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Journal articles on the topic 'Network telescope'

Author: Grafiati

Published: 28 June 2021

Last updated: 1 February 2022

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1

Chou, Dean-Yi, Ming-Tsung Sun, Javier Fernandez Fernandez, Li-Han Wang, Antonio Jimenez, Alexander Serebryanskiy, and Shuhrat Ehgamberdiev. "Taiwan Automated Telescope Network." Advances in Astronomy 2010 (2010): 1–4. http://dx.doi.org/10.1155/2010/125340.

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A global network of small automated telescopes, the Taiwan Automated Telescope (TAT) network, dedicated to photometric measurements of stellar pulsations, is under construction. Two telescopes have been installed in Teide Observatory, Tenerife, Spain and Maidanak Observatory, Uzbekistan. The third telescope will be installed at Mauna Loa Observatory, Hawaii, USA. Each system uses a 9-cm Maksutov-type telescope. The effective focal length is 225 cm, corresponding to anf-ratio of 25. The field of view is 0.62 degree square. The images are taken with a 16-bit1024×1024CCD camera. The telescope is equipped with UBVRI filters. Each telescope is fully automated. The telescope can be operated either interactively or fully automatically. In the interactive mode, it can be controlled through the Internet. In the fully automatic mode, the telescope operates with preset parameters without any human care, including taking dark frames and flat frames. The network can also be used for studies that require continuous observations for selected objects.

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López-Casado, C., C. J. Pérez del Pulgar, E. Fernández, V. F. Muñoz, and A. Castro-Tirado. "GLSCH: OBSERVATION SCHEDULER FOR THE GLORIA TELESCOPE NETWORK." Revista Mexicana de Astronomía y Astrofísica Serie de Conferencias 51 (April 13, 2019): 111–15. http://dx.doi.org/10.22201/ia.14052059p.2019.51.18.

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This paper proposes the design and development of a scheduler for the GLORIA telescope network. This network, which main objective is to make astronomy closer to citizens in general, is formed by 18 telescopes spread over four continents and both hemispheres. Part of the management of this network is made by the network scheduler. It receives the observation requests made by the GLORIA users and then sends it to the most suitable telescope. A key module of the network scheduler is the telescope decision algorithm that makes possible to choose the best telescope, and thus avoiding offering an observation to a telescope that cannot execute it. This paper shows two different telescope decision algorithms: the first one is only based on weather forecast, meanwhile the second one uses fuzzy logic and information from each network telescope. Both algorithms were deployed in the GLORIA network. The achieved results coupled with a comparative of their performance is shown. Moreover, the network scheduler architecture, based on a hybrid distributed-centralized schema, is detailed.

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Elliott, Ian. "Requirements of a network telescope." Symposium - International Astronomical Union 123 (1988): 541–44. http://dx.doi.org/10.1017/s0074180900158668.

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General purpose telescopes fail to provide a cost-effective means of obtaining photometric data for asteroseismology. A continuous observing run on a particular star is best suited to automatic operation with a dedicated photoelectric telescope. As optical requirements for on-axis photometry are less severe than those for imaging, low-cost light-weight mirrors permit a saving in the size and cost of mount and dome. A stiff mounting with a low moment of inertia permits rapid movement under computer control. Adoption of a permanently mounted photometer and the elimination of manual controls also leads to design and operating economies. Maintenance can be shared with other instruments and travel and subsistence requirements are minimised. Therefore remote operation of a network of automatic telescopes at good sites could provide high quality data at reasonable cost.

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Wang, Jing-Sheng. "Newly Installed Radio and Optical Telescopes in China." Publications of the Astronomical Society of Australia 9, no. 1 (1991): 60–61. http://dx.doi.org/10.1017/s1323358000024899.

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AbstractNew radio and optical telescopes installed in recent years in China are summarised. These include the 2.16-m optical telescope, the solar magnetic field telescope, the Miyun synthesis radio telescope, the 1.26-m infrared telescope (Beijing Astronomical Observatory), the 25-m radio telescope as the first station of China’s VLBI network, the 1.56-m astrometric telescope (Shanghai Observatory), and the 13.7-m millimetre wave radio telescope.

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Gomez, E. L. "Las Cumbres Observatory: Building a global telescope network from the ground up." Proceedings of the International Astronomical Union 10, H16 (August 2012): 646. http://dx.doi.org/10.1017/s1743921314012678.

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AbstractLas Cumbres Observatory Global Telescope Network (LCOGT) are building a global network of telescopes which will be available to both professional scientists and the science curious public. This telescope network will be global and so will the community, therefore all aspects of the endeavour must be online and self-sustaining - from the observing software to the analysis tools. During 2012 LCOGT have deployed the first 1-meter telescopes, and launched a citizen science project using LCOGT data, Agent Exoplanet, as well as many other online resources for anyone to use as they explore astronomy.

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Street, R. A., T. A. Lister, Y. Tsapras, A. Shporer, F. B. Bianco, B. J. Fulton, D. A. Howell, et al. "A Global Robotic Telescope Network for Time-Domain Science." Proceedings of the International Astronomical Union 7, S285 (September 2011): 408–10. http://dx.doi.org/10.1017/s174392131200124x.

