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36-630: The Liverpool Telescope ( LT ) is a two-metre-aperture robotic Ritchey–Chrétien telescope that observes autonomously (without human intervention). However professional astronomers, school groups and other credible registered users submit specifications to be considered by its robotic control system (RCS) at any time using an online graphical user interface . Each night the RCS decides among these choices, and among any notified or glimpsed transient events, what to observe, based on target visibility and weather conditions. The telescope had first light in 2003, and

72-431: A 38 km baseline. Supporting these wide field systems are two other operational telescopes. The first of these is a cataloging patrol instrument with a mosaic 16 square degree field of view down to 16 magnitude. The other system is a .4m OTA with a yielding a depth of 19-20th magnitude and a coverage of .35 degrees. Three additional systems are currently undergoing development and testing and deployment will be staged over

108-461: A few professional facilities (see following section). The need for proprietary software is usually driven by the competition for research dollars between institutions. Since the late 1980s, the University of Iowa has been in the forefront of robotic telescope development on the professional side. The Automated Telescope Facility (ATF), developed in the early 1990s, was located on the roof of

144-413: A large number of unique subsystems, both in hardware and software. This contributed to a lack of progress in the development of robotic telescopes early in their history. By the early 1980s, with the availability of cheap computers, several viable robotic telescope projects were conceived, and a few were developed. The 1985 book, Microcomputer Control of Telescopes , by Mark Trueblood and Russell M. Genet,

180-477: A robotic telescope system points itself and collects its data without inspecting the results of its operations to ensure it is operating properly. An open loop telescope is sometimes said to be operating on faith, in that if something goes wrong, there is no way for the control system to detect it and compensate. A closed loop system has the capability to evaluate its operations through redundant inputs to detect errors. A common such input would be position encoders on

216-424: A web-based user interface. RTS2 was from the beginning designed as a completely open source system, without any proprietary components. In order to support growing list of mounts, sensors, CCDs and roof systems, it uses own, text based communication protocol. The RTS2 system is described in papers appearing in 2004 and 2006. The Instrument Neutral Distributed Interface (INDI) was started in 2003. In comparison to

252-530: Is computer software that implements a mathematical model of conditions leading to errors in telescope pointing and tracking. The model can then be used in a telescope control system to correct the pointing and tracking. Such errors are typically caused by mechanical or structural defects . For example, TPoint can analyze and compensate for systematic errors such as polar misalignment , mechanical and optical non-orthogonality, lack of roundness in telescope mounting drive gears , as well as for flexure of

288-513: Is also widely used by amateur astronomers . Software Bisque distributes TPoint as an add-on to TheSkyX Serious Astronomer Edition and TheSkyX Professional; this version is used to improve the pointing on amateur telescopes. TPoint was invented and developed by Patrick Wallace. It grew out of work he and John Straede performed at the Anglo-Australian Telescope (AAT) between 1974 and 1980 using Interdata 70 computers. In

324-638: Is one of the primary players in the Heterogeneous Telescope Networks Consortium, a global collaboration between major research groups in the field of robotic telescopes which seeks a standard for communication between remote telescopes, telescope users, and other scientific resources. Plans for an improved version, the Liverpool Telescope 2, are underway. Robotic telescope By 2004, robotic observations accounted for an overwhelming percentage of

360-815: Is operated (maintained) by the Astrophysics Research Institute , partly funded by the UK's STFC . It is at the Roque de los Muchachos Observatory on La Palma . Along with the Faulkes Telescope North and South , it is available for use by school children around the world over the internet. The registration and time allocation for the LT is organised by the National Schools Observatory. The Liverpool Telescope

396-443: Is the brainchild and property of Liverpool John Moores University . The RCS has a rapid-response capability where it will often automatically interrupt regular observations to slew (shift) to observe short-lived events with higher priority, such as gamma-ray bursts . The LT is one of the largest robotic telescopes in the world and was built by a subsidiary set up by Liverpool John Moores University who own and masterminded it. It

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432-751: The Microsoft Windows centric ASCOM standard, INDI is a platform independent protocol developed by Elwood C. Downey of ClearSky Institute to support control, automation, data acquisition, and exchange among hardware devices and software frontends. A newer introduction to the consumer market are smart telescopes. They are self contained robotic astronomical imaging devices that combine a small (50mm to 114mm in diameter) telescope and mount with pre-packaged software designed for astrophotography of deep-sky objects . They use GPS data and automatic star pattern recognition ( plate solving ) to find out where they are pointed. They have no optical system that allows

