Wide-Area Linear Optical Polarimeter (WALOP)-South is the first wide-field and survey-capacity polarimeter in the optical wavelengths. On schedule for commissioning in 2024, it will be mounted on the 1 m SAAO telescope in Sutherland Observatory, South Africa to undertake the PASIPHAE sky survey. PASIPHAE program will create the first polarimetric sky map in the optical wavelengths, spanning more than 2000 square degrees of the southern Galactic region. In a single exposure, WALOP-South’s innovative design will enable it to measure the linear polarization (Stokes parameters q and u) of all sources in a field of view (FoV) of 35 × 35 arc-minutes-squared in the SDSS-r broadband and narrowband filters between 500-750 nm with 0.1 % polarization accuracy. The unique goals of the instrument place very stringent systems engineering goals, including on the performance of the optical, polarimetric, optomechanical, and electronic subsystems. In particular, the major technical hurdles for the project included the development of: (a) an optical design to achieve imaging quality PSFs across the FoV, (b) an optomechanical design to obtain high accuracy optical alignment in conjugation with minimal instrument flexure and stress birefringence on optics (which can lead to variable instrumental polarization), and (c) an on-sky calibration routine to remove the strong polarimetric cross-talk induced instrumental polarization to obtain 0.1% across the FoV. All the subsystems have been designed carefully to meet the overall instrument performance goals. As of May 2024, all the instrument optical and mechanical subsystems have been assembled and are currently getting tested and integrated. The complete testing and characterization of the instrument in the lab is expected to be completed by August 2024. While the instrument was initially scheduled for commissioning in 2022, it got delayed due to various technical challenges; WALOP-South is now on schedule for commissioning in second half of 2024. In this paper, we will present (a) the design and development of the entire instrument and its major subsystems, focusing the instrument’s opto-mechanical design which has not been reported before, and (b) assembly and integration of the instrument in the lab and early results from lab characterization of the instrument’s optical performance.
The South African Astronomical Observatory’s (SAAO’s) “Intelligent Observatory” (IO) project is an initiative that aims to future-proof and strategically position the SAAO as a follow-up characterisation “machine” for transient alerts using the diverse facilities owned and hosted by the observatory. We present an overview of the many facilities available at the SAAO, with a particular emphasis on the new and upgraded facilities tailored towards autonomous rapid-response observing. Additionally, we delve into some of the scientific programs that currently leverage these new capabilities.
We present Mookodi (meaning “rainbow” in Sesotho), a multipurpose instrument with a low-resolution spectrograph mode and a multi-filter imaging mode for quick-reaction astronomical observations. The instrument, mounted on the 1-m Lesedi telescope at the South African Astronomical Observatory in Sutherland (South Africa), is based on the low-resolution spectrograph for the rapid acquisition of transients (SPRAT) instrument in operation on the 2-m Liverpool Telescope in La Palma (Canary Islands, Spain). Similar to SPRAT, Mookodi has a resolution R≈350 and an operating wavelength range in the visible (∼4000 to 8000 Å). The linear optical design, as in SPRAT, is made possible through the combination of a volume phase holographic transmission grating as the dispersive element and a prism pair (grism), which makes it possible to rapidly and seamlessly switch to an imaging mode by pneumatically removing the slit and grism from the beam and using the same detector as in spectrographic mode to image the sky. This imaging mode is used for auto-target acquisition, but the inclusion of filter slides in Mookodi’s design also provides the capability to perform imaging with a field-of-view ≈10′×10′ (∼0.6″/px) in the complete Sloan Digital Sky Survey filter set.
We present an overview of the Intelligent Observatory (IO) and the architecture used at the South African Astronomical Observatory (SAAO) to develop instrument and telescope control and monitoring software. The IO aims to link and coordinate the usage of the SAAO telescopes and instruments for optimal efficiency. This will entail a Central Control System (CCS) selecting appropriate instruments and telescopes and controlling observations on these. This requires interoperable instrument and telescope control software. The SAAO software architecture is flexible, allows multiple user interfaces, and supports remote control and monitoring of both telescope and instrument through a web browser. Furthermore, the architecture allows an external agent (such as the IO CCS) simultaneous control of both instruments and telescopes.