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AbstractLas Cumbres Observatory Global Telescope Network (LCOGT) is currently building a new kind of general-purpose astronomical facility: a fully robotic network of telescopes of 2m, 1m and 0.4m apertures and homogeneous instrumentation. A pan-network approach to scheduling (rather than per individual telescope) offers redundancy in the event of poor weather or technical failure, as well as the ability to observe a target around the clock. Here we describe the network design and instrumentation under development, together with the main science programmes already being lead by LCOGT staff.

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Shporer, Avi, Tim Brown, Tim Lister, Rachel Street, Yiannis Tsapras, Federica Bianco, Benjamin Fulton, and Andy Howell. "The LCOGT Network." Proceedings of the International Astronomical Union 6, S276 (October 2010): 553–55. http://dx.doi.org/10.1017/s1743921311021193.

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AbstractMotivated by the increasing need for observational resources for the study of time varying astronomy, the Las Cumbres Observatory Global Telescope (LCOGT) is a private foundation, whose goal is to build a global network of robotic telescopes for scientific research and education. Once completed, the network will become a unique tool, capable of continuous monitoring from both the Northern and Southern Hemispheres. The network currently includes 2 × 2.0 m telescopes, already making an impact in the field of exoplanet research. In the next few years they will be joined by at least 12 × 1.0 m and 20 × 0.4 m telescopes. The increasing amount of LCOGT observational resources in the coming years will be of great service to the astronomical community in general, and the exoplanet community in particular.

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Majcher, Ariel, Arkadiusz Cwiek, Mikołaj Cwiok, Lech Mankiewicz, Marcin Zaremba, and Aleksander F. Zarnecki. "“PI OF THE SKY” OFF-LINE EXPERIMENT WITH GLORIA." Acta Polytechnica 54, no. 3 (June 27, 2014): 205–9. http://dx.doi.org/10.14311/ap.2014.54.0205.

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GLORIA is the first free and open-access network of robotic telescopes in the world. Based on the Web 2.0 environment, amateur and professional users can do research in astronomy by observing with robotic telescope, and/or analyzing data acquired with GLORIA, or from other free access databases. The GLORIA project develops free standards, protocols and tools for controlling Robotic Telescopes and related instrumentation, for scheduling observations in the telescope network, and for conducting so-called off-line experiments based on the analysis of astronomical data. This contribution summarizes the implementation and results from the first research level off-line demonstrator experiment implemented in GLORIA, which was based on data collected with the “Pi of the Sky” telescope in Chile.

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Duncan, A. R. "Observation Scheduling for a Network of Small-Aperture Telescopes." Publications of the Astronomical Society of Australia 24, no. 2 (2007): 53–60. http://dx.doi.org/10.1071/as07011.

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AbstractOver the past several years, a system for accepting, servicing and returning the results from a large number of imaging requests has been developed for use with automated optical telescopes. One of the primary goals of this project is to increase the accessibility of astronomy to school, college and university students. A key component of this system is a request scheduling engine, which produces schedules for each telescope for its current night. This engine is dynamic, adjusting schedules to accommodate new requests and rescheduling failed requests on a time scale of the order of ten minutes. If a telescope is unavailable for an extended period, imaging requests will be reallocated to other telescopes in the network. Various models of dynamic scheduling are considered, and the current implementation is explored with a number of numerical experiments.

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Hidas, M. G., E. Hawkins, Z. Walker, T. M. Brown, and W. E. Rosing. "Las Cumbres Observatory Global Telescope: A homogeneous telescope network." Astronomische Nachrichten 329, no. 3 (March 2008): 269–70. http://dx.doi.org/10.1002/asna.200710950.

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Lister, Tim A., S. Greenstreet, E. Gomez, E. Christensen, and S. Larson. "The LCOGT NEO Follow-up Network." Proceedings of the International Astronomical Union 10, S318 (August 2015): 321–23. http://dx.doi.org/10.1017/s1743921315006778.

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AbstractLas Cumbres Observatory Global Telescope Network (LCOGT) has deployed a homogeneous telescope network of nine 1-meter telescopes to four locations in the northern and southern hemispheres, with a planned network size of twelve 1-meter telescopes at 6 locations. This network is very versatile and is designed to respond rapidly to target of opportunity events and also to perform long term monitoring of slowly changing astronomical phenomena. The global coverage of the network and the apertures of telescope available make LCOGT ideal for follow-up and characterization of Solar System objects (e.g. asteroids, Kuiper Belt Objects, comets, Near-Earth Objects (NEOs)) and additionally for the discovery of new objects.We are using the LCOGT network to confirm newly detected NEO candidates produced by the major sky surveys such as Catalina Sky Survey (CSS) and PanSTARRS (PS1&2) and several hundred targets are now being followed per year. An increasing amount of time is being spent to obtain follow-up astrometry and photometry for radar-targeted objects and those on the Near-Earth Object Human Space Flight Accessible Targets Study (NHATS) or Asteroid Retrieval Mission (ARM) lists in order to improve the orbits, determine the light curves and rotation periods and improve the characterization. This will be extended to obtain more light curves of other NEOs which could be targets. Recent results have included the first period determinations for several of the Goldstone-targeted NEOs. We are in the process of building a NEO follow-up portal which will allow professionals, amateurs and Citizen Scientists to plan, schedule and analyze NEO imaging and spectroscopy observations and data using the LCOGT Network and to act as a co-ordination hub for the NEO follow-up efforts.

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12

Nordling, Linda. "Recycled dishes form telescope network." Nature 488, no. 7413 (August 2012): 571. http://dx.doi.org/10.1038/488571a.

