KEYWORDS: Mirrors, Field programmable gate arrays, LabVIEW, Telescopes, Control systems, Observatories, Human-machine interfaces, Control systems design, Telecommunications, Actuators, Borosilicate glass
The Rubin Observatory’s Simonyi Survey Telescope M1M3 is a lightweight honeycomb 8.4 meter Ohara E- 6 borosilicate glass mirror, cast by the University of Arizona (UofA) Mirror Lab. It combines primary and tertiary mirror surfaces, hence its acronym. Its control software might be referenced as a 3rd generation UofA mirror active control system - after the Multiple Mirror Telescope’s (MMT) and the Large Binocular Telescope Observatory’s (LBTO). The control software uses a combination of LabVIEW Field Programmable Gate Array (FPGA),1 C++ (”back office”), and Python/Web (Graphical User Interface (GUI)/Engineering User Interface (EUI) to control the mirror. With the telescope’s first light expected soon, details of control software evolution, performed changes, as well as new development and status are described.
The Vera C. Rubin observatory will be performing numerous studies and high cadence surveys. In order to perform the surveys most efficiently, the observations need to be planned in an optimal way, taking into account numerous atmospheric effects such as the current weather conditions and cloud cover. Building on the heritage from the MASCARA station, the DREAM team is developing the cloud & transmission monitoring system. The DREAM station is an upgraded version of the MASCARA station, which has been already been successfully operational on La Palma, Canary Islands, Spain, and La Silla, Chile. Using a set of wide-field cameras, nearly the full local sky is imaged every 6.4 seconds. Using calibrated brightness measurements of all bright stars (V < 8.4) in the field of view, the transmission and extinction is monitored, at a 30-60 seconds cadence. DREAM is currently being assembled and tested in the Netherlands and is expected to be deployed on-site by the end of 2022.
Uniquely designed with two 8.4m mirrors, a 22.8m interferometric baseline, and the collecting area of an 11.8m telescope, the Large Binocular Telescope Observatory (LBTO), has a narrow window of opportunity to exploit its status as the “first” of the ELTs. Prompted by urgency to maximum scientific output during this favorable interval, we undertook a multi-year project to reshape the user experience. The initial stage, implementing a new suite of software to facilitate proposal submission, script creation, binocular planning, and nighttime execution, is nearing completion. Reuse and adaptation of existing software, particularly Gemini Observatory’s cross-platform PIT and OT, proved critical, although as expected, we encountered many challenges presented by our one-of-a-kind binocular design and operations. We hope to leverage our success in the early phases of this project toward further improvement of our science operations model, specifically, augmenting our nighttime operations to include observatory-led observing. We plan to focus this observing mode primarily on instruments that require block scheduling and/or superb and rare conditions such as our newly commissioned GLAO system, ARGOS. In this paper, we outline our workflow, describe lessons learned, and present our resulting software products. We also detail future development toward our ultimate goal, improved efficiency and user interactions throughout every step of the observing experience.
The Arizona Robotic Telescope Network (ARTN) project is a long term effort to develop a system of telescopes to carry out a flexible program of PI observing, survey projects, and time domain astrophysics including monitoring, rapid response, and transient/target-of-opportunity followup. Steward Observatory operates and shares in several 1-3m class telescopes with quality sites and instrumentation, largely operated in classical modes. Science programs suited to these telescopes are limited by scheduling flexibility and people-power of available observers. Our goal is to adapt these facilities for multiple co-existing queued programs, interrupt capability, remote/robotic operation, and delivery of reduced data. In the long term, planning for the LSST era, we envision an automated system coordinating across multiple telescopes and sites, where alerts can trigger followup, classification, and triggering of further observations if required, such as followup imaging that can trigger spectroscopy. We are updating telescope control systems and software to implement this system in stages, beginning with the Kuiper 61” and Vatican Observatory 1.8-m telescopes. The Kuiper 61” and its Mont4K camera can now be controlled and queue-scheduled by the RTS2 observatory control software, and operated from a remote room at Steward. We discuss science and technical requirements for ARTN, and some of the challenges in adapting heterogenous legacy facilities, scheduling, data pipelines, and maintaining capabilities for a diverse user base.
