The SCALES instrument being developed at UC Observatories is designed to take spectra of directly imaged exoplanets in the thermal infrared (1-5 microns). The ability to switch from science imaging mode to pupil imaging mode to taking spectra at specific wavelengths requires precision mechanical subsystems to enable these different modes of operation at cryogenic temperatures. In this paper we discuss the design of a rotary stage that can position different Lyot masks, as well as different high precision metal optics to enable some of the broad functionality of SCALES. We will also review some of the analysis involved with validating the design, and specifics pertaining to the design of the precision mirrors mounted to this stage.
We present preliminary laboratory cryogenic testing and validation results for the first rotary stage for SCALES (Slicer Combined with an Array of Lenslets for Exoplanet Spectroscopy). SCALES is a 2-5 micron high-contrast lenslet integral field spectrograph currently undergoing final design and testing for the W. M. Keck Observatory. The rotary stage, known as the Lyot mechanism, is a rotating wheel with 15 selectable pupil masks and optics. When deployed behind the Keck Adaptive Optics system, SCALES will be used to detect and characterize a wide variety of exoplanets. To minimize thermal emission, all optical and mechanical components of SCALES are fully cryogenic. Testing was first performed at ambient temperatures and pressures, then validated under vacuum at cryogenic temperatures.
SCALES (Slicer Combined with Array of Lenslets for Exoplanet Spectroscopy) is the next-generation, diffraction-limited, thermal infrared, fully cryogenic, coronagraphic exoplanet spectrograph and imager for W.M. Keck Observatory. SCALES is fed by the Keck II Adaptive Optics bench. Both modes use common fore-optics to simplify the optical design and have individual detectors, which are JWST flight spares. The imager mode operates from 1 to 5 microns with selectable narrow- and broadband filters over a field of view 12.3 arcseconds on a side, and the integral field spectrograph mode operates from 2 to 5 microns with both low and mid spectral resolutions (R∼ 100 to R∼ 7500) over a field of view 2.15 arcseconds on a side. The diamond-turned aluminum optics, most of which are already delivered, with the rest being fabricated, provide low distortion, low wavefront error, and high throughput for all modes. The slicing unit, located behind the lenslet array, allows SCALES to reach heretofore unheard-of spatially-resolved spectral resolution for exoplanet and disc observations from the ground with a coronagraphic integral field spectrograph. The SCALES consortium includes UC Observatories, CalTech, W.M. Keck Observatory, the Indian Institute of Astrophysics, and the University of Durham, with over 40 science team members. We report on the overall design and project status during its ongoing fabrication phase, which started in early 2023.
Since the start of science operations in 1993, the twin 10-meter W. M. Keck Observatory (WMKO) telescopes have continued to maximize their scientific impact and to produce transformative discoveries that keep the observing community on the frontiers of astronomical research. Upgraded capabilities and new instrumentation are provided though collaborative partnerships with Caltech, the University of California, and the University of Hawaii instrument development teams, as well as industry and other organizations. This paper summarizes the performance of recently commissioned infrastructure projects, technology upgrades, and new additions to the suite of observatory instrumentation. We also provide a status of projects currently in design or development phases and, since we keep our eye on the future, summarize projects in exploratory phases that originate from our 2022 strategic plan developed in collaboration with our science community to adapt and respond to evolving science needs.
The new deployable tertiary mirror for the Keck I telescope (K1DM3) at the W. M. Keck Observatory has been assembled, tested and shipped to the telescope site, and is currently being installed. The mirror is capable of reflecting the beam to one of six positions around the telescope elevation ring or to retract out of the way to allow the use of Cassegrain instruments. This new functionality is intended to allow rapid instrument changes for transient event observations and improve telescope operations. This paper presents the final as-built design. Additionally, this paper presents detailed information about our alignment approach in the attempt to duplicate the instrument pointing orientation of the existing M3.