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Coughlin, Michael W., Sarah Antier, David Corre, Khalid Alqassimi, Shreya Anand, Nelson Christensen, David A. Coulter, et al. "Optimizing multitelescope observations of gravitational-wave counterparts." Monthly Notices of the Royal Astronomical Society 489, no. 4 (September 7, 2019): 5775–83. http://dx.doi.org/10.1093/mnras/stz2485.

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ABSTRACT The ever-increasing sensitivity of the network of gravitational-wave detectors has resulted in the accelerated rate of detections from compact binary coalescence systems in the third observing run of Advanced LIGO and Advanced Virgo. Not only has the event rate increased, but also the distances to which phenomena can be detected, leading to a rise in the required sky volume coverage to search for counterparts. Additionally, the improvement of the detectors has resulted in the discovery of more compact binary mergers involving neutron stars, revitalizing dedicated follow-up campaigns. While significant effort has been made by the community to optimize single telescope observations, using both synoptic and galaxy-targeting methods, less effort has been paid to coordinated observations in a network. This is becoming crucial, as the advent of gravitational-wave astronomy has garnered interest around the globe, resulting in abundant networks of telescopes available to search for counterparts. In this paper, we extend some of the techniques developed for single telescopes to a telescope network. We describe simple modifications to these algorithms and demonstrate them on existing network examples. These algorithms are implemented in the open-source software gwemopt, used by some follow-up teams, for ease of use by the broader community.

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Chun, Francis K., Roger D. Tippets, David M. Strong, Devin J. Della-Rose, Daniel E. Polsgrove, Kimberlee C. Gresham, Joshua A. Reid, et al. "A New Global Array of Optical Telescopes: The Falcon Telescope Network." Publications of the Astronomical Society of the Pacific 130, no. 991 (July 1, 2018): 095003. http://dx.doi.org/10.1088/1538-3873/aad03f.

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Guinan, Edward F., Scott Engle, and Edward J. Devinney. "Advances in Telescope and Detector Technologies – Impacts on the Study and Understanding of Binary Star and Exoplanet Systems." Proceedings of the International Astronomical Union 7, S282 (July 2011): 11–20. http://dx.doi.org/10.1017/s1743921311026792.

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AbstractCurrent and planned telescope systems (both on the ground and in space) as well as new technologies will be discussed with emphasis on their impact on the studies of binary star and exoplanet systems. Although no telescopes or space missions are primarily designed to study binary stars (what a pity!), several are available (or will be shortly) to study exoplanet systems. Nonetheless those telescopes and instruments can also be powerful tools for studying binary and variable stars. For example, early microlensing missions (mid-1990s) such as EROS, MACHO and OGLE were initially designed for probing dark matter in the halos of galaxies but, serendipitously, these programs turned out to be a bonanza for the studies of eclipsing binaries and variable stars in the Magellanic Clouds and in the Galactic Bulge. A more recent example of this kind of serendipity is the Kepler Mission. Although Kepler was designed to discover exoplanet transits (and so far has been very successful, returning many planetary candidates), Kepler is turning out to be a “stealth” stellar astrophysics mission returning fundamentally important and new information on eclipsing binaries, variable stars and, in particular, providing a treasure trove of data of all types of pulsating stars suitable for detailed Asteroseismology studies. With this in mind, current and planned telescopes and networks, new instruments and techniques (including interferometers) are discussed that can play important roles in our understanding of both binary star and exoplanet systems. Recent advances in detectors (e.g. laser frequency comb spectrographs), telescope networks (both small and large – e.g. Super-WASP, HAT-net, RoboNet, Las Combres Observatory Global Telescope (LCOGT) Network), wide field (panoramic) telescope systems (e.g. Large Synoptic Survey Telescope (LSST) and Pan-Starrs), huge telescopes (e.g. the Thirty Meter Telescope (TMT), the Overwhelming Large Telescope (OWL) and the Extremely Large Telescope (ELT)), and space missions, such as the James Webb Space Telescope (JWST), the possible NASA Explorer Transiting Exoplanet Survey Satellite (TESS – recently approved for further study) and Gaia (due for launch during 2013) will all be discussed. Also highlighted are advances in interferometers (both on the ground and from space) and imaging now possible at sub-millimeter wavelengths from the Extremely Long Array (ELVA) and Atacama Large Millimeter Array (ALMA). High precision Doppler spectroscopy, for example with HARPS, HIRES and more recently the Carnegie Planet Finder Spectrograph, are currently returning RVs typically better than ~2-m/s for some brighter exoplanet systems. But soon it should be possible to measure Doppler shifts as small as ~10-cm/s – sufficiently sensitive for detecting Earth-size planets. Also briefly discussed is the impact these instruments will have on the study of eclipsing binaries, along with future possibilities of utilizing methods from the emerging field of Astroinformatics, including: the Virtual Observatory (VO) and the possibilities of analyzing these huge datasets using Neural Network (NN) and Artificial Intelligence (AI) technologies.

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Polińska, M., K. Kamiński, W. Dimitrov, M. Fagas, W. Borczyk, T. Kwiatkowski, R. Baranowski, P. Bartczak, and A. Schwarzenberg–Czerny. "Global Astrophysical Telescope System – GATS." Proceedings of the International Astronomical Union 9, S301 (August 2013): 475–76. http://dx.doi.org/10.1017/s1743921313015123.

