Arcus is an innovative MIDEX-class photon-counting X-ray spectroscopy mission. Due to the nature of the sources that Arcus will focus on, observations can be many tens of kiloseconds (ks) long. The resulting spectral images are reconstructed on the ground to remove measured pointing and instrument deflection effects that take place over that time, achieving a higher resolution than would be possible without removing these effects. Arcus’s 12 m focal length grazing incidence optics are separated from the detectors by a 10.8 m long by Ø1.85 m, onorbit deployable boom. This paper describes an implementation of an internal aspect sensor that uses flight tested commercial off the shelf (COTS) components to measure linear deflection from one end of that boom to the other to achieve a better than 22 micron resolution (3σ) correction for that motion, meeting the required performance that Arcus needs to maintain its achieve its imaging resolution.
The Robert Stobie Spectrograph is currently the main workhorse spectroscopic instrument on the Southern African Large Telescope (SALT), which has been undergoing regular scientific operations since 2011. The visible beam of the RSS was designed to perform polarimetry in all of its modes, imaging and grating spectroscopy (with Multi Object Spectroscopy capability) from 3200 to 9000 Å. The polarimetric field of view is 4×8 arcmin. Initial early commissioning of the polarimetric modes was stalled in 2011 because a coupling fluid leak developed in the polarizing beamsplitter after less than a year of operation. As a result, it was decided to redesign the beamsplitter to use a different optical couplant. This was complicated by the unusual thermal expansion properties of the calcite optic, and by the necessity of aligning the individual elements in the beamsplitter mosaic (RSS is the first instrument to use a mosaic beamsplitter). Laboratory work selected a new couplant: a gel, Nye 451. Testing was completed with satisfactory results on a "sacrificial" calcite prism with the same geometry as an actual mosaic element. A successful assembly was performed and the beamsplitter was re-installed in SALT in mid-2015. We describe results from the renewed commissioning efforts to characterize polarimetry from SALT and include some early performance verification science.
Liquid lens coupling provides excellent transmission efficiency when compared to multilayer coatings especially for applications where broadband transmission is required. However, long term reliability of liquid coupling is difficult to achieve. This is typically due to chemical compatibility issues affecting both the optical transmission and the integrity of the opto-mechanical support. As part of a recent service of the Robert Stobie Spectrograph on SALT we had the opportunity to study these problems further and in this paper we provide analysis of problems identified and some solutions to prevent them. We also present general guidelines which could aid future opto-mechanical designs for liquid coupling of lenses.
The Robert Stobie Spectrograph Near Infrared Instrument (RSS-NIR), a prime focus facility instrument for the 11-meter
Southern African Large Telescope (SALT), is well into its laboratory integration and testing phase. RSS-NIR will
initially provide imaging and single or multi-object medium resolution spectroscopy in an 8 arcmin field of view at
wavelengths of 0.9 - 1.7 μm. Future modes, including tunable Fabry-Perot spectral imaging and polarimetry, have been
designed in and can be easily added later. RSS-NIR will mate to the existing visible wavelength RSS-VIS via a dichroic
beamsplitter, allowing simultaneous operation of the two instruments in all modes. Multi-object spectroscopy covering a
wavelength range of 0.32 - 1.7 μm on 10-meter class telescopes is a rare capability and once all the existing VIS modes
are incorporated into the NIR, the combined RSS will provide observational modes that are completely unique.
The VIS and NIR instruments share a common telescope focal plane, and slit mask for spectroscopic modes, and
collimator optics that operate at ambient observatory temperature. Beyond the dichroic beamsplitter, RSS-NIR is
enclosed in a pre-dewar box operating at -40 °C, and within that is a cryogenic dewar operating at 120 K housing the
detector and final camera optics and filters. This semi-warm configuration with compartments at multiple operating
temperatures poses a number of design and implementation challenges. In this paper we present overviews of the RSSNIR
instrument design and solutions to design challenges, measured performance of optical components, detector
system optimization results, and an update on the overall project status.
We report on extensive laboratory testing of the optical compatibility of immersion fluids often used in astronomical
instrumentation. A strong near-ultraviolet absorption feature is seen after incubating several fluids with polyurethane often
used in expansion bladders, and a lesser absorption in the farther UV with Viton O-Ring material. Substitute materials were
tested, many of which show no such absorption. This program was started in response to a strong UV feature which
developed over time in the Robert Stobie Spectrograph of the Southern African Large Telescope. A repair strategy was
successfully implemented.
The Prime Focus Imaging Spectrograph (PFIS) is a first light instrument for the Southern African Large Telescope
(SALT). PFIS is a versatile instrument designed to operate in a number of scientific modes by utilizing volume phase
holographic gratings, Fabry-Perot etalons, and polarimetric optics, which are manipulated in and out of the beam using
various placement mechanisms. The instrument is mounted at the prime focus 15m above the primary mirror and tilted at
37°. This remote placement and the need for 240° of rotation about the optical axis raises important design issues with
mass, flexure and access. The instrument structure provides the interface to the telescope Prime Focus Instrument
Platform (PFIP) as well as support points for all the optics, mechanisms and electrical equipment. The structure is a
welded open truss of hollow, square-section Invar beams. The open truss provides the highest stiffness to weight ratio
and minimizes the effect of wind loading, while the use of Invar negates the effects of thermal expansion. It has been
designed using finite element analysis in conjunction with an optical tolerance analysis of the optics nodes to minimize
effective image motion under the varying gravity load. The fundamentals of the design of the structure to minimize the
flexure and its effect on image motion, the motivation for using the open Invar truss structure, and the design of the
remotely operated mechanisms are discussed. In 2005 PFIS was installed and commissioned on SALT in South Africa.
Included in this text are some of the results and experiences of taking PFIS into operation.
The Echellette Spectrograph and Imager (ESI), currently being delivered for use at the Cassegrain focus of the Keck II telescope employs an all-spherical, 308 mm focal length f/1.07 Epps camera. The camera consists of 10 lens elements in 5 groups: an oil-coupled doublet; a singlet, an oil- coupled triplet; a grease-coupled triplet; and a field flattener, which also serves as the vacuum-dewar window. A sensitivity analysis suggested that mechanical manufacturing tolerances of order +/- 25 microns were appropriate. In this paper we discuss the sensitivity analysis, the assembly and the testing of this camera.
We describe a new telescope encoder that overcomes several traditional problems. The system uses a camera, a ruled scale, and a robust image processing algorithm to determine angular position. The ruled scale can be any of a variety of materials. The system is noncontacting, dirt insensitive, and has typical alignment tolerances of 0.25 mm.
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