The Keck Cosmic Web Imager (KCWI) is a new facility instrument being developed for the W. M. Keck Observatory and funded for construction by the Telescope System Instrumentation Program (TSIP) of the National Science Foundation (NSF). KCWI is a bench-mounted spectrograph for the Keck II right Nasmyth focal station, providing integral field spectroscopy over a seeing-limited field up to 20" x 33" in extent. Selectable Volume Phase Holographic (VPH) gratings provide high efficiency and spectral resolution in the range of 1000 to 20000. The dual-beam design of KCWI passed a Preliminary Design Review in summer 2011. The detailed design of the KCWI blue channel (350 to 700 nm) is now nearly complete, with the red channel (530 to 1050 nm) planned for a phased implementation contingent upon additional funding. KCWI builds on the experience of the Caltech team in implementing the Cosmic Web Imager (CWI), in operation since 2009 at Palomar Observatory. KCWI adds considerable flexibility to the CWI design, and will take full advantage of the excellent seeing and dark sky above Mauna Kea with a selectable nod-and-shuffle observing mode. In this paper, models of the expected KCWI sensitivity and background subtraction capability are presented, along with a detailed description of the instrument design. The KCWI team is lead by Caltech (project management, design and implementation) in partnership with the University of California at Santa Cruz (camera optical and mechanical design) and the W. M. Keck Observatory (program oversight and observatory interfaces). The optical design of the blue camera for the Keck Cosmic Web Imager (KCWI) by Harland Epps of the University of California, Santa Cruz is a lens assembly consisting of eight spherical optical elements. Half the elements are calcium fluoride and all elements are air spaced. The design of the camera barrel is unique in that all the optics are secured in their respective cells with an RTV annulus without additional hardware such as retaining rings. The optical design and the robust lens mounting concept has allowed UCO/Lick to design a straightforward lens camera assembly. However, alignment sensitivity is a strict 15 μm for most elements. This drives the fabrication, assembly, and performance of the camera barrel.
KEYWORDS: Mirrors, Telescopes, Astronomy, Calibration, Sensors, Distortion, Data modeling, Spectroscopy, James Webb Space Telescope, Magnetic resonance imaging
Motivated by the ever increasing pursuit of science with the transient sky (dubbed Time Domain Astronomy or TDA), we are fabricating and will commission a new deployable tertiary mirror for the Keck I telescope (K1DM3) at the W.M. Keck Observatory. This paper presents the detailed design of K1DM3 with emphasis on the opto- mechanics. This project has presented several design challenges. Foremost are the competing requirements to avoid vignetting the light path when retracted against a sufficiently rigid system for high-precision and repeatable pointing. The design utilizes an actuated swing arm to retract the mirror or deploy it into a kinematic coupling. The K1DM3 project has also required the design and development of custom connections to provide power, communications, and compressed air to the system. This NSF-MRI funded project is planned to be commissioned in Spring 2017.
The Lick Observatory's Shane 3-meter telescope has been upgraded with a new infrared instrument (ShARCS - Shane Adaptive optics infraRed Camera and Spectrograph) and dual-deformable mirror adaptive optics (AO) system (ShaneAO). We present first-light measurements of imaging sensitivity in the Ks band. We compare mea- sured results to predicted signal-to-noise ratio and magnitude limits from modeling the emissivity and throughput of ShaneAO and ShARCS. The model was validated by comparing its results to the Keck telescope adaptive optics system model and then by estimating the sky background and limiting magnitudes for IRCAL, the pre- vious infra-red detector on the Shane telescope, and comparing to measured, published results. We predict that the ShaneAO system will measure lower sky backgrounds and achieve 20% higher throughput across the JHK bands despite having more optical surfaces than the current system. It will enable imaging of fainter objects (by 1-2 magnitudes) and will be faster to reach a fiducial signal-to-noise ratio by a factor of 10-13. We highlight the improvements in performance over the previous AO system and its camera, IRCAL.
The University of California Observatories will design and construct a deployable tertiary mirror (named K1DM3) for the Keck 1 telescope, which will complement technical and scientific advances in the area of time-domain astronomy. The K1DM3 device will enable astronomers to swap between any of the foci on Keck 1 in under 2 minutes, both to monitor varying sources (e.g. stars orbiting the Galactic center) and catch rapidly fading sources (e.g. supernovae, flares, gamma-ray bursts). In this paper, we report on the design development during our in-progress Preliminary Design phase. The design consists of a passive wiffle tree axial support system and a diaphragm lateral support system with a 5 arcminute field-of-view mirror. The mirror assembly is inserted into the light path with an actuation system and it relies on a kinematic mechanism for achieving repeatable, precise positioning. This project, funded by an NSF MRI grant, aspires to complete by the end of 2016.