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AbstractThe Global Astronomical Telescope System is a project managed by the Astronomical Observatory Institute of Adam Mickiewicz University in Poznań (Poland) and it is primarily intended for stellar medium/high resolution spectroscopy. The system will be operating as a global network of robotic telescopes. The GATS consists of two telescopes: PST 1 in Poland (near Poznań) and PST 2 in the USA (Arizona). The GATS project is also intended to cooperate with the BRITE satellites and supplement their photometry with spectroscopic observations.

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Crawford, David L. "A Global Network of Small Telescopes as a Resource for Astronomical Research and Education." Highlights of Astronomy 11, no. 2 (1998): 923–26. http://dx.doi.org/10.1017/s1539299600019171.

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There is no question that relatively small telescopes are powerful tools for astronomy, just as they always have been. With the new detectors and full usage of computers, they have become even more powerful, enabling us to do with a one-meter aperture telescope today more than 4-meter or 5-meter telescopes could do only a few decades ago. And the small ones cost a lot less to build and operate than the large ones. As such, small telescopes are the main hope for observing time for the many astronomers worldwide who need them as part of their research (or educational) tools. They can make a major impact on many areas of research and will be of great value for scientific education as well. Astronomy is very interesting to students and to the general public, not just to astronomers. Furthermore, most areas of astronomical research are data poor and more telescopes are needed to effectively attack the problems. Only a very few of us have adequate telescope time for our research or educational needs.

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Lewis, Fraser, Rachel Street, Paul Roche, Vanessa Stroud, and David M. Russell. "Robotic Astronomy with the Faulkes Telescopes and Las Cumbres Observatory Global Telescope." Advances in Astronomy 2010 (2010): 1–4. http://dx.doi.org/10.1155/2010/873059.

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We present results from ongoing science projects conducted by members of the Faulkes Telescope (FT) team and Las Cumbres Observatory Global Telescope (LCOGT). Many of these projects incorporate observations carried out and analysed by FT users, comprising amateur astronomers and schools. We also discuss plans for the further development of the LCOGT network.

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Brown, T. M., N. Baliber, F. B. Bianco, M. Bowman, B. Burleson, P. Conway, M. Crellin, et al. "Las Cumbres Observatory Global Telescope Network." Publications of the Astronomical Society of the Pacific 125, no. 931 (September 2013): 1031–55. http://dx.doi.org/10.1086/673168.

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Abbott, Alison. "Report praises European radio telescope network." Nature 407, no. 6803 (September 2000): 437. http://dx.doi.org/10.1038/35035251.

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Chou, Dean-Yi, Ming-Tsung Sun, and Ming-Hsu Yang. "Earthshine and Asteroseismology Telescope (East) Network." Space Science Reviews 122, no. 1-4 (February 2006): 221–28. http://dx.doi.org/10.1007/s11214-006-8187-x.

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Isobe, Syuzo. "Possible Collaborative Network with Small Telescopes and a Standard CCD in Japan." International Astronomical Union Colloquium 148 (1995): 536–41. http://dx.doi.org/10.1017/s025292110002248x.

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AbstractThere are two obvious ways to make a quick survey work. A: A telescope with a wide field and a large size detector. B: Many telescopes with a rather narrow field and a small size detector. In Japan, there are now 47 telescopes with diameters of 50-100 cm dedicated to public use. If we develop a simple-to-handle detector system, non-professional observers at each public observatory would have the possibility of joining a collaborative survey network. We started a test observation which is expected to extend to a survey network.

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Crawford, D. L. "GNAT — A Global Network of Automatic Telescopes." International Astronomical Union Colloquium 136 (1993): 244–49. http://dx.doi.org/10.1017/s0252921100007624.

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AbstractAll of us “have-nots” need more telescope time, for ourselves and for our students. There are also many programs where a global linkage is needed to accomplish the objectives. In addition, the world needs more and better science education; astronomy can be a leader if it has adequate facilities to do so. A global network of automatic telescopes can help supply these needs, which are global, spanning all countries. A new non-profit organization (GNAT, Inc.) has been formed to be the catalyst to develop and implement such a concept. We hope that many astronomers and organizations will become “members” of GNAT.

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Sohib, Ahmad, Niko Danusaid, Astri Sawitri, Bebeh Wahid Nuryadin, and Rena Denya Agustina. "Low cost digitalization of observation telescope by utilizing smartphone." MATEC Web of Conferences 197 (2018): 02002. http://dx.doi.org/10.1051/matecconf/201819702002.

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Digitalization of telescopes used as learning media observation of the object is quite effective. However, the cost of operating this system becomes one of the obstacles. The approach to overcome the obstacle can be conducted by utilization of the present technology such as smartphone. Physical experiments have been conducted on the design of digitalization of the starter binoculars interfacing to Personal Computer (PC) using a smartphone. This experiment is aimed to design a more efficient digitalization of telescope observations. Smartphone stative is made in such a way that the camera in the right position on the telescope lens. Data retrieval is taken by a smartphone camera and ASI120MC camera as a comparison parameter. The data will be sent to the PC via an application installed both on smartphone and PC attributed by Bluetooth network. The camera is supported with a camera stative to keep it apart from binoculars. The observations obtained from this system is an interpretation between the camera on the telescope and PC. Such interpretations may produce images or videos observed by telescopes. This design can simplify the interfacing of telescope resulting good enough photo quality.