RTS2 is an open source observatory control system. Being developed from early 2000, it continue to receive new features in last two years. RTS2 is a modulat, network-based distributed control system, featuring telescope drivers with advanced tracking and pointing capabilities, fast camera drivers and high level modules for ”business logic” of the observatory, connected to a SQL database. Running on all continents of the planet, it accumulated a lot to control parts or full observatory setups.
The LSST Camera science sensor array will incorporate 189 large format Charge Coupled Device (CCD) image sensors.
Each CCD will include over 16 million pixels and will be divided into 16 equally sized segments and each segment will
be read through a separate output amplifier.
The science goals of the project require CCD sensors with state of the art performance in many aspects. The broad
survey wavelength coverage requires fully depleted, 100 micrometer thick, high resistivity, bulk silicon as the imager
substrate. Image quality requirements place strict limits on the image degradation that may be caused by sensor effects:
optical, electronic, and mechanical.
In this paper we discuss the design of the prototype sensors, the hardware and software that has been used to perform
electro-optic testing of the sensors, and a selection of the results of the testing to date. The architectural features that lead
to internal electrostatic fields, the various effects on charge collection and transport that are caused by them, including
charge diffusion and redistribution, effects on delivered PSF, and potential impacts on delivered science data quality are
addressed.
We describe a complex process needed to turn an existing, old, operational observatory - The Steward Observatory’s 61” Kuiper Telescope - into a fully autonomous system, which observers without an observer. For this purpose, we employed RTS2,1 an open sourced, Linux based observatory control system, together with other open sourced programs and tools (GNU compilers, Python language for scripting, JQuery UI for Web user interface). This presentation provides a guide with time estimates needed for a newcomers to the field to handle such challenging tasks, as fully autonomous observatory operations.
We report here on the software Hack Day organised at the 2014 SPIE conference on Astronomical Telescopes and Instrumentation in Montréal. The first ever Hack Day to take place at an SPIE event, the aim of the day was to bring together developers to collaborate on innovative solutions to problems of their choice. Such events have proliferated in the technology community, providing opportunities to showcase, share and learn skills. In academic environments, these events are often also instrumental in building community beyond the limits of national borders, institutions and projects. We show examples of projects the participants worked on, and provide some lessons learned for future events.
X-rays frames offer a lot of information about CCD. 55Fe sources are traditionally being used for CCD gain and charge transfer efficiency (CTE) measurements. The pixel size of modern scientific CCDs is getting smaller. The charge diffusion causes the charge spread among neighboring pixels especially in thick fully depleted sensors. This enables measurement of the charge diffusion using 55Fe X-rays. On the other hand, the usual CTE char- acterization method based on single pixel X-ray events becomes statistically deficient. A new way of measuring CTE using shape and amplitude analysis of X-ray clusters is presented and discussed. This method requires high statistical samples. Advances in test automation and express analysis technique allows for acquiring such statistical samples in a short period of time. The details of our measurement procedure are presented. The lateral diffusion measured using e2v CCD250 is presented and implications for X-ray cluster size and expected cluster shape are discussed. The CTE analysis using total X-ray cluster amplitude is presented. This analysis can reveal CTE problems for certain conditions. The statistical analysis of average X-ray cluster shape is presented. Characteristics X-rays can be used for the whole system absolute calibration. We demonstrate how spectral features of 55Fe and 241Am rad. sources are used for system linearity measurements.
Tight requirements on the Large Synoptic Survey Telescope point spread function (PSF) demand sensor contribution
to PSF be both small and well characterized. The sensor PSF is determined by the lateral charge
diffusion on the drift path from the photon conversion point to the gates. The maximum drift path occurs
for photons converted at the window, for blue optical photons in particular. Charges generated at the window
surface undergo "worst case" charge spreading and the blue optical PSF is used to characterize the sensor's PSF.
