Editing Robotic telescope (section)

==Professional robotic telescopes==
Robotic telescopes were first developed by [[astronomer]]s after [[electromechanical]] interfaces to [[computer]]s became common at [[observatory|observatories]]. Early examples were expensive, had limited capabilities, and included 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, 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 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 [[Obsolescence|obsolete]] because the [[graduate student]]s 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 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 {{visible anchor|Automated Telescope Facility}} (ATF), developed in the early 1990s, was located on the roof of the physics building at the University of Iowa in [[Iowa City, Iowa|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 star]]s and contributed observations to dozens of [[scientific paper]]s. 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 the Talon program.<ref>{{cite web |url=http://www.sierrastars.com/gp/Rigel/RigelTelescope.aspx |title=About Rigel |access-date=2009-02-14 |url-status=dead |archive-url=https://web.archive.org/web/20090130014917/http://sierrastars.com/gp/Rigel/RigelTelescope.aspx |archive-date=2009-01-30 }}</ref> 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 [[United Kingdom|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, 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 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 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 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{{When|date=May 2021}} RAPTOR has been re-tuned to be the key hardware element of the Thinking Telescopes Technologies Project.<ref>{{Cite web|last=Hutterer|first=Eleanor|date=August 2014|title=Tracking Transients|url=http://www.thinkingtelescopes.lanl.gov/}}</ref> Its new mandate will be 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 a 38&nbsp;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 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. 

{{Further|Fenton Hill Observatory#RAPTOR}}