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Molotov, I., M. Zakhvatkin, L. Elenin, L. Canals Ros, F. Graziani, P. Teofilatto, T. Schildknecht, et al. "ISON NETWORK TRACKING OF SPACE DEBRIS: CURRENT STATUS AND ACHIEVEMENTS." Revista Mexicana de Astronomía y Astrofísica Serie de Conferencias 51 (April 13, 2019): 144–49. http://dx.doi.org/10.22201/ia.14052059p.2019.51.25.

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Interagency International Scientific Optical Network (ISON) represents one of largest systems specializing in observation of space objects. ISON provides permanent monitoring of the whole GEO region, regular surveying of Molniya type orbits, and tracking of objects at GEO, GTO, HEO and LEO. Currently ISON cooperates with 43 observation facilities of various affiliations with 100 telescopes in 17 countries. Six telescope subsets have been completed to the date, ISON encompasses five groups of telescopes and three scheduling centers. Obtained measurements are processed at the KIAM ballistic center to be used for scientific and applied goals, including collision risks analysis and space situation analysis. 20 millions measurements in 2.58 millions of tracklets for more 6740 objects have been collected by KIAM in 2016.

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van der Gucht, Jeffrey, Jordy Davelaar, Luc Hendriks, Oliver Porth, Hector Olivares, Yosuke Mizuno, Christian M. Fromm, and Heino Falcke. "Deep Horizon: A machine learning network that recovers accreting black hole parameters." Astronomy & Astrophysics 636 (April 2020): A94. http://dx.doi.org/10.1051/0004-6361/201937014.

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Context. The Event Horizon Telescope recently observed the first shadow of a black hole. Images like this can potentially be used to test or constrain theories of gravity and deepen the understanding in plasma physics at event horizon scales, which requires accurate parameter estimations. Aims. In this work, we present Deep Horizon, two convolutional deep neural networks that recover the physical parameters from images of black hole shadows. We investigate the effects of a limited telescope resolution and observations at higher frequencies. Methods. We trained two convolutional deep neural networks on a large image library of simulated mock data. The first network is a Bayesian deep neural regression network and is used to recover the viewing angle i, and position angle, mass accretion rate Ṁ, electron heating prescription Rhigh and the black hole mass MBH. The second network is a classification network that recovers the black hole spin a. Results. We find that with the current resolution of the Event Horizon Telescope, it is only possible to accurately recover a limited number of parameters of a static image, namely the mass and mass accretion rate. Since potential future space-based observing missions will operate at frequencies above 230 GHz, we also investigated the applicability of our network at a frequency of 690 GHz. The expected resolution of space-based missions is higher than the current resolution of the Event Horizon Telescope, and we show that Deep Horizon can accurately recover the parameters of simulated observations with a comparable resolution to such missions.

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Fraser, S. N. "Scheduling for Robonet-1 homogenous telescope network." Astronomische Nachrichten 327, no. 8 (September 2006): 779–82. http://dx.doi.org/10.1002/asna.200610632.

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Yost, S. A., F. Aharonian, C. W. Akerlof, M. C. B. Ashley, S. Barthelmy, N. Gehrels, E. Göğüş, et al. "Status of the ROTSE-III telescope network." Astronomische Nachrichten 327, no. 8 (September 2006): 803–5. http://dx.doi.org/10.1002/asna.200610683.

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Gorosabel, Javier, Petr Kubánek, Martin Jelínek, Alberto J. Castro-Tirado, Antonio de Ugarte Postigo, Sebastián Castillo-Carrión, Sergey Guziy, et al. "Recent GRBs Observed with the 1.23 m CAHA Telescope and the Status of Its Upgrade." Advances in Astronomy 2010 (2010): 1–8. http://dx.doi.org/10.1155/2010/701534.

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We report on optical observations of Gamma-Ray Bursts (GRBs) followed up by our collaboration with the 1.23 m telescope located at the Calar Alto observatory. The 1.23 m telescope is an old facility, currently undergoing upgrades to enable fully autonomous response to GRB alerts. We discuss the current status of the control system upgrade of the 1.23 m telescope. The upgrade is being done by our group based on the Remote Telescope System, 2nd Version (RTS2), which controls the available instruments and interacts with the EPICS database of Calar Alto. (Our group is called ARAE (Robotic Astronomy & High-Energy Astrophysics) and is based on members of IAA (Instituto de Astrofísica de Andalucía). Currently the ARAE group is responsible to develop the BOOTES network of robotic telescopes (Jelínek et al. 2009).) Currently the telescope can run fully autonomously or under observer supervision using RTS2. The fast reaction response mode for GRB reaction (typically with response times below 3 minutes from the GRB onset) still needs some development and testing. The telescope is usually operated in legacy interactive mode, with periods of supervised autonomous runs under RTS2. We show the preliminary results of several GRBs followed up with observer intervention during the testing phase of the 1.23 m control software upgrade.

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Luminet, Jean-Pierre. "Seeing Black Holes: From the Computer to the Telescope." Universe 4, no. 8 (August 9, 2018): 86. http://dx.doi.org/10.3390/universe4080086.

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Astronomical observations are about to deliver the very first telescopic image of the massive black hole lurking at the Galactic Center. The mass of data collected in one night by the Event Horizon Telescope network, exceeding everything that has ever been done in any scientific field, should provide a recomposed image in 2018. All this, forty years after the first numerical simulations performed by the present author.

