Journal articles: 'And Astronomical Observations'

1

Street, R. "Astronomical observations." Physics World 3, no. 5 (May 1990): 15. http://dx.doi.org/10.1088/2058-7058/3/5/11.

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Nikolov, A. S. "An Application of Personal Computers in Astronomy Education." International Astronomical Union Colloquium 105 (1990): 177–78. http://dx.doi.org/10.1017/s0252921100086668.

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Observations play an important role in the process of teaching astronomical knowledge. Practical observations of astronomical phenomena lead to analysis and explanation based on natural laws and so form the basis of cognitive processes in the education. Evidently the observations are an integral part of acquiring astronomical knowledge. Giving up observations, no matter what the reasons, is equivalent to losing quality in the educational process. It decreases the possible influence over the personal development of pupils and students. At the same time, observation and observational results are important for success in education.Carefully planned observational time has a substantial influence on cognitive and educational processes. It leads to considerably more active participation in astronomy lectures.

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Walker, Gordon, Pierre Léna, Daniel J. Schroeder, and Joseph S. Miller. "Astronomical Observations: An Optical Perspective and Observational Astrophysics and Astronomical Optics." Physics Today 42, no. 3 (March 1989): 97. http://dx.doi.org/10.1063/1.2810932.

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Zhang, X. Z., and J. H. Wu. "IPS Observations at Beijing Astronomical Observatory." Highlights of Astronomy 12 (2002): 398. http://dx.doi.org/10.1017/s1539299600013903.

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The radio wave from distant radio sources will be scattered by the irregular structures of the solar wind plasma when propagating through the interplanetary space, resulting into a randomly fluctuating pattern of the radio wave in observation. This pattern is called interplanetary scintillation (IPS). Observation on IPS can give information of the solar wind speed and irregular structures in solar wind plasma. The IPS observations began at Miyun Station, Beijing Astronomical Observatory from the late half of 1999. The properties of the telescope and description of the data analysis can be found in the papers of Wang (1987) and Wu, Zhang and Zheng (2000) respectively.Table 1 summarizes some observational results using IPS source 3C48 in April and May 2000. The Fresnel knees and the first minima in the IPS spectra were used to estimate solar wind speeds. Comparisons of our results with the unpublished data of Hiraiso Solar Terrestrial Research Center obtained from their web site, have been done and good agreement between the two systems was found. Since the collecting area of Miyun telescope is limited, the system noise is relatively high and dominates the high-frequency parts of the spectra. The Miyun IPS observation and data reduction procedures are still under developing and will soon be completed.

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Edberg, Stephen J. "Working with Amateur Astronomers." International Astronomical Union Colloquium 98 (1988): 95–99. http://dx.doi.org/10.1017/s0252921100092307.

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Amateur astronomers have a vast store of talent and expertise in making astronomical observations. When carefully channelled, their enthusiasm coupled with these characteristics can lead to the acquisition of large volumes of high-quality astronomical data. The Amateur Observation Network of the International Halley Watch (IHW) was organized to encourage comet observations by amateurs, standardize techniques whenever possible, and then collect and archive these observations for use by the astronomical community in the near and distant future as part of the whole IHW archive. The lessons learned from this experience will be useful to organizers who plan observation campaigns involving amateur astronomers in the future.

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Klioner, S. A. "Relativistic astrometry and astrometric relativity." Proceedings of the International Astronomical Union 3, S248 (October 2007): 356–62. http://dx.doi.org/10.1017/s174392130801956x.

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AbstractThe interplay between modern astrometry and gravitational physics is very important for the progress in both these fields. Below some threshold of accuracy, Newtonian physics fails to describe observational data and the Einstein's relativity theory must be used to model the data adequately. Many high-accuracy astronomical techniques have already passed this threshold. Moreover, modern astronomical observations cannot be adequately modeled if relativistic effects are considered as small corrections to Newtonian models. The whole way of thinking must be made compatible with relativity: this starts with the concepts of time, space and reference systems.An overview of the standard general-relativistic framework for modeling of high-accuracy astronomical observations is given. Using this framework one can construct a standard set of building blocks for relativistic models. A suitable combination of these building blocks can be used to formulate a model for any given type of astronomical observations. As an example the problem of four dimensional solar system ephemerides is exposed in more detail. The limits of the present relativistic formulation are also briefly summarized.On the other hand, high-accuracy astronomical observations play important role for gravitational physics itself, providing the latter with crucial observational tests. Perspectives for these astronomical tests for the next 15 years are summarized.

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Šprajc, Ivan. "Astronomical aspects of Group E-type complexes and implications for understanding ancient Maya architecture and urban planning." PLOS ONE 16, no. 4 (April 27, 2021): e0250785. http://dx.doi.org/10.1371/journal.pone.0250785.