A new high-order adaptive optics system is now being commissioned at the Lick Observatory Shane 3-meter telescope in California. This system uses a high return efficiency sodium beacon and a combination of low and high-order deformable mirrors to achieve diffraction-limited imaging over a wide spectrum of infrared science wavelengths covering 0.8 to 2.2 microns. We present the design performance goals and the first on-sky test results. We discuss several innovations that make this system a pathfinder for next generation AO systems. These include a unique woofer-tweeter control that provides full dynamic range correction from tip/tilt to 16 cycles, variable pupil sampling wavefront sensor, new enhanced silver coatings developed at UC Observatories that improve science and LGS throughput, and tight mechanical rigidity that enables a multi-hour diffraction-limited exposure in LGS mode for faint object spectroscopy science.
A Cassegrain mounted adaptive optics instrument presents unique challenges for opto-mechanical design. The flexure and temperature tolerances for stability are tighter than those of seeing limited instruments. This criteria requires particular attention to material properties and mounting techniques. This paper addresses the mechanical designs developed to meet the optical functional requirements. One of the key considerations was to have gravitational deformations, which vary with telescope orientation, stay within the optical error budget, or ensure that we can compensate with a steering mirror by maintaining predictable elastic behavior. Here we look at several cases where deformation is predicted with finite element analysis and Hertzian deformation analysis and also tested. Techniques used to address thermal deformation compensation without the use of low CTE materials will also be discussed.
The Automated Planet Finder (APF) is a new telescope on Mount Hamilton with an instrument designed and built by
UCO. During the development of the instrument's camera lens assembly the largest optical element fractured during
fabrication. The glass grade is a relatively robust material and not known for any special sensitivity. Transient thermal
and structural FEA modeling was performed on the element geometry for several glass materials to better understand the
mechanics involved and the relative nature of the properties and response of the glass that failed. Results show that the
glass in question yielded the highest surface stresses of all those considered and high internal stresses as well. The
analysis technique described here is a simple tool that can be used to evaluate a material and make valid comparisons
with others.
In this article we present the mechanical design and the manufacturing of the support structure for the Reionization And
Transients InfraRed (RATIR) camera. The instrument is mounted at the f/13 Cassegrain focus of the 1.5-meter Harold
Johnson telescope of the Observatorio Astronómico Nacional at San Pedro Mártir (OAN/SPM) in Mexico. We describe
the high-level requirements and explain their translation to the mechanical specifications and requirements. We describe
the structural finite-element analysis and the boundary conditions, loads, and general assumptions included in the
simulations. We summarize the expected displacements, rotations and stresses. We present the optomechanical
components and the elements used to attach the instrument to the telescope. Finally, we show the instrument installed on
the telescope.
The Keck Cosmic Web Imager (KCWI) is a new facility instrument being developed for the W. M. Keck Observatory
and funded for construction by the Telescope System Instrumentation Program (TSIP) of the National Science
Foundation (NSF). KCWI is a bench-mounted spectrograph for the Keck II right Nasmyth focal station, providing
integral field spectroscopy over a seeing-limited field up to 20"x33" in extent. Selectable Volume Phase Holographic
(VPH) gratings provide high efficiency and spectral resolution in the range of 1000 to 20000. The dual-beam design of
KCWI passed a Preliminary Design Review in summer 2011. The detailed design of the KCWI blue channel (350 to
700 nm) is now nearly complete, with the red channel (530 to 1050 nm) planned for a phased implementation contingent
upon additional funding. KCWI builds on the experience of the Caltech team in implementing the Cosmic Web Imager
(CWI), in operation since 2009 at Palomar Observatory. KCWI adds considerable flexibility to the CWI design, and will
take full advantage of the excellent seeing and dark sky above Mauna Kea with a selectable nod-and-shuffle observing
mode. In this paper, models of the expected KCWI sensitivity and background subtraction capability are presented,
along with a detailed description of the instrument design. The KCWI team is lead by Caltech (project management,
design and implementation) in partnership with the University of California at Santa Cruz (camera optical and
mechanical design) and the W. M. Keck Observatory (program oversight and observatory interfaces).
The Ken and Gloria Levy Spectrometer is now operational at a new 2.4 meter telescope on Mt. Hamilton. Together the
spectrometer and telescope comprise the Automated Planet Finder (APF), a radial velocity instrument. A catastrophic
failure occurred during transit as the instrument was being shipped to the observatory. Several struts buckled in the space
frame that supported the echelle grating. This event has caused UCO/Lick to re-evaluate design methodology and how
engineering safety factors apply to this type of structure. This paper describes the shipping container design, events
during shipment, the failure mechanism, testing and analysis of a remedy, and its implementation. We also suggest
design changes to prevent similar failures in the future.