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Howell, Andrew. "Determining the progenitors of supernovae with early robotic observations." Proceedings of the International Astronomical Union 11, A29B (August 2015): 222. http://dx.doi.org/10.1017/s1743921316005007.

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AbstractWe present results from the LCOGT Supernova Key Project, a three year program to obtain lightcurves and spectra of 600 supernovae. The Las Cumbres Observatory Global Telescope Network is a network of eleven robotic 1m and 2m telescopes located at 5 sites around the world. With this facility long term monitoring of transient phenomena is possible, as are nearly instantaneous observations. We report on both core-collapse and thermonuclear supernovae observed within days of explosion, allowing insight into their progenitor stars.

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Stasielak, Jarosław, Paweł Malecki, Dmitry Naumov, Vladimir Allakhverdian, Alexandra Karnakova, Konrad Kopański, and Wojciech Noga. "High-Energy Neutrino Astronomy—Baikal-GVD Neutrino Telescope in Lake Baikal." Symmetry 13, no. 3 (February 26, 2021): 377. http://dx.doi.org/10.3390/sym13030377.

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High-energy neutrino astronomy is a fascinating new field of research, rapidly developing over recent years. It opens a new observation window on the most violent processes in the universe, fitting very well to the concept of multi-messenger astronomy. This may be exemplified by the recent discovery of the high-energy neutrino emissions from the γ-ray loud blazar TXS 0506+056. Constraining astrophysical neutrino fluxes can also help to understand the long-standing mystery of the origin of the ultra-high energy cosmic rays. Astronomical studies of high-energy neutrinos are carried out by large-scale next-generation neutrino telescopes located in different regions of the world, forming a global network of complementary detectors. The Baikal-GVD, being currently the largest neutrino telescope in the Northern Hemisphere and still growing up, is an important constituent of this network. This paper briefly reviews working principles, analysis methods, and some selected results of the Baikal-GVD neutrino telescope.

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BACKES, M., J. K. BECKER, F. CLEVERMANN, D. NEISE, W. RHODE, S. ROLLKE, M. POHL, et al. "LONG-TERM MONITORING OF BRIGHT BLAZARS WITH A DEDICATED CHERENKOV TELESCOPE." International Journal of Modern Physics D 18, no. 10 (October 2009): 1645–49. http://dx.doi.org/10.1142/s0218271809015357.

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Flaring activity of Active Galactic Nuclei (AGN) in VHE γ-ray astronomy is observed on timescales from minutes to years and can be explained either by the interaction of relativistic jets with the surrounding material or by imprints of the central engine, like temporal modulation caused by binary systems of supermassive black holes. The key to answer those questions lies in combining 24/7 monitoring with short high sensitivity exposures as provided by the third generation γ-ray astronomy instruments like MAGIC, VERITAS and H.E.S.S. The long-term observations can be provided by a global network of small robotic Cherenkov telescopes.1 As a first step, we are currently setting up a dedicated Cherenkov telescope, which will carry out joint observations with the Whipple 10 m telescope for AGN monitoring. The new telescope will be designed for low costs but high performance by upgrading one of the former HEGRA telescopes, still located at the MAGIC site on the Canary Island of La Palma (Spain). The main novelties will be its robotic operation and a novel camera type, resulting in a greatly improved sensitivity and a lower energy threshold.

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Kawaler, Steven D. "The Whole Earth Telescope: An International Adventure in Asteroseismology." International Astronomical Union Colloquium 183 (2001): 3–12. http://dx.doi.org/10.1017/s0252921100078532.

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AbstractToday, we are beginning to probe the interior of stars through the new science of stellar seismology. Certain stars, ranging from our own Sun to white dwarfs, undergo natural vibrations that can be detected with sensitive time-series photometry and/or spectroscopy. Since the signal we seek is an unbroken time-series to allow determination of the vibration frequencies, data from a single-site is usually incapable of uniquely identifying the pulsation modes, no matter how large the telescope being used. In many cases, the observational goals can be achieved using small-ish telescopes in well-coordinated global networks. Here, I briefly describe the work of one such international network of observatories and scientists known as the Whole Earth Telescope (WET). With the WET, we have sounded out the interiors of a large number of nonradially pulsating stars. Over the past 14 years, WET has observed dozens of stars in 20 separate observing campaigns. Our team has wide span of interests, and has observed several other classes of objects such as delta Scuti stars, CV stars, pulsating sdB stars, and rapidly oscillating Ap stars.

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Jaroenjittichai, Phrudth. "Status of the Thai 40-m Radio Telescope." Proceedings of the International Astronomical Union 13, S337 (September 2017): 346–47. http://dx.doi.org/10.1017/s1743921317008602.

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AbstractSince the first light of the 2.4-m Thai National Telescope in 2013, Thailand foresees another great leap forward in astronomy. A project known as “Radio Astronomy Network and Geodesy for Development” (RANGD) by National Astronomical Research Institute of Thailand (NARIT) has been approved for year 2017-2021. A 40-m radio telescope has been planned to operate up to 115-GHz observation with prime-focus capability for low frequency and phased array feed receivers. The telescope’s first light is expected in late 2019 with a cryogenics K-band and L-band receivers. RFI environment at the site has been investigated and shown to be at reasonable level. A 13-m VGOS telescope is also included for geodetic applications. Early single-dish science will focus on time domain observations, such as pulsars and transients, outbursts and variability of maser and AGN sources.

