Relevant bibliographies by topics / Mount John University Observatory

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Academic literature on the topic 'Mount John University Observatory'

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Published: 4 June 2021
Last updated: 7 February 2022

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Journal articles on the topic "Mount John University Observatory"

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Cottrell, Peter. "Long term photometric programmes at Mount John University observatory." Experimental Astronomy 5, no. 1-2 (March 1994): 99. http://dx.doi.org/10.1007/bf01583817.

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Mohr, J. L., R. A. Johnston, and P. L. Cottrell. "Optical Turbulence Measurements and Models for Mount John University Observatory." Publications of the Astronomical Society of Australia 27, no. 3 (2010): 347–59. http://dx.doi.org/10.1071/as10008.

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AbstractSite measurements were collected at Mount John University Observatory in 2005 and 2007 using a purpose-built scintillation detection and ranging system. C2N(h) profiling indicates a weak layer located at 12–14 km above sea level and strong low altitude turbulence extending up to 5 km. During calm weather conditions, an additional layer was detected at 6–8 km above sea level. V(h) profiling suggests that tropopause layer velocities are nominally 12–30m s−1, and near-ground velocities range between 2 and 20m s−1, dependent on weather. Little seasonal variation was detected in either C2N(h) and V(h) profiles. The average coherence length, r0, was found to be 7±1 cm for the full profile at a wavelength of 589 nm. The average isoplanatic angle, θ0, was 1.0±0.1 arcsec. The mean turbulence altitude, , was found to be 2.0±0.7 km above sea level. No average in the Greenwood frequency, fG, could be established due to the gaps present in the V(h) profiles obtained. A modified Hufnagel-Valley model was developed to describe the C2N(h) profiles at Mount John, which estimates r0 at 6 cm and θ0 at 0.9 arcsec. A series of V(h) models were developed, based on the Greenwood wind model with an additional peak located at low altitudes. Using the C2N(h) model and the suggested V(h) model for moderate ground wind speeds, fG is estimated at 79 Hz.
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Cropp, Malcolm, Karen R. Pollard, and Jovan Skuljan. "Spectroscopy of southern δ Scuti stars." International Astronomical Union Colloquium 193 (2004): 275–78. http://dx.doi.org/10.1017/s0252921100010782.

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AbstractFour δ Scuti stars were observed with the HERCULES fibrefed échelle spectrograph at Mount John University Observatory, New Zealand. These observations were analysed by looking at the radial velocity variations as given by a cross-correlation technique as well as spectral line moment variations. These results were compared to published photometric studies of these stars to see if the modes identified in the photometry were also present in the spectroscopic data obtained.
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Watson, R. D., S. R. D. West, William Tobin, and A. C. Gilmore. "CCD Photometry of the Eclipsing Binary HV 2274 in the Large Magellanic Cloud." Symposium - International Astronomical Union 151 (1992): 509–13. http://dx.doi.org/10.1017/s0074180900122843.

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B, V and Ic photometry of the eclipsing binary HV 2274, located in the LMC, was obtained with the CCD system at the Mount John University Observatory, Lake Tekapo, New Zealand during 1990. Over 100 data points were acquired in each filter to an estimated precision of 0.02 mag. The flat maxima evident in the light curves suggest that the system, which is currently classed as an interacting candidate, should probably be considered as a detached one. A revised orbital period based on the inclusion of current data is presented. Eclipse timings indicate an eccentric orbit. An apsidal period in the vicinity of 120 yr is likely.
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Cottrell, P. L., L. Skuljan, P. M. Kilmartin, C. Gilmore, and W. A. Lawson. "R Coronae Borealis Stars: Long-Term Photometric & Spectroscopic Studies." Highlights of Astronomy 11, no. 1 (1998): 379. http://dx.doi.org/10.1017/s1539299600021298.

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For more than a decade we have been able to acquire and analyse a significant amount of photometric data of the highly variable R Coronae Borealis (RCB) stars. This has made been possible by a photometric service observing programme instigated at the Observatory. These photometric data have been combined with less extensive spectroscopic coverage, particularly of the decline phase of these stars. These have been supplemented by observations obtained at Mount Stromlo and Siding Spring Observatories for a radial velocity study. Significantly more spectroscopic observations are now being acquired with the development of a new medium resolution spectrograph at Mount John University Observatory.In this poster we will present recent photometric and spectroscopic results for a number of the RCB stars in our sample. This observational and analysis work can be used to provide further insight into the nature of these stars, their likely progeny and progenitors and the processes that are involved in the formation and evolution of the obscuring dust clouds which cause the decline phase.
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Cottrell, P. L., and W