We aim to build a new tertiary mirror (M3) and its mount for the 10 m Keck I (K1) telescope at the W. M. Keck
Observatory (WMKO) to make its full observational capabilities available for time-sensitive scientific programs.. In
contrast to the existing tertiary mirror and mount, the device will rapidly deploy and rotate the mirror to any instrument
at a Nasmyth focus or, as desired, stow the mirror out of the light path to permit observations at the Cassegrain focus. In
this manner, the K1 deployable tertiary mirror (K1DM3) will enable observations with any of the K1 instruments on any
given night, and at any given time. The K1DM3 device will be integrated within the K1 telescope control system and
WMKO has committed to a new operations model that takes full advantage of this new capability.
The Lick Observatory 3-meter telescope has a history of serving as a testbed for innovative adaptive optics techniques.
In 1996, it became one of the first astronomical observatories to employ laser guide star (LGS) adaptive optics as a
facility instrument available to the astronomy community. Work on a second-generation LGS adaptive optics system,
ShaneAO, is well underway, with plans to deploy on telescope in 2013. In this paper we discuss key design features and
implementation plans for the ShaneAO adaptive optics system. Once again, the Shane 3-m will host a number of new
techniques and technologies vital to the development of future adaptive optics systems on larger telescopes. Included is a
woofer-tweeter based wavefront correction system incorporating a voice-coil actuated, low spatial and temporal
bandwidth, high stroke deformable mirror in conjunction with a high order, high bandwidth MEMs deformable mirror.
The existing dye laser, in operation since 1996, will be replaced with a fiber laser recently developed at Lawrence
Livermore National Laboratories. The system will also incorporate a high-sensitivity, high bandwidth wavefront sensor
camera. Enhanced IR performance will be achieved by replacing the existing PICNIC infrared array with an Hawaii
2RG. The updated ShaneAO system will provide opportunities to test predictive control algorithms for adaptive optics.
Capabilities for astronomical spectroscopy, polarimetry, and visible-light adaptive optical astronomy will be supported.
The Ken and Gloria Levy Spectrometer is being constructed at the Instrument Development Laboratory (Technical
Facilities) of UCO/ Lick Observatory for use on the 2.4 meter Automated Planet Finder Telescope at Mt. Hamilton. The
mechanical design of the instrument has been optimized for precision Doppler measurements. A key component of the
design is the space-frame structure that contains passive thermal compensation. Determinate hexapod structures are used
to mount the collimator, prism, and echelle grating. In this paper we describe the instrument mechanical design and some
features that will help it detect rocky planets in the habitable zone.
Within the general astronomical community as well as at the University of California Observatories, there has been a
long history of using epoxy to mount optics within instruments such as spectrometers and telescopes. The Ken & Gloria
Levy Spectrometer, part of the Automated Planet Finder (APF) telescope located at Mt. Hamilton's Lick Observatory,
relies on epoxy-bonded joints to attach the instrument's large cross-dispersing prism and echelle grating to its Invar
space-frame structure. Design constraints dictated that these large optics each be attached at only three points, and that
the bond areas be as small as possible while maintaining an adequate strength factor of safety. Previous UCO
instruments, such as the Keck Telescopes' primary mirror segments and the ESI Spectrometer, used Hysol's 9313 epoxy
product for this purpose. Concerns over long-term reliability of such joints led us to re-examine this issue. We
empirically investigated the roles played by epoxy selection and techniques such as surface preparation and the use of a
primer, in creating a robust metal-to-glass bond. Bond strength data was generated, leading us to select a previously
unused epoxy, and to implement particular techniques to ensure bond quality. Most notably, we found that bond strength
data as typically reported on adhesive manufacturers' datasheets was not a reliable indicator of long-term bond reliability
between metal and optical glass.
A mosaic of two 2k x 4k fully depleted, high resistivity CCD
detectors was installed in the red channel of the Low Resolution
Imaging Spectrograph for the Keck-I Telescope in June, 2009 replacing
a monolithic Tektronix/SITe 2k x 2k CCD. These CCDs were fabricated
at Lawrence Berkeley National Laboratory (LBNL) and packaged and
characterized by UCO/Lick Observatory. Major goals of the detector
upgrade were increased throughput and reduced interference fringing
at wavelengths beyond 800 nm, as well as improvements in the
maintainability and serviceability of the instrument. We report on
the main features of the design, the results of optimizing detector
performance during integration and testing, as well as the
throughput, sensitivity and performance of the instrument as
characterized during commissioning.
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