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In the 1920s, during the first archaeological excavations at Uaxactún, Petén, Guatemala, an architectural complex named Group E was interpreted as an ancient Maya astronomical observatory, intended specifically for sighting the equinoctial and solstitial sunrises. In the following decades, a large number of architectural compounds with the same configuration have been found, most of them in the central lowlands of the Yucatan peninsula. The multiple hypotheses that have been proposed about the astronomical function of these complexes, commonly designated as E Groups, range from those attributing them a paramount role in astronomical observations to those that consider them merely allegorical or commemorative allusions to celestial cycles, without any observational use. This study, based on quantitative analyses of a reasonably large sample of alignment data, as well as on contextual evidence, shows that many of the previous hypotheses cannot be sustained. I argue that E Groups, although built primarily for ritual purposes, were astronomically functional, but also that they had no specific or particularly prominent role in astronomical observations. Their orientations belong to widespread alignment groups, mostly materialized in buildings of other types and explicable in terms of some fundamental concerns of the agriculturally-based Maya societies. I present the evidence demonstrating that the astronomical orientations initially embedded in E Groups, which represent the earliest standardized form of Maya monumental architecture and whose occurrence in practically all early cities in the central Yucatan peninsula attests to their socio-political significance, were later transferred to buildings and compounds of other types. Therefore, it is precisely the importance of the astronomically and cosmologically significant directions, first incorporated in E Groups, that allows us to understand some prominent aspects of ancient Maya architecture and urbanism.

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Millis, Robert L. "Astronomical observations—an optical perspective." Icarus 74, no. 2 (May 1988): 374–75. http://dx.doi.org/10.1016/0019-1035(88)90052-8.

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Garcia-Piquer, A., J. C. Morales, I. Ribas, J. Colomé, J. Guàrdia, M. Perger, J. A. Caballero, et al. "Efficient scheduling of astronomical observations." Astronomy & Astrophysics 604 (August 2017): A87. http://dx.doi.org/10.1051/0004-6361/201628577.

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Patris, J., and A. Sarkissian. "Astronomical observations with OHP telescopes." Journal de Physique IV (Proceedings) 139, no. 1 (December 2006): 373–90. http://dx.doi.org/10.1051/jp4:2006139024.

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Voelkel, James R. "Publish or Perish: Legal Contingencies and the Publication of Kepler's Astronomia nova." Science in Context 12, no. 1 (1999): 33–59. http://dx.doi.org/10.1017/s0269889700003306.

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The ArgumentThe publication of Johannes Kepler's brilliant and revolutionary Astronomia nova (1609) has hitherto been viewed as somehow inevitable. This paper argues that, on the contrary, the book's very existence and a measure of its unusual form and content are in fact highly contingent, and derive from a legal dispute between Kepler and Tycho's heirs over the right to capitalize on his astronomical legacy. On Tycho's death, Kepler rather accidentally found himself in charge of Tycho's posthumous astronomical publications, especially the highly prestigious Rudol phine Tables. Tycho's legal heirs, not having been paid by the emperor for Tycho's astronomical assets and feigning Kepler's unworthiness as his successor, wrested this mandate back. Ordered in turn to justify his employment, Kepler contrived the Astronomia nova as an interim announcement of the fruits of his astronomical research. In an effort to block Kepler's continuing exploitation of Tycho's observations, the heirs obtained the legal right to censor his publications, which severely threatened his philosophical freedom. The threat of editorial interference was responsible in part for Astronomia nova's unusual narrative form.

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Liu, Haocheng, Xinhua Huang, and Qingkai Meng. "Geographical-environmental factors extraction and analysis for optical astronomical site selection based on multi-source remote sensing in Lenghu, Qinghai Province." ITM Web of Conferences 47 (2022): 03034. http://dx.doi.org/10.1051/itmconf/20224703034.

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At present, there are scarce sites that can require high-quality astronomical observations over the world, therefore, analysis of geographical-environmental factors and extraction of the potential places for astronomical observations is of significance. Remote sensing has the specific advantage for rapid and widespread monitoring and geo-spatial analysis. In this paper, Precipitable Water Vapor (PWV), clear nights, altitude and surface coverage, these four parameters associated with optical astronomical observation was selected, Analytic Hierarchy Process (AHP) evaluating model was adopted to determine the weighting parameters and calculated geo-environmental suitability. The results show that: (1) The lenghu region is characterized by seasonal variation with high PWV in summer and low PWV in the winter, representing non-summer periods are the best observation time. (2) The Lenghu region has relatively high clear nights with more than half of times through one year is suitable for observation. (3) Based on Geoenvironmental suitability mapping,Saishiteng Mountain is selected as a priority site for optical astronomical sites.

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Gienko, Elena G., Sergey A. Parshikov, and Elizaveta A. Bubir. "SANCTUARY "TEMPLE OF TIME" IN NORTHERN KHAKASSIA: MODELING LIGHT-AND-SHADOW PICTURE." Vestnik SSUGT (Siberian State University of Geosystems and Technologies) 25, no. 4 (2020): 5–18. http://dx.doi.org/10.33764/2411-1759-2020-25-4-5-18.