The SALT’s 91 primary mirror (PM) segments require annual recoating with aluminum because it is exposed to harsh environmental conditions during telescope operation. Recoating is used as a broad term entailing mirror segment removal, aluminizing and segment installation. Ideally, most large telescope, such as SALT, attempt to use individuals who are professionally educated and trained to handle optics for recoating of their primary mirrors. Unfortunately, South Africa doesn’t have tertiary institutions providing courses in optics or optical engineering. This paper describes how the SALT operations team overcame that challenge and trained and certified personnel, with no tertiary education whatsoever, recruited from the rural community of Sutherland, where SALT is located, by deskilling the individual PM segments handling and recoating tasks.
The SALT Building Management System (BMS) was designed to control sub-system cooling and environmental control in the telescope chamber as part of ensuring optimal science data quality. With over 400 inputs and output points for monitoring and control, this required an effective system when performing maintenance in the event of any failure or degradation of the system. The BMS lacked this effectiveness due to an unstructured design and a lack of documentation, causing time-consuming root cause analysis and excessive downtime. In this paper, we describe the research and development of an effective Building Management System.
The South African Astronomical Observatory (SAAO) is currently developing WiNCam, the Wide-field Nasmyth Camera, to be mounted on Lesedi, the observatory’s new 1-metre telescope. This paper discusses the design and results for the remotely-operated camera system. The camera consists of an E2V-231-C6 Back Illuminated Scientific Charge Coupled Device (CCD) sensor with 6144x6160 pixels, four outputs operating in non-inverted mode. This is to date the largest single chip CCD-system developed at SAAO. The CCD is controlled with a modified Inter-University Centre for Astronomy and Astrophysics (IUCAA) Digital Sampler Array Controller (IDSAC) utilizing digital correlated double sampling. The camera system will have full-frame and frame-transfer read out modes available with sub-windowing and pre-binning abilities. Vacuum through-wall PCB technology is used to route signals through the vacuum interface between the controller and the CCD. A thin, compact, 125x125mm aperture, sliding-curtain-mechanism shutter was designed and manufactured together with a saddle-type filter-magazine-gripper system. The CCD is cryogenically cooled using a Stirling Cooler with active vibration cancellation; CCD temperature control is done with a Lake Shore Temperature Controller. A Varian Ion Pump and Activated Charcoal are used to maintain good vacuum and to prolong intervals between vacuum pump down. The various hardware components of the system are connected using distributed software architecture, and a web-based GUI allows remote and scripted operation of the instrument.
KEYWORDS: Sensors, Telescopes, Mirrors, Environmental sensing, Humidity, Simulation of CCA and DLA aggregates, Temperature metrology, Control systems, Transmitters, Actuators
The Southern African Large Telescope (SALT) is a 10-m class 91-segment fixed altitude telescope located at Sutherland, South Africa. The segment alignment is maintained by inductively coupled sensors mounted on Sitall brackets beneath the segments. An extensive period of testing in environmental chambers and on the telescope has been conducted to establish the stability of the sensors and their response to temperature and humidity variations in the telescope chamber. We present some of the test results, including a demonstration of the ability of the sensors to maintain the alignment of the primary mirror over a period of 6 days.
The Southern African Large Telescope has till recently operated without active closed loop control of its Primary Mirror. The reason for this was that there were no suitable edge sensor system available on the market. Recently a system became available and SALT form Fogale Nanotech. The system consist of a sensor, cables and control electronics. The system was still under development and SALT was responsible for the integration of the sensors before deployment on the Telescope. Several issues still had to be addressed. One of these issues was the integration of the sensors at an appropriate production rate. The sensors was supplied as flexible pc boards with different types making up the transmitters and receivers. These flexible boards were bonded to ClearCeram Z L-Brackets before the appropriate connectors were installed. This paper describes the process used to integrate and test the sensors.
The development of an inductive edge sensor is in process for the control of the Southern African Large Telescope’s (SALT)1 segmented mirror primary. The original capacitive edge sensing system was not capable of maintaining the figure of the primary mirror due to excessive noise and a severe sensitivity to humidity despite exhaustive attempts at characterisation1. The prototype of the inductive edge sensor has progressed to a mature industrialised version that is in the process of being installed and commissioned on SALT. The performance of the sensor in response to temperature and RH is very good with a maximum error of 10nm typical after temperature compensation. The noise and control characteristics of the array have been simulated in order to establish the maximum cumulative error and error rate tolerable for the SALT specific case. It has been established through simulation that over the expected 5 day alignment cycle, a maximum cumulative error of 30nm can be tolerated.