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Янчуковский, Валерий, Valery Yanchukovsky, Владислав Григорьев, Vladislav Grigoryev, Гермоген Крымский, Germogen Krymsky, Василий Кузьменко, Vasiliy Kuzmenko, Антон Молчанов, and Anton Molchanov. "Receiving vectors of muon telescope of cosmic ray station “Novosibirsk”." Solnechno-Zemnaya Fizika 2, no. 1 (March 17, 2016): 76–87. http://dx.doi.org/10.12737/16762.

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The method of receiving vectors allows us to determine cosmic ray anisotropy at each moment. Also, the method makes it possible to study fast anisotropy fluctuations related to the interplanetary medium dynamics. Receiving vectors have been calculated earlier for neutron monitors and muon telescopes. However, the most of muon telescopes of the network of cosmic ray stations for which calculations were made does not operate now. In recent years, new improved detectors appeared. Unfortunately, the use of them is limited because of absence of receiving coefficients. These detectors include the matrix telescope in Novosibirsk. Therefore, components of receiving vector for muon telescopes of observation cosmic ray station “Novosibirsk” have been defined. Besides, design features of the facility, its orientation, and directional diagram depending on zenith and azimuth angles were taken into account. Also, for the system of telescopes, we allowed for coupling coefficients found experimentally using the test detector.

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37

Янчуковский, Валерий, Valery Yanchukovsky, Владислав Григорьев, Vladislav Grigoryev, Гермоген Крымский, Germogen Krymsky, Василий Кузьменко, Vasiliy Kuzmenko, Антон Молчанов, and Anton Molchanov. "Receiving vectors of muon telescope of cosmic ray station Novosibirsk." Solar-Terrestrial Physics 2, no. 1 (June 1, 2016): 103–19. http://dx.doi.org/10.12737/19883.

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The method of receiving vectors allows us to determine cosmic ray anisotropy at every moment of time. Also, the method makes it possible to study fast anisotropy fluctuations related to the interplanetary medium dynamics. Receiving vectors have been calculated earlier for neutron monitors and muon telescopes. However, most muon telescopes of the network of cosmic ray stations for which calculations were made does not operate now. In recent years, new, improved detectors have been developed. Unfortunately, the use of them is limited because of the absence of receiving coefficients. These detectors include a matrix telescope in Novosibirsk. Therefore, receiving vector components for muon telescopes of observation cosmic ray station Novosibirsk have been defined. Besides, design features of the facility, its orientation, and directional diagram depending on zenith and azimuth angles were taken into account. Also, for the system of telescopes, we allowed for coupling coefficients found experimentally by the test detector.

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38

Moon, Hong-Kyu, Myung-Jin Kim, Hong-Suh Yim, Young-Jun Choi, Young-Ho Bae, Dong-Goo Roh, Jintae Park, and Bora Moon. "DEEP-South: Network Construction, Test Runs and Early Results." Proceedings of the International Astronomical Union 10, S318 (August 2015): 306–10. http://dx.doi.org/10.1017/s1743921315008455.

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AbstractKorea Microlensing Telescope Network (KMTNet) which consists of three identical 1.6 m wide-field telescopes with 18k × 18k CCDs, is the first optical survey system of its kind. The combination of fast optics and the mosaic CCD delivers seeing limited images over a 4 square degrees field of view. The main science goal of KMTNet is the discovery and characterization of exoplanets, yet it also offers various other science applications including DEep Ecliptic Patrol of SOUTHern sky (DEEP-South). The aim of DEEP-South is to discover and characterize asteroids and comets, including Near Earth Objects (NEOs). We started test runs last February after commissioning, and will return to normal operations in October 2015. A summary of early results from the test runs will be presented.

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Gresham, Kimberlee C., Christopher Palma, Daniel E. Polsgrove, Francis K. Chun, Devin J. Della-Rose, and Roger D. Tippets. "Education and outreach using the falcon telescope network." Acta Astronautica 129 (December 2016): 130–34. http://dx.doi.org/10.1016/j.actaastro.2016.09.006.

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Hessman, F. V. "Prospects for a global Heterogeneous Telescope Network (HTN)." Astronomische Nachrichten 327, no. 8 (September 2006): 763–66. http://dx.doi.org/10.1002/asna.200610628.

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41

Grundahl, Frank, J. Christensen-Dalsgaard, H. Kjeldsen, S. Frandsen, T. Arentoft, P. Kjaergaard, and U. G. Jørgensen. "SONG – Stellar Observations Network Group." Proceedings of the International Astronomical Union 4, S252 (April 2008): 465–66. http://dx.doi.org/10.1017/s174392130802351x.

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AbstractSeveral areas of stellar observations depend critically on nearly continuous observations of individual objects over very extended periods. Important examples are investigations of stellar oscillations to carry out asteroseismology, and the search for extra-solar planets. To meet this requirement we are establishing the SONG network, consisting of 8 sites with a 1-meter-class telescope with a suitable geographical distribution. These will be optimized for asteroseismology based on Doppler-velocity observations and the characterization of extra-solar planets with photometry, using gravitational microlensing. Funding has been obtained towards the construction of the prototype SONG telescope which will be set up on Tenerife, with first light expected in 2011. The full network will be established in parallel with the tests of the prototype and is planned to be operational in 2014.

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Grundahl, Frank, Jørgen Christensen-Dalsgaard, Pere L. Pallé, Mads F. Andersen, Søren Frandsen, Kennet Harpsøe, Uffe Gråe Jørgensen, et al. "Stellar Observations Network Group: The prototype is nearly ready." Proceedings of the International Astronomical Union 9, S301 (August 2013): 69–75. http://dx.doi.org/10.1017/s1743921313014117.

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AbstractThe prototype telescope and instruments for the Stellar Observations Network Group (SONG) are nearing completion at the Observatorio del Teide on Tenerife. In this contribution we describe the current status (autumn 2013) of the telescope and its instrumentation. Preliminary performance characteristics are presented for the high-resolution spectrograph based on daytime observations of the Sun and a 4 hour test series obtained for the sub-giant β Aquilae.

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43

Chou, Dean-Yi. "Taiwan Oscillation Network and Small-Telescope Research at Tsing Hua University." International Astronomical Union Colloquium 183 (2001): 39–43. http://dx.doi.org/10.1017/s0252921100078581.

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AbstractTwo projects, the Taiwan Oscillation Network (TON) project and the earthshine project, at Tsing Hua University will be discussed. The TON is a ground-based network to measure solar intensity oscillations to study the solar interior. Four telescopes have been installed in Tenerife (Spain), Big Bear (USA), Huairou (PRC), and Tashkent (Uzbekistan). The recent scientific results from the TON data will be briefly discussed. The earthshine project is to measure the brightness of the dark portion of the lunar disk to obtain the Earth’s global albedo. The dark portion of the Moon is lit by the sunlight reflected from the Earth. The global albedo is linked to the global temperature of the Earth. The long-term measurement of earthshine will provide information on the long-term variation of the global temperature. An automated earthshine telescope is being developed at Tsing Hua University. It will be installed at Lulin Mountain in central Taiwan. The ultimate goal is to build a ground-based global network to measure the long-term variation of earthshine to learn about the long-term variation of the global temperature.

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Hillebrandt, Wolfgang, and Brian P. Schmidt. "DIVISION VIII / WG: SUPERNOVAE." Proceedings of the International Astronomical Union 3, T26B (December 2007): 181–82. http://dx.doi.org/10.1017/s1743921308024022.

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As far as coordination and planning of observational activities are concerned, the main need for WG-SN activities seem to lie in the field of suitable follow-ups to the many on-going and planned search programs (in particular for SNe Ia's; LOTOSS, NGSS, SNfactory, SNLS, ESSENCE, GOODS, PanStarrs, . . .). With the new robotic 2m-class telescopes (e.g., the Las Cumbres Observatory Global Telescope Network and other robotic telescopes) photometric follow-ups do not seem a major problem, but for most of the searches spectroscopic follow-up requires 4m-class telescopes at least which will become rare in the future. Possible ways out were discussed.

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Scaife, A. M. M. "Big telescope, big data: towards exascale with the Square Kilometre Array." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 378, no. 2166 (January 20, 2020): 20190060. http://dx.doi.org/10.1098/rsta.2019.0060.

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Unlike optical telescopes, radio interferometers do not image the sky directly but require specialized image formation algorithms. For the Square Kilometre Array (SKA), the computational requirements of this image formation are extremely demanding due to the huge data rates produced by the telescope. This processing will be performed by the SKA Science Data Processor facilities and a network of SKA Regional Centres, which must not only deal with SKA-scale data volumes but also with stringent science-driven image fidelity requirements. This article is part of a discussion meeting issue ‘Numerical algorithms for high-performance computational science’.

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ZHU, WEI, and ANDREW GOULD. "AUGMENTING WFIRST MICROLENSING WITH A GROUND-BASED TELESCOPE NETWORK." Journal of The Korean Astronomical Society 49, no. 3 (June 30, 2016): 93–107. http://dx.doi.org/10.5303/jkas.2016.49.3.93.

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Gomez, Edward L., and Haley L. Gomez. "The World's first global telescope network at your fingertips." Proceedings of the International Astronomical Union 5, S260 (January 2009): 607–15. http://dx.doi.org/10.1017/s1743921311002924.

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AbstractWe discuss the creation of the World's largest homogeneous telescope network. We summarize both the scientific and education programmes, and outline why this organization provides unique opportunities for anyone interested in astronomy, whether they are professionals or amateurs, experienced or novice.

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Dhar, V. K., A. K. Tickoo, M. K. Koul, R. Koul, B. P. Dubey, R. C. Rannot, K. K. Yadav, et al. "Artificial Neural Network based segregation methodology for TACTIC telescope." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 708 (April 2013): 56–71. http://dx.doi.org/10.1016/j.nima.2012.12.118.

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López-Casado, Carmen, Carlos Pérez-del-Pulgar, Víctor F. Muñoz, and Alberto J. Castro-Tirado. "Observation scheduling and simulation in a global telescope network." Future Generation Computer Systems 95 (June 2019): 116–25. http://dx.doi.org/10.1016/j.future.2018.12.066.

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Kubánek, P. "RTS2: Lessons learned from a widely distributed telescope network." Astronomische Nachrichten 329, no. 3 (March 2008): 271–74. http://dx.doi.org/10.1002/asna.200710936.

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