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The results of the study of the archaeological monument of Tagar culture (VIII-III centuries BC) "Temple of time", located in Northern Khakassia, are described. The main purpose of the study was to obtain natural scientific evidence of the monument calendar significance, as well as that its construction was performed in accordance with the light-and-dark picture during the sunrise and sunset at the equinoxes and winter solstice. To modeling the annual illumination of the monument by the Sun, azimuth orientation, geodesic measurements, and astronomical calculations were performed. In addition, in order to clarify the details, the simulation of a solar beam with a total station laser beam was applied. The modeling results were confirmed by direct observations during the autumnal equinox and winter solstice, when photographs were taken with recording of the shooting moments for subsequent astronomical calculations. As a result, the importance of astronomical research methods and direct observations on astronomically significant days of the year in the study of such archaeological objects is justified. Using astronomical calculations, it is proved that the light-and-shadow picture observed on the monument in modern times is almost identical to the light-and-shadow picture in the Tagar epoch. Suggestions have been made for using laser scanning to model a light-and-shadow picture. The monument "Temple of Time" is a unique object, it is a complex spatial structure in accordance with the illumination on astronomically significant days of the year. The direction of the main axis of the monument to the rising Sun at the winter solstice is made with an error of no more than 10, which indicates that the ancient organizers of the monument knew astronomical dates well and solved a direct problem by direct observations of the Sun. Measurements, calculations, modeling and field observations confirmed the assumptions about its calendar significance of the monument's discoverer, doctor of historical Sciences V. E. Larichev.

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14

Xu, J. Y., W. J. Liu, J. C. Bian, X. Liu, W. Yuan, and C. Wang. "Method for retrieval of atmospheric water vapor using OH airglow for correction of astronomical observations." Astronomy & Astrophysics 639 (July 2020): A29. http://dx.doi.org/10.1051/0004-6361/201834621.

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Context. Water vapor in the atmosphere undergoes quick spatial and temporal variations. This has a serious impact on ground-based astronomical observations from the visible band to the infrared band resulting from water vapor attenuation and emission. Aims. We seek to show how the sky spectrum of an astronomical observation can be used to determine the amount of precipitable water vapor (PWV) along the line of sight toward the science target. Methods. In this work, we discuss a method to retrieve the PWV from the OH(8-3) band airglow spectrum. We analyzed the influences of the pressure and temperature of the atmosphere and the different water vapor vertical distributions on the PWV retrieval method in detail. Meanwhile, the accuracy of the method was analyzed via Monte Carlo simulations. To further verify the method of PWV retrieval, we carried out cross comparisons between the PWV retrieved from OH airglow and PWV from the standard star spectra of UVES using equivalent widths of telluric absorption lines observed from 2000 to 2016 at Cerro Paranal in Chile. Results. The Monte Carlo tests and the comparison between the two different methods prove the availability the PWV retrieval method from OH airglow. These results show that using OH airglow spectra in astronomical observations, PWVs along the same line of sight as the astronomical observations can be retrieved in real time. Conclusions. We provide a quick and economical method for retrieving the water vapor along the same line of sight of astronomical observation in the real time. This is especially helpful to correcting the effect of water vapor on astronomical observations.

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15

Wu, J., X. Zhang, and Y. Zheng. "IPS Observations at Miyun Station, BAO." International Astronomical Union Colloquium 182 (2001): 189–92. http://dx.doi.org/10.1017/s0252921100000956.

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AbstractIPS observations have recently begun at Miyun Station, Beijing Astronomical Observatory. This paper briefly describes the radio telescope at Miyun Station, discusses the observation and the data reduction procedures, and presents the preliminary results of observations on IPS source 3C48.

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Zhang, X. Z., and J. H. Wu. "IPS Observations at Miyun Station, BAO." Symposium - International Astronomical Union 203 (2001): 580–82. http://dx.doi.org/10.1017/s0074180900220056.

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IPS observations have recently begun at Miyun Station, Beijing Astronomical Observatory. This paper briefly describes the radio telescope at Miyun Station, discusses the observation and the data reduction procedures and presents the preliminary results of observations on IPS source 3C48.

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17

Branham, Richard L. "Techniques for dealing with discordant observations." Symposium - International Astronomical Union 114 (1986): 229–31. http://dx.doi.org/10.1017/s0074180900148247.

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To test any theory such as theories of motion–Newtonian or relativistic–of solar system objects, one must compare the predictions of theory with observation. But discordant observations habitually plague the reducer of astronomical data. To alleviate the baleful effects, particularly harmful when the observations are reduced by the method of least squares, of discordant data investigators almost invariably reject observations whose corresponding (0-C)'s or post-solution residuals exceed a cutoff. But techniques that are insensitive to the assumption that the observational errors are normally distributed, called robust estimation in the literature, have also been developed.

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Kleshchonok, V. V., V. L. Karbovsky, M. I. Buromsky, M. V. Lashko, Yu M. Gorbanev, V. I. Kashuba, C. R. Kimakovskiy, et al. "Star occultation by small bodies of the Solar system: current state of observations in Ukraine." Kosmìčna nauka ì tehnologìâ 28, no. 5 (October 28, 2022): 56–66. http://dx.doi.org/10.15407/knit2022.05.056.

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Observations of stars’ occultations by small bodies of the Solar system allow solving of a series of problems described in this article. The Main Astronomical Observatory of the National Academy of Sciences of Ukraine, together with the Astronomical Observatory of the Taras Shevchenko National University of Kyiv, created a software and hardware complex for observing the star coatings with long-focus telescopes. The complex uses a highly sensitive Apogee Alta U47 CCD camera in time delay integration (TDI) mode. It also includes a focus reducer with a block of light filters. The stationary variant of the complex can be used on the AZT-2 telescope of MAO NAS of Ukraine and the AZT-14 of the Lesniki observation station. The mobile complex is also made on the basis of the telescope of Newton’s system (D = 203 mm, F = 1200 mm) and the computerized installation of Sky-Watcher EQ-5 with the GOTO system for field observations. The worth of occultation observations increases significantly when using several observation points. To this end, we have initiated the gathering of the group of observers and their instrumentation from Ukrainian astronomical institutions, both professional and amateur. The Odesa Astronomical Observatory is presented in the group by the Richie-Chrétien telescope OMT-800 (D = 800 mm, F = 2134 mm) with the CCD camera QHY174M GPS at the Mayaki station and Schmidt system telescope (D = 271.25 mm, F = 440 mm) with the “VIDEO SCAN-415-2001” camera at the Kryzhanivka station. The group also includes several amateur observatories. Among them, there are stations in the village of Petrovka in the Odesa region, the astronomical observatory of Lozova school in the Ternopil region, private astronomical observatory L33 at Ananiiv, the Odesa region, and private observatory L58 “Heavenly Owl” in the town of Velikodolinskoye, the Odesa region. A description of the equipment used in these observation points and several examples of effective observations of occultations obtained by this group are given.

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19

Hald, A. "Galileo's Statistical Analysis of Astronomical Observations." International Statistical Review / Revue Internationale de Statistique 54, no. 2 (August 1986): 211. http://dx.doi.org/10.2307/1403145.

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Pandey, A. "STELLAR EVOLUTION AND THEIR ASTRONOMICAL OBSERVATIONS." Revista Mexicana de Astronomía y Astrofísica Serie de Conferencias 53 (September 1, 2021): 147–50. http://dx.doi.org/10.22201/ia.14052059p.2021.53.29.

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There is a hugh number of stars (~ few hundred billions) of different ages, sizes and masses in our galaxy, the Milky Way, and billions of other galaxies in the Universe. It was extremely challenging for astronomers to classify them into different groups to understand their properties precisely. In general, stars remains in the main sequence phases in the HR diagram for the largest fraction of its life time because it maintains hydro-static equilibrium during this phase. Stars of diverse mass range pass through different evolutionary phases. Some of these end their lives as catastrophic explosions not understood well so far and have a great potential to understand the overall evolution process of stars and in turn evolution of the Universe. Ground and space-based multi-wavelength observations of these objects are crucial to understand them in terms of laws of physics. In near future, advancement of technology demands extensive use of artificial intelligence, neural networks, robotics to understand astronomical observations in a better way.

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21

Kovalevsky, J. "12. Environmental Disturbances of Astronomical Observations." Highlights of Astronomy 11, no. 1 (1998): 214. http://dx.doi.org/10.1017/s1539299600020542.

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Miyazaki, Satoshi. "6 CCD Cameras for Astronomical Observations." Journal of the Institute of Image Information and Television Engineers 67, no. 3 (2013): 220–24. http://dx.doi.org/10.3169/itej.67.220.

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23

Babu, G. S. D. "First Indian astronomical observations in Antarctica." Highlights of Astronomy 9 (1992): 595. http://dx.doi.org/10.1017/s1539299600022644.

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An Indian expedition to Antarctica (to the coastal base Maitri) in the 1989/90 summer made observations of the Sun to study the evolution and decay of supergranules, an experiment which benefited greatly from uninterrupted sessions of a few days. The instrument comprised a heliostat, a 1.2 Å bandwidth blue filter, and a 10 cm aperture lens of about 3 metre focal length with recording on film. During January and February, one continuous period of more than 100 hours completely clear sky occurred, during which the transparency of the atmosphere was excellent. However, at times the seeing was a little poor. More than 2500 photographs were made at 10 minute intervals, as well as some at shorter intervals for studying the evolution of other solar features such as flares.

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Zhan, Yinhu, Yong Zheng, and Chao Zhang. "Astronomical Azimuth Determination by Lunar Observations." Journal of Surveying Engineering 142, no. 2 (May 2016): 04015009. http://dx.doi.org/10.1061/(asce)su.1943-5428.0000158.