468-874: The Tenagra Observatories site near Cottage Grove, Oregon was constructed by Michael Schwartz with a robotic 14-inch (360 mm) Celestron Schmidt-Cassegrain telescope c. 1998. Meanwhile, ASCOM users designed ever more capable master control systems. Papers presented at the Minor Planet Amateur-Professional Workshops (MPAPW) in 1999, 2000, and 2001 and the International Amateur-Professional Photoelectric Photometry Conferences of 1998, 1999, 2000, 2001, 2002, and 2003 documented increasingly sophisticated master control systems. Some of

504-400: The graduate students who wrote it move on to new positions, and their institutions lose their knowledge. Large telescope consortia or government funded laboratories don't tend to have this same loss of developers as experienced by universities. Professional systems generally feature very high observing efficiency and reliability. There is also an increasing tendency to adopt ASCOM technology at

540-450: The 1970s, notably the 3.9m Anglo-Australian Telescope . In 2004, some professional robotic telescopes were characterized by a lack of design creativity and a reliance on closed source and proprietary software . The software is usually unique to the telescope it was designed for and cannot be used on any other system. Often, robotic telescope software developed at universities becomes impossible to maintain and ultimately obsolete because

576-596: The Robotic Optical Transient Search Experiment (ROTSE) wide-field telescope array, named ROTSE-I, began operation in manual mode. Software systems allowed fully automated robotic operation in late March 1998, with the first automated responses to GRB 980326 from triggers received over the GRB Coordinates Network. ROTSE-I operated from then on and was the first fully autonomous closed-loop robotic telescope, and

612-678: The Talon program. Each of these was a progression toward a more automated and utilitarian observatory. One of the largest current networks of robotic telescopes is RoboNet , operated by a consortium of UK universities. The Lincoln Near-Earth Asteroid Research (LINEAR) Project is another example of a professional robotic telescope. LINEAR's competitors, the Lowell Observatory Near-Earth-Object Search , Catalina Sky Survey , Spacewatch , and others, have also developed varying levels of automation. In 1997,

648-400: The capabilities of these systems included automatic selection of observing targets, the ability to interrupt observing or rearrange observing schedules for targets of opportunity, automatic selection of guide stars, and sophisticated error detection and correction algorithms. Remote telescope system development started in 1999, with first test runs on real telescope hardware in early 2000. RTS2

684-410: The detector (typically a CCD camera), control of the dome or telescope enclosure, control over the telescope's focuser , detection of weather conditions, and other capabilities. Frequently these varying subsystems are presided over by a master control system, which is almost always a software component. Robotic telescopes operate under closed loop or open loop principles. In an open loop system,

720-498: The development of amateur robotic telescopes has been the tedium of making research-oriented astronomical observations, such as taking endlessly repetitive images of a variable star. In 1998, Bob Denny conceived of a software interface standard for astronomical equipment, based on Microsoft 's Component Object Model , which he called the Astronomy Common Object Model (ASCOM). He also wrote and published

756-401: The explosion of amateur robotic telescopes was the availability of relatively inexpensive CCD cameras, which appeared on the commercial market in the early 1990s. These cameras not only allowed amateur astronomers to make pleasing images of the night sky, but also encouraged more sophisticated amateurs to pursue research projects in cooperation with professional astronomers. The main motive behind

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792-436: The first examples of this standard, in the form of commercial telescope control and image analysis programs, and several freeware components. He also convinced Doug George to incorporate ASCOM capability into a commercial camera control software program. Through this technology, a master control system that integrated these applications could easily be written in perl , VBScript , or JavaScript . A sample script of that nature

828-552: The goal of RAPTOR was to develop a system of ground-based telescopes that would reliably respond to satellite triggers and more importantly, identify transients in real-time and generate alerts with source locations to enable follow-up observations with other, larger, telescopes. It has achieved both of these goals. Now RAPTOR has been re-tuned to be the key hardware element of the Thinking Telescopes Technologies Project. Its new mandate will be

864-477: The monitoring of the night sky looking for interesting and anomalous behaviors in persistent sources using some of the most advanced robotic software ever deployed. The two wide field systems are a mosaic of CCD cameras. The mosaic covers and area of approximately 1500 square degrees to a depth of 12th magnitude. Centered in each wide field array is a single fovea system with a field of view of 4 degrees and depth of 16th magnitude. The wide field systems are separated by