Different techniques for charge diffusion characterization have been developed, each with its own systematics
and measurement difficulties. A new way to measure charge diffusion using an X-ray source is presented. We
demonstrate the effectiveness and limitations of our technique and discuss relation of charge diffusion value
obtained with X-ray measurements to sensor PSF.
The Reionization And Transients InfraRed (RATIR) camera has been built for rapid Gamma-Ray Burst (GRB)
followup and will provide quasi-simultaneous imaging in ugriZY JH. The optical component uses two 2048 × 2048
pixel Finger Lakes Imaging ProLine detectors, one optimized for the SDSS u, g, and r bands and one optimized
for the SDSS i band. The infrared portion incorporates two 2048 × 2048 pixel Teledyne HgCdTe HAWAII-2RG
detectors, one with a 1.7-micron cutoff and one with a 2.5-micron cutoff. The infrared detectors are controlled by
Teledyne's SIDECAR (System for Image Digitization Enhancement Control And Retrieval) ASICs (Application
Specific Integrated Circuits). While other ground-based systems have used the SIDECAR before, this system
also utilizes Teledyne's JADE2 (JWST ASIC Drive Electronics) interface card and IDE (Integrated Development
Environment). Here we present a summary of the software developed to interface the RATIR detectors with
Remote Telescope System, 2nd Version (RTS2) software. RTS2 is an integrated open source package for remote
observatory control under the Linux operating system and will autonomously coordinate observatory dome,
telescope pointing, detector, filter wheel, focus stage, and dewar vacuum compressor operations. Where necessary
we have developed custom interfaces between RTS2 and RATIR hardware, most notably for cryogenic focus stage
motor drivers and temperature controllers. All detector and hardware interface software developed for RATIR
is freely available and open source as part of the RTS2 distribution.
RTS2, or Remote Telescope System 2nd Version, is a modular observatory control system. Development of RTS2 began in 2003 and since then it has been used at more than 20 observatories world-wide. Its main users are small, fully autonomous observatories, performing target of opportunity observations.
Since June 2007 RTS2 has been used at Brookhaven National Laboratory (BNL) to control the acquisition of images for the Large Synoptic Survey Telescope (LSST) CCD characterisation. The CCD test laboratory includes multiple devices which need to be controlled in order to perform the electro-optical testing of the CCD.
The configuration of the devices must be recorded in order for that information to be used later during data analysis.
The main factors leading to use of RTS2 were its availability, open - source code, and modular design which allows its fast customisation to fit changing needs of a R&D project.
This article focuses on the description of changes to the system which allow for the integration of LSST's
multiple output CCD imagers. The text provides details of the multiple channel implementation, which parts
of the system were affected, and how these changes influenced overall system design. It also describes how easy
and fast it was to run the multiple channel instrument on night and twilight sky during prototype CCD testing,
and demonstrates how the complex routines, such as twilight skyflats acquisitions, worked out of the box.
RTS2, or Remote Telescope System 2nd Version, is an open-source, distributed and modular observatory control
system. During the course of its development lasting over a decade, the original goal to develop software capable
of searches for optical transients of
γ-ray bursts changed to develop a system for full control of large observatories
executing complex observing scenarios.
In this presentation, we would like to share our experience with meta-queues scheduling, developed primarily
for automation of the FLWO 1.2m telescope. Meta-queues scheduling allows observers to quickly build and com-
bine dierent observational scenarios, while still retaining ToO and weather interruption capabilities. Thanks
to the queues and scheduling graphical user interface, observers can use the system without the need to under-
stand complex functions used in the traditional merit function scheduling. By combining meta-queues and merit
function scheduling, observatories can oer dierent options to schedule their observations to their users, so the
acquired data will match the observers' expectations.
Petr Kubánek, Alberto Castro-Tirado, Antonio de Ugarte Postigo, Ronan Cunniffe, Michael Prouza, Jan Štrobl, Hendrik van Heerden, Javier Gorosabel, René Hudec, Phil Yock, William Allen, Ian Bond, Grant Christie, Sergei Guziy, Lorraine Hanlon, Martin Jelínek, Seamus Meehan, Cyril Polášek, Victor Reglero, Primo Vitale
We discuss our experiences operating a heterogeneous global network of autonomous observatories. The observatories
are presently situated on four continents, with a fifth expected during the summer of 2010. The network
nodes are small to intermediate diameter telescopes (<= 150 cm) owned by different institutions but running the
same observatory control software. We report on the experience gained during construction, commissioning and
operation of the observatories, as well as future plans. Problems encountered in the construction and operation
of the nodes are summarised. Operational statistics as well as scientific results from the observatories are also
presented.
