersenne-Schmidt telescope has better image quality, wider waveband coverage, greater light power, shorter tube length and larger usage area of the primary mirror. For a light collecting area larger than that of existing ones, the Mersenne-Schmidt telescope would be a better choice for astronomical frontier work.
Normally the atmosphere dispersion compensator (ADC) is a permanent fixture in the image corrector, even though at times the ADC is not needed. But, in Cassegrain focus it is possible to design a removable ADC, which can be taken out to achieve higher light transmission. Three such design examples are given in this paper. All of them are designed for the Cassegrain focus of the planned NOAO 8-meter telescope project. At this focus, the aberration corrector has three lenses. In the first two designs, the ADC has to be inserted between the second and third lens of the corrector; in the third the ADC is placed behind the third lens of the corrector. The first design requires adjustment of the secondary mirror of the telescope as well as the third lens of the aberration corrector when the ADC is inserted. The second design does not require any adjustment but requires two extra curved surfaces in the ADC. In the third design, the focal surface, the secondary mirror, and the third lens require adjustment. Spot diagrams of the three designs at three zenith distances are given.
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