900-518: The mounting caused by gravity . TPoint is in use on the majority of professional telescopes worldwide, including among many others the Anglo-Australian Telescope , Keck Observatory , Gemini Observatory and the Large Binocular Telescope . It has significantly improved the performance and efficiency of telescope operation and has had an especially strong impact on the development of automated and robotic telescopes . TPoint

936-472: The next two years. All of the systems are mounted on custom manufactured, fast-slewing mounts capable of reaching any point in the sky in 3 seconds. The RAPTOR System is located on site at Los Alamos National Laboratory (USA) and has been supported through the Laboratory's Directed Research and Development funds. In 2004, most robotic telescopes are in the hands of amateur astronomers . A prerequisite for

972-711: The physics building at the University of Iowa in Iowa City . They went on to complete the Iowa Robotic Observatory , a robotic and remote telescope at the private Winer Observatory in 1997. This system successfully observed variable stars and contributed observations to dozens of scientific papers . In May 2002, they completed the Rigel Telescope . The Rigel was a 0.37-meter (14.5-inch) F/14 built by Optical Mechanics, Inc. and controlled by

1008-469: The published scientific information on asteroid orbits and discoveries, variable star studies, supernova light curves and discoveries, comet orbits and gravitational microlensing observations. All early phase gamma ray burst observations were carried by robotic telescopes. Robotic telescopes are complex systems that typically incorporate a number of subsystems. These subsystems include devices that provide telescope pointing capability, operation of

1044-630: The telescope is set up. They can be operated remotely and are able to collect a series of images unattended. They can automate various techniques of astrophotography, including " lucky imaging " and " speckle imaging ". The design of the imaging system, combined with relatively small optics, are not optimal for imaging planets or the Moon. Examples include models from the French companies Unistellar and Vaonis. See below for further information on these professional robotic telescopes: Tpoint TPoint

1080-526: The telescope's axes of motion, or the capability of evaluating the system's images to ensure it was pointed at the correct field of view when they were exposed. Most robotic telescopes are small telescopes . While large observatory instruments may be highly automated, few are operated without attendants. Robotic telescopes were first developed by astronomers after electromechanical interfaces to computers became common at observatories . Early examples were expensive, had limited capabilities, and included

1116-400: The user to directly view astronomical objects and instead send an image captured over time via image stacking to a built in digital display (usually shaped like a conventional eyepiece ), or to a smartphone or tablet . They come with a database of pre-programmed objects, per-determined imaging routines, and Mobile app software that allows the end user to begin astrophotography as soon as

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1152-415: Was a landmark engineering study in the field. One of this book's achievements was pointing out many reasons, some quite subtle, why telescopes could not be reliably pointed using only basic astronomical calculations. The concepts explored in this book share a common heritage with the telescope mount error modeling software called Tpoint , which emerged from the first generation of large automated telescopes in

1188-479: Was primary intended for Gamma ray burst follow-up observations, so ability to interrupt observation was core part of its design. During development, it became an integrated observatory management suite. Other additions included use of the Postgresql database for storing targets and observation logs, ability to perform image processing including astrometry and performance of the real-time telescope corrections and

1224-642: Was provided by Denny. Following coverage of ASCOM in Sky & Telescope magazine several months later, ASCOM architects such as Bob Denny, Doug George, Tim Long , and others later influenced ASCOM into becoming a set of codified interface standards for freeware device drivers for telescopes, CCD cameras, telescope focusers, and astronomical observatory domes. As a result, amateur robotic telescopes have become increasingly more sophisticated and reliable, while software costs have plunged. ASCOM has also been adopted for some professional robotic telescopes. Also in 1998,

1260-477: Was used for GRB responses, X-ray transients and Soft Gamma-ray Repeater study, variable star and meteor study. The first prompt optical burst from a GRB was discovered by ROTSE-I for GRB 990123. The ROTSE-III project involved four half-meter telescopes based on the ROTSE-I operation approach, which began operation in 2003. These were used primarily for GRB follow up study, and also a supernova search and study. It

1296-560: Was with ROTSE-III observations that the first superluminous supernovae were discovered. In 2002, the RAPid Telescopes for Optical Response (RAPTOR) project, designed in 2000, began full deployment in 2002. The project was headed by Tom Vestrand and his team: James Wren, Robert White, P. Wozniak, and Heath Davis. Its first light on one of the wide field instruments was in late 2001. The second wide field system came online in late 2002. Closed loop operations began in 2003. Originally

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