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25

Saha, S. K. "Speckle Interferometric Technique for Astronomical Observations." Journal of Optics 32, no. 1 (March 2003): 37–56. http://dx.doi.org/10.1007/bf03354713.

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Steinmetz, T., T. Wilken, C. Araujo-Hauck, R. Holzwarth, T. W. Hansch, L. Pasquini, A. Manescau, et al. "Laser Frequency Combs for Astronomical Observations." Science 321, no. 5894 (September 5, 2008): 1335–37. http://dx.doi.org/10.1126/science.1161030.

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Zhang, Guo-dong, Yan-ben Han, and Fu-yuan Zhao. "Earthquake precursors detected by astronomical observations." Acta Seismologica Sinica 15, no. 1 (January 2002): 82–89. http://dx.doi.org/10.1007/s11589-002-0050-x.

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Allen, Michael. "Climate change will damage astronomical observations." Physics World 35, no. 11 (December 1, 2022): 12i. http://dx.doi.org/10.1088/2058-7058/35/11/14.

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Lourenço, Ana, Sara Carvalho, Teresa Barata, Adriana Garcia, Víctor Carrasco, and Nuno Peixinho. "Solar observations at the Coimbra Astronomical Observatory." Open Astronomy 28, no. 1 (January 1, 2019): 165–79. http://dx.doi.org/10.1515/astro-2019-0015.

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Abstract In 2020, the Geophysical and Astronomical Observatory of the University of Coimbra will celebrate the 95th anniversary of its first spectroheliographic observation. Keeping a daily service of solar observations since then, making almost a century, led to one of the largest continuous solar data collections in the world. This long–term solar database is essential for studies where solar activity is involved. This work reviews the development of synoptic observations made at the Observatory of Coimbra since 1925 and presents a summary of some of the principal stages of the Observatory’s history since its founding in 1772. We refer the main technical improvements and present some perspectives for the near future. One of the most significant upgrades was the installation of a CCD camera in 2007. The transition from photographic emulsion to digital recording methods allowed the development of image analysis algorithms to process solar images and improved data sharing with other institutions. This upgrade enabled also to carry–out modern climate and space weather studies. This valuable advancement makes it possible to create a new catalogue of solar observations to be published in the future.

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Ferradas-Alva, C., G. Ferrero, M. Huamán, W. Guevara-Day, E. Meza, J. Samanes, and P. Becerra. "Seeing measurement on Sasahuine mountain, Moquegua, Perú." Proceedings of the International Astronomical Union 7, S286 (October 2011): 448–51. http://dx.doi.org/10.1017/s174392131200525x.

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AbstractOne of the greatest factors that significantly affect the quality of astronomical images is the atmospheric turbulence causing what we call “seeing”. We present results of the reduction and photometry of astronomical images obtained at the Sasahuine mountain astronomical site (4511 m.a.s.l.), located in the Southern Peruvian Andes, in the department of Moquegua, near the town of Cambrune. These data show preliminary seeing measurements for this site. The present work is part of a bigger investigation program called JANAX which seeks to evaluate potential astronomical observation sites in Peruvian territory through a series of observation missions. The program's aim is to gather data to validate the site for the future construction of a National Astronomical Observatory. The observations were made using an SBIG ST-7MX CCD camera and a BVR standard filter set, attached to a MEADE LX200 356mm telescope.

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Davenhall, Clive. "Dr Katterfelto and the Prehistory of Astronomical Ballooning1." Culture and Cosmos 18, no. 1 (June 2014): 45–53. http://dx.doi.org/10.46472/cc.0118.0209.

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Regular telescopic astronomical observations made from balloons began after World War II, though scientific, particularly meteorological, ballooning dates from the mid-nineteenth century. However, astronomical ballooning has a curious prehistory at the dawn of lighter-than-air travel in the 1780s. The self-styled Dr Katterfelto (c.1743?-99) was a German-born travelling showman, lecturer and considerable self-publicist who in 1784-85 claimed to have made important astronomical discoveries from observations made from a balloon. It is unlikely that he made any such observations, or, indeed, any balloon flights. However, the episode throws some light on the world of the itinerant, eighteenth-century astronomical lecturer and the diffusion of contemporary astronomical and scientific knowledge.

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Klioner, Sergei A., Gérard Petit, Victor A. Brumberg, Nicole Capitaine, Agnès Fienga, Toshio Fukushima, Bernard R. Guinot, et al. "COMMISSION 52: RELATIVITY IN FUNDAMENTAL ASTRONOMY." Proceedings of the International Astronomical Union 4, T27A (December 2008): 55–59. http://dx.doi.org/10.1017/s1743921308025295.

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The tremendous progress in technology which we have witnessed during the last 30 years has led to enormous improvements of observational accuracy in all disciplines of fundamental astronomy. Relativity has been becoming increasingly important for modeling and interpretation of high accuracy astronomical observations during at least these 30 years. It is clear that for current accuracy requirements astronomical problems have to be formulated within the framework of General Relativity Theory. Many high-precision astronomical techniques have already required the application of relativistic effects, which are several orders of magnitude larger than the technical accuracy of observations. In order to interpret the results of such observations, one has to construct involved relativistic models. Many current and planned observational projects can not achieve their goals if relativity is not taken into account properly. The future projects will require the introduction of higher-order relativistic effects. To make the relativistic models consistent with each other for different observational techniques, to formulate them in the simplest possible way for a given accuracy, and to formulate them in a language understandable for astronomers and engineers who have little knowledge of relativity are the challenges of a multidisciplinary research field called Applied Relativity.

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Stephenson, F. Richard. "East Asian Astronomical Records." Highlights of Astronomy 12 (2002): 317–21. http://dx.doi.org/10.1017/s1539299600013642.

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AbstractChinese, Japanese and Korean celestial observations have made major contributions to Applied Historical Astronomy, especially in the study of supernovae, comets, Earth’s rotation (using eclipses) and solar variability (via sunspots and aurorae). Few original texts now survive; almost all extant records exist only in printed versions, often with the loss of much detail. The earliest Chinese astronomical observations extend back to before 1000 BC. However, fairly systematic records are only available since 200 BC - and even these have suffered losses through wars, etc. By around AD 800, many independent observations are available from Japan and Korea and these provide a valuable supplement to the Chinese data. Throughout East Asia dates were expressed in terms of a luni-solar calendar and conversion to the Julian or Gregorian calendar can be readily effected.

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Tsvetkov, D. Yu. "Photometric Observations of Recent Supernovae." International Astronomical Union Colloquium 192 (2005): 189–93. http://dx.doi.org/10.1017/s0252921100009179.

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SummaryRegular photometric observations of sufficiently bright northern supernovae are carried out at Sternberg Astronomical Institute’s observatories. Since 1998 the observations of more than 60 supernovae were obtained on about 150 nights with different telescopes and detectors. We present the data of the observation program, the parameters of light curves for 18 SNe and the light curves for SNe 1999aa, 2001B, 2002bo.

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Bykov, Oleg P. "CCD Observations with Small Telescopes of Moving Bodies." Transactions of the International Astronomical Union 24, no. 3 (2001): 231. http://dx.doi.org/10.1017/s0251107x00000821.

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Astronomy for developing countries must be simple, cheap and attractive. Advanced amateurs with small astronomical CCD instruments could be its base in these regions. Together with the astronomical community and professional astronomers of other countries, amateurs can solve a lot of practical tasks connected with the CCD observations of moving celestial bodies.

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36

Khmil, S. V. "On observations in Schwarzschild background." Symposium - International Astronomical Union 114 (1986): 199–203. http://dx.doi.org/10.1017/s0074180900148193.

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37

Golubaev, А., and A. Mozgova. "The first results of meteor phenomena observations using automated video-spectral meteor patrol of V.N. Karazin Kharkiv National University." Bulletin of Taras Shevchenko National University of Kyiv. Astronomy, no. 59 (2019): 36–41. http://dx.doi.org/10.17721/btsnua.2019.59.36-41.

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In 2018, an observation complex (automatic video-spectral meteor patrol (AVSMP)) was designed and constructed at the Institute of Astronomy, V.N. Karazin Kharkiv National University, for obtaining kinematic and physical characteristics of meteor bodies and their spectra. Cameras were tested in astronomical observations mode with the aim to identify the technical capabilities of the device. This paper presents some of the first results of observations conducted with the help of AVSMP. The created observation complex is intended to expand the material, scientific, as well as educational and scientific base of the Institute of Astronomy. It will be used in the educational process at the Department of Astronomy and Space Informatics of V.N. Karazin KhNU, during practical and laboratory classes, performing bachelor’s and master’s works and developing the newest methods of remote sensing of astronomical objects of the Solar system. In August 2019, the first baseline observations of Perseid’s meteor shower were conducted using AVSMP. At Chuguev observational station of the Institute of Astronomy, where the complex is located, 225 video fragments with meteors in integral light and 98 videos with spectra of meteors were recorded. In Kharkiv, 132 video fragments with meteors in integral light were recorded by the secondary video camera. Of the obtained observation footage, 98 meteors recorded in the integral light are basic, and another 40 video fragments with spectra of meteors have corresponding basic observations in the integral light.

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Isobe, Syuzo. "Effects of artificial light to astronomical observations." JOURNAL OF THE ILLUMINATING ENGINEERING INSTITUTE OF JAPAN 73, no. 4 (1989): 178–85. http://dx.doi.org/10.2150/jieij1980.73.4_178.

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Unterguggenberger, Stefanie, Stefan Noll, Wuhu Feng, John M. C. Plane, Wolfgang Kausch, Stefan Kimeswenger, Amy Jones, and Sabine Moehler. "Measuring FeO variation using astronomical spectroscopic observations." Atmospheric Chemistry and Physics 17, no. 6 (March 28, 2017): 4177–87. http://dx.doi.org/10.5194/acp-17-4177-2017.

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Abstract. Airglow emission lines of OH, O2, O and Na are commonly used to probe the MLT (mesosphere–lower thermosphere) region of the atmosphere. Furthermore, molecules like electronically excited NO, NiO and FeO emit a (pseudo-) continuum. These continua are harder to investigate than atomic emission lines. So far, limb-sounding from space and a small number of ground-based low-to-medium resolution spectra have been used to measure FeO emission in the MLT. In this study the medium-to-high resolution echelle spectrograph X-shooter at the Very Large Telescope (VLT) in the Chilean Atacama Desert (24°37′ S, 70°24′ W; 2635 m) is used to study the FeO pseudo-continuum in the range from 0.5 to 0.72 µm based on 3662 spectra. Variations of the FeO spectrum itself, as well as the diurnal and seasonal behaviour of the FeO and Na emission intensities, are reported. These airglow emissions are linked by their common origin, meteoric ablation, and they share O3 as a common reactant. Major differences are found in the main emission peak of the FeO airglow spectrum between 0.58 and 0.61 µm, compared with a theoretical spectrum. The FeO and Na airglow intensities exhibit a similar nocturnal variation and a semi-annual seasonal variation with equinoctial maxima. This is satisfactorily reproduced by a whole atmosphere chemistry climate model, if the quantum yields for the reactions of Fe and Na with O3 are 13 ± 3 and 11 ± 2 % respectively. However, a comparison between the modelled O3 in the upper mesosphere and measurements of O3 made with the SABER satellite instrument suggests that these quantum yields may be a factor of ∼ 2 smaller.

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Davydov, V. Yu. "Compensation of refraction in astronomical interference observations." Measurement Techniques 36, no. 6 (June 1993): 662–67. http://dx.doi.org/10.1007/bf00980011.

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Peeters, E. "Astronomical observations of the PAH emission bands." EAS Publications Series 46 (2011): 13–27. http://dx.doi.org/10.1051/eas/1146002.

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Mielczarek, Jakub. "From causal dynamical triangulations to astronomical observations." EPL (Europhysics Letters) 119, no. 6 (September 1, 2017): 60003. http://dx.doi.org/10.1209/0295-5075/119/60003.

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Marché II, Jordan. "Edward Hitchcock's Promising Astronomical Career." Earth Sciences History 12, no. 2 (January 1, 1993): 180–86. http://dx.doi.org/10.17704/eshi.12.2.p320q01j5v627552.

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Edward Hitchcock's observations of the Great Comet of 1811, the partial solar eclipse of 17 September 1811, and others for determining his latitude and longitude, marked the development of a mature research program in theoretical and practical astronomy which he pursued vigorously for more than two years until his health failed. Hitchcock's results were communicated to astronomer John Farrar of Harvard College and extracts were published in the Memoirs of the American Academy of Arts and Sciences. This paper compares Hitchcock's comet sightings with those of Farrar himself. Although astronomy did not become Hitchcock's final career choice, the mental skills which he perfected through instrumental observation and mathematical reduction were to be of service throughout his later professional life as an earth scientist.

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Harutyunian, Hayk, and Areg Mickaelian. "Modern facilities in astronomy education." Proceedings of the International Astronomical Union 2, SPS5 (August 2006): 263–64. http://dx.doi.org/10.1017/s1743921307007119.

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AbstractAstronomical education is entering a new stage of development which is closely connected with the development of new technologies for communication, computing and data visualization. We discuss this evolution in the context of astronomy education in Armenia. As students spend only a short time in Byurakan Observatory for training in observations, they are not able to carry out systematic astronomical observations. Hence their training places emphasis on the use of astronomical archives and analysis of observational data obtained previously with the Byurakan telescopes and other ground-based and space telescopes. Thus, one of the aims of the Armenian Virtual Observatory is to support the training of students in this modern context.

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Yoshizawa, M. "New Astrometric Instrumentation in Japan." Symposium - International Astronomical Union 166 (1995): 31–34. http://dx.doi.org/10.1017/s0074180900227794.

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The meridian circle is one of the most fundamental instrument in the field of astrometry where the astronomical objects are studied observationally for positions and their changes on the celestial sphere. At the Tokyo Astronomical Observatory (= National Astronomical Observatory since July, 1988) the Gautier Meridian Circle of 1903 was used until 1982 for various international meridian circle observations like SRS and NPZT programs, as well as for observations of OB stars, and the Moon and planets.

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Ratnatunga, Kavan U. "Astronomy Research via the Internet." Transactions of the International Astronomical Union 24, no. 3 (2001): 279–90. http://dx.doi.org/10.1017/s0251107x0000095x.

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AbstractSmall developing countries may not have a dark site with good seeing for an astronomical observatory or be able to afford the financial commitment to set up and support such a facility. Much of astronomical research today is however done with remote observations, such as from telescopes in space, or obtained by service observing at large facilities on the ground. Cutting-edge astronomical research can now be done with low-cost computers, with a good Internet connection to get on-line access to astronomical observations, journals and most recent preprints. E-mail allows fast easy collaboration between research scientists around the world. An international program with some short-term collaborative visits, could mine data and publish results from available astronomical observations for a fraction of the investment and cost of running even a small local observatory. Students who have been trained in the use of computers and software by such a program would also be more employable in the current job market. The Internet can reach you wherever you like to be and give you direct access to whatever you need for astronomical research.

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Guélin, Michel. "Radio and Millimetre Observations of Less Complex Molecules." Symposium - International Astronomical Union 120 (1987): 171–81. http://dx.doi.org/10.1017/s0074180900153987.

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Progress in laboratory and astronomical instrumentation has renewed the already large interest for simple astrophysical molecules. On the laboratory side, one of the most notable advances has been the spectroscopic observation of an increasing number of small reactive molecular species. On the astronomical side, the access to submillimetre wavelengths and the completion of millimetric interferometers and large single-dish telescopes, have allowed the detection of many new molecular species and open the way for detailed studies of the distribution of molecules in interstellar and circumstellar clouds.

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Griffin, R. E. M. "Through a Glass Darkly: The Status of Archiving Astronomical Spectra." Highlights of Astronomy 10 (1995): 607–17. http://dx.doi.org/10.1017/s1539299600012259.

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Astronomical research comprises a curious mixture of team work and individualism. From the hardware point of view data are ends in themselves, while from a strictly scientific aspect their acquisition is but the first stage in the complicated process of building astrophysical models. This dichotomy is reflected in a polarization of attitudes regarding the handling of observational data, and the activity of creating archives of astronomical data for use by posterity has consequently tended to fall in no-man’s-land. To the technology team, a telescope that can successfully deliver a data-bank full of raw observations has achieved its specification, while to the scientist who is under pressure to publish papers on fresh science, the concept of voluntarily creating public archives out of data originating from personal ideas may seem more than a little alien. Nevertheless, the formation of useable and efficient archives of astronomical observations is an activity that has taken on new meaning with the advent and monopoly of digital detectors; it is a procedure that builds bridges as well as access routes and it opens new global perspectives for astronomical data, but it still relies too heavily on individual initiatives.

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Taufikurrahman, Arief. "Sistem Kontrol Teleskop Ioptron AZ Mount Pro Berbasis Android." AL - AFAQ : Jurnal Ilmu Falak dan Astronomi 4, no. 2 (December 11, 2022): 254–59. http://dx.doi.org/10.20414/afaq.v4i2.5439.

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The development of astronomical observation instrument technology makes astronomical observations easier and simpler. One of them is a telescope equipped with a computerized motor. Control of the telescope can now be done wirelessly through an android application on a smartphone, one of which is the Sky Safari Plus 6 application. By using the Ioptron AZ Mount Pro telescope, the telescope can be controlled using the Sky Safari Plus 6 application wirelessly via a smartphone without using a computer and additional driver.

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Ningombam, Shantikumar S., H.-J. Song, S. K. Mugil, Umesh Chandra Dumka, E. J. L. Larson, Brijesh Kumar, and Ram Sagar. "Evaluation of fractional clear sky over potential astronomical sites." Monthly Notices of the Royal Astronomical Society 507, no. 3 (September 9, 2021): 3745–60. http://dx.doi.org/10.1093/mnras/stab1971.

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ABSTRACT The estimation of the night-time cloud fraction (CF) is found to be one of the key parameters for evaluating the number of useful nights at an astronomical site. This work evaluates useful astronomical night-time observation over eight sites using a minimum threshold of CF from 21 years (2000–2020) of ground-based hourly visual and daily satellite data along with 41 years (1980–2020) of long-term hourly reanalysis data. The estimated number of photometric nights is underestimated by 8–24 per cent using the reanalysis data at Indian Astronomical Observatory-Hanle in comparison with the visual observations, while the estimated number of spectroscopic nights is 70–75 per cent per year and in good agreement with the visual observations. Among the astronomical sites, Paranal is found to be the best for astronomical observations, with 87 per cent spectroscopic nights per year. On the other hand, Hanle, Ali and Devasthal, located in the Himalayan region, exhibit an average of 68–78 per cent spectroscopic nights per year based on long-term reanalysis data, while Merak exhibits 61–68 per cent spectroscopic nights per year. Vertical profiles and global horizontal distributions for CF and related variable parameters are further compared among the sites. Global CF trends based on 41 years of reanalysis data show a decreasing tendency over most land regions and an increasing tendency over oceanic regions as well as over the Sahara desert, Middle East, and Indian subcontinent along the adjacent Tibetan Plateau. Such different CF trends between the ocean and land regions are thought to be the result of differential surface warming and water vapour changes associated with climate change.

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Journal articles on the topic 'And Astronomical Observations'

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