This paper describes the cleaning of M5, one of the four mirrors that make up the Southern African Large Telescope's
Spherical Aberration Corrector. As the top upward-facing mirror in a relatively exposed environment, M5 had
accumulated a considerable amount of dust and dirt during the six years it had been on the telescope. With the corrector
on the ground for re-alignment and testing, we had the opportunity to remove, wash and replace the mirror. Various
cleaning techniques were investigated, including an unsuccessful trial application of First Contact surface cleaning
polymer film - fortunately only to a small region outside the mirror's clear aperture. Ultimately, "drag-wiping" with
wads of cotton wool soaked in a 10g/l sodium lauryl sulphate solution proved highly effective in restoring the reflectivity
of M5's optical surface. Following this success, we repeated the procedure for M3, the other upward-facing mirror in the
corrector. The results for M3 were equally spectacular.
KEYWORDS: Sensors, Mirrors, Environmental sensing, Space telescopes, Telescopes, Current controlled current source, Large telescopes, Nanotechnology, Sensor technology, Sensing systems
At the Southern African Large Telescope (SALT), in collaboration with FOGALE Nanotech, we have been testing the recently-developed new generation inductive edge sensors. The Fogale inductive sensor is one
technology being evaluated as a possible replacement for the now defunct capacitance-based edge sensing system.
We present the results of exhaustive environmental testing of two variants of the inductive sensor. In addition to the environmental testing including RH and temperature cycles, the sensor was tested for sensitivity to dust and metals. We also consider long-term sensor stability, as well as that of the electronics and of the glue used to bond the sensor to its supporting structure. A prototype design for an adjustable mount is presented which will allow for in-plane gap and shear variations present in the primary mirror configuration without adversely disturbing the figure of the individual mirror segments or the measurement accuracy.
The Southern African Large Telescope (SALT) recently (2008) abandoned attempts at using capacitive mirror edge
sensors, mainly due to poor performance at a relative humidity above ~60%, a not infrequent occurrence. Different
technologies are now being explored for alternative sensors on SALT. In this paper we describe the design and
development of a novel prototype optical edge sensor, based on the application of the interferential scanning principle,
as used in optical encoders. These prototype sensors were subsequently tested at SAAO and ESO, for potential
application on SALT and E-ELT.
Environmental tests, conducted in climatic control chambers, looked at temperature and relative humidity sensitivity,
long term stability and sensor noise. The temperature sensitivity for height and gap were, respectively, 10nm/°C and
44nm/°C, while for relative humidity they were 4nm/10% and 50nm/10%, respectively. These either met, or were close
to, the SALT specification. While there were significant lags in response, this was due to the sensor's relatively large
mass (~200 gm per sensor half), which was not optimized. This is likely to improve, should a revised design be
developed in future. Impressively the sensor noise was <0.015 nm RMS, over three orders of magnitude better than the
specification. Our conclusions are that optical edge sensing is a viable technique for use on segmented mirror telescopes.
KEYWORDS: Mirrors, Telescopes, Monochromatic aberrations, Image quality, Cameras, Simulation of CCA and DLA aggregates, Image segmentation, Wavefront sensors, Wavefronts, Interfaces
Construction of the Southern African Large Telescope (SALT) was largely completed by the end of 2005 and since then
it has been in intensive commissioning. This has now almost been completed except for the telescope's image quality
which shows optical aberrations, chiefly a focus gradient across the focal plane, along with astigmatism and other less
significant aberrations. This paper describes the optical systems engineering investigation that has been conducted since
early 2006 to diagnose the problem. A rigorous approach has been followed which has entailed breaking down the
system into the major sub-systems and subjecting them to testing on an individual basis. Significant progress has been
achieved with many components of the optical system shown to be operating correctly. The fault has been isolated to a
major optical sub-system. We present the results obtained so far, and discuss what remains to be done.
KEYWORDS: Sensors, Humidity, Mirrors, Temperature metrology, Sensing systems, Simulation of CCA and DLA aggregates, Telescopes, Calibration, Environmental sensing, Nanotechnology
The SAMS (Segment Alignment Measurement System) is a
capacitance-based edge sensing solution for the active
alignment of the 10m SALT segmented primary mirror. Commissioning and calibrating the system has been an ongoing
task in an attempt to counteract the unfavourable response of the sensors to high humidity conditions and high dust
levels. Several solutions were implemented and tested including
real-time feedback systems and the application of
corrective functions.
In parallel with the continuing efforts to improve the performance of the capacitive sensors, we have also been testing a
prototype inductive sensor developed by Fogale Nanotech that is of a very similar flexible plate construction.
In this paper we present the results obtained and performance gains achieved thus far with the capacitive edge-sensing
system as well as a performance comparison of the Fogale inductive sensor to the capacitive edge sensor.
Segmented primary mirrors dominate the current generation of 10m class telescopes as well as the designs for the next
generation of Extremely Large Telescopes (ELT's). The complex nature of these telescopes is demonstrated by the long
time periods associated with their commissioning and the difficulty of performing high precision optical alignments.
However, additional tools to provide in situ measurements of their optical alignment can be provided by making use of
the individual mirrors of a segmented primary; with the ability to move in six degrees of freedom, the individual mirrors
can be deployed to trace multiple optical paths through the telescope. In this paper we describe how it is possible to use
the segments themselves to create a number of Hartmann masks that allow focus and other aberrations to be measured
using a standard imaging camera rather than a dedicated wavefront sensor. The Southern African Large Telescope
(SALT), with a primary mirror composed of 91 1m segments, is used as an example. The segments were arranged to
create eight Hartmann masks to measure the optical alignment. Through imaging data obtained at the telescope, the
sensitivity of this method to changes in focus along with aberrations inherent in the system is demonstrated through
Zernike polynomial fits to the observed patterns. Finally, we present simulations of possible patterns for use on future
ELT's.
KEYWORDS: Sensors, Mirrors, Sensing systems, Humidity, Temperature metrology, Control systems, Simulation of CCA and DLA aggregates, Actuators, Environmental sensing, Large telescopes
The 10-m class Southern African Large Telescope (SALT) at Sutherland, South Africa, was inaugurated in November 2005, following completion of all its major sub-systems. It is the largest single optical telescope in the southern hemisphere. The SAMS (Segment Alignment Measurement System) is a unique capacitive edge sensing solution for the active alignment of the SALT primary mirror. Twelve thin film edge sensors are bonded directly onto the edges of each of the 91 segments, with heat-generating control electronics housed remotely in temperature-controlled enclosures. The SAMS is capable of measuring the tip/tilt and piston of each segment, as well as the change in global radius of curvature, a mode normally undetected by such a system. The primary objective was to build a system that offered an excellent cost-to-performance ratio without sacrificing measurement accuracy, a very necessary requirement because of the scale and number of sensors required for large segmented mirrors. This paper describes the results obtained during the commissioning and calibration of the completed system.
On completion by the end of 2004 the Southern African Large Telescope (SALT) being erected in Sutherland, South Africa, will be the largest single optical telescope in the southern hemisphere. This paper addresses the process of designing, building and demonstrating a high performance primary mirror system for SALT that meets the overall telescope requirements. Throughout the process consideration was given to the fact that SALT is budget sensitive, which required careful allocation of funds among the various subsystems, innovative designs, and using COTS components where possible. The process delivered subsystems with a very high cost-performance ratio.
The design of the Southern African Large Telescope (SALT), which is based closely on the Hobby-Eberly Telescope (HET) at the University of Texas but includes advances incorporating lessons learned from HET, is briefly reviewed. The flowdown of requirements from the optical error budget to the primary mirror control subsystems is presented. The techniques and algorithms used by the Center of Curvature Alignment Sensor (CCAS) to measure segment tilt and piston and estimate the global radius of curvature of the primary are discussed in detail. The steps in the process that allows CCAS to capture and identify segments misaligned by more than 70 arcsec and bring them into alignment with residual errors less than 50milli-arcsec is fully described. Next, the hardware and software designs of CCAS are presented, as well as the results of laboratory performance testing. CCAS has been installed and integrated with the primary mirror control system. Performance results of the integrated system over a range of environmental conditions will be shown. Finally, the overall results of this project are summarized and suggestions for future improvements presented.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.