We present the latest modifications of the open source observatory control software package RTS2. New features
were developed specifically for the automated testing of CCD chips for the mosaic camera of the Large Synoptic
Survey Telescope. Currently, the system is in operation at Brookhaven National Laboratory in Upton, USA and
at Laboratoire de Physique Nucl´eaire et des Hautes ´Energies in Paris, France. RTS2 software is currently used to
characterize the sensors from various vendors and will be used first for selection and then for testing of production
CCD sensors. With our system we are able to automatically obtain a series of images for analysis. Data is used
to study many aspects of sensor characteristics, including wavelength dependence of quantum efficiency, the dark
current, and the linearity of the CCD response as a function of back-bias voltage and temperature. We also can
measure a point spread function over the whole surface of the CCD sensors.
KEYWORDS: Observatories, Telescopes, Charge-coupled devices, Sensors, Space telescopes, Control systems design, C++, CCD image sensors, Image processing, Control systems
For almost a decade we have been developing an open source control system for autonomous observatories
called Remote Telescope System, 2nd version - RTS2. The system is currently used to operate about dozen
observatories. It was designed from the beginning as the ultimate tool for autonomously performing any possible
observing plan on any hardware. Its modular design allows exactly this and enables even more. Currently it
is used to control not only observatories but also CCD testing laboratories. We present the internal design of
this open source observatory and laboratory control package, and discuss its overall structure. We emphasise
new developments and our experiences building a community of users and developers of the package. Design
of the system modularity is explained in detail, and various approaches to software reuse are discussed, with a
demonstration of how the best solution emerged. We describe problems that were encountered as mirror sizes
and associated operational complexity grew. We also describe how the system is being used at a CCD testing
laboratory, and detail the quick transition from previously unsupported hardware to fully automated operation.
We discuss how the system's evolution has affected code design, and present unexpected benefits it is brought.
Our experience with use of open source code and libraries are discussed.
OCTOCAM is a multi-channel imager and spectrograph that has been proposed for the 10.4m GTC telescope. It will use
dichroics to split the incoming light to produce simultaneous observations in 8 different bands, ranging from the
ultraviolet to the near-infrared. The imaging mode will have a field of view of 2' x 2' in u, g, r, i, z, J, H and KS bands,
whereas the long-slit spectroscopic mode will cover the complete range from 4,000 to 23,000 A with a resolution of 700
- 1,000 (depending on the arm and slit width). An additional mode, using an image slicer, will deliver a spectral
resolution of over 3,000. As a further feature, it will use state of the art detectors to reach high readout speeds of the
order of tens of milliseconds. In this way, OCTOCAM will be occupying a region of the time resolution - spectral
resolution - spectral coverage diagram that is not covered by a single instrument in any other observatory, with an
exceptional sensitivity.
Future wide field astronomical surveys, like Large Synoptic Survey Telescope (LSST), require photometric precision
on the percent level. The accuracy of sensor calibration procedures should match these requirements. Pixel
size variations found in CCDs from different manufacturers are the source of systematic errors in the flat field
calibration procedure. To achieve the calibration accuracy required to meet the most demanding science goals
this effect should be taken into account.
The study of pixel area variations was performed for fully depleted, thick CCDs produced in a technology
study for LSST. These are n-channel, 100μm thick devices.
We find pixel size variations in both row and column directions. The size variation magnitude is smaller in
the row direction. In addition, diffusion is found to smooth out electron density variations. It is shown that the
characteristic diffusion width can be extracted from the flat field data.
Results on pixel area variations and diffusion, data features, analysis technique and modeling technique are
presented and discussed.
Remote Telescope System 2nd version (RTS2) is an open source project aimed at developing a software environment
to control a fully robotic observatory. RTS2 consists of various components, which communicate via
an ASCII based protocol. As the protocol was from the beginning designed as an observatory control system,
it provides some unique features, which are hard to find in the other communication systems. These features
include advanced synchronisation mechanisms and strategies for setting variables. This presentation describes
the protocol and its unique features. It also assesses protocol performance, and provides examples how the RTS2
library can be used to quickly build an observatory control system.
BIRCAM is a near-infrared (0.8-2.5um) cryogenic camera based on a 1Kx1K HgCdTe array. It was designed for - and
is now mounted at - one of the Nasmyth foci of the fast-slewing 0.6 m BOOTES-IR telescope at the Sierra Nevada
Observatory (OSN) in Spain. The primary science mission is prompt Gamma Ray-Burst afterglow research, with an
implied demand for extremely time-efficient operation. We describe the challenges of installing a heavy camera on a
small high-speed telescope, of integrating the dithering mechanism, the filterwheel, and the array itself into a high-efficiency
instrument, the design of the software to meet the requirements.
We present a novel design of an all-sky 4096×4096 pixels camera devoted to continuous observations of the sky.
A prototype camera is running at the BOOTES-1 astronomical station in Huelva (Spain) since December 2002
and a second one is working at the BOOTES-2 station in Málaga (Spain) since July 2004. Scientific applications
are the search for simultaneous optical emission associated to gamma-ray bursts, study of meteor showers, and
determination of possible areas for meteorite recovery from the reconstruction of fireball trajectories. This last
application requires that at least two such devices for simultaneously recording the sky at distance of the order
of ~ 100 km. Fifteen GRB error boxes (13 for long/soft events and 2 for short/hard GRBs) have been imaged
simultaneously to the gamma-ray emission, but no optical emission has been detected. Bright fireballs have been
also recorded, allowing the determination of trajectories, as in the case of the fireball of 30 July 2005. This device
is a very promising instrument for continuous recording of the night sky with moderate angular resolution and
limiting magnitude (up to R ~ 10).
"BOOTES-IR" is the extension of the BOOTES experiment, which has been operating in Southern Spain since
1998, to the near-infrared (nIR). The goal is to follow up the early stage of the gamma ray burst (GRB)
afterglow emission in the nIR, as BOOTES does already at optical wavelengths. The scientific case that drives
the BOOTES-IR performance is the study of GRBs with the support of spacecraft like HETE-2, INTEGRAL and
SWIFT (and GLAST in the future). Given that the afterglow emission in both, the nIR and the optical, in the
instances immediately following a GRB, is extremely bright (reached V = 8.9 in one case), it should be possible
to detect this prompt emission at nIR wavelengths too. Combined observations by BOOTES-IR and BOOTES-1
and BOOTES-2 since 2006 can allow for real time identification of trustworthy candidates to have a ultra-high
redshift (z > 6). It is expected that, few minutes after a GRB, the nIR magnitudes be H ~ 10-15, hence very
high quality spectra can be obtained for objects as far as z = 10 by much larger ground-based telescopes. A
significant fraction of observing time will be available for other scientific projects of interest, objects relatively
bright and variable, like Solar System objects, brown dwarfs, variable stars, planetary nebulae, compact objects
in binary systems and blazars.
RTS2, or Remote Telescope System, 2nd Version, is an integrated package for remote telescope control under the Linux operating system. It is designed to run in fully autonomous mode, picking targets from a database table, storing image meta data to the database, processing images and storing their WCS coordinates in the database and offering Virtual-Observatory enabled access to them. It is currently running on various telescope setups world-wide. For control of devices from various manufacturers we developed an abstract device layer, enabling control of all possible combinations of mounts, CCDs, photometers, roof and cupola controllers.
We describe the evolution of RTS2 from Python-based RTS to C and later C++ based RTS2, focusing on the problems we faced during development. The internal structure of RTS2, focusing on object layering, which is used to uniformly control various devices and provides uniform reporting layer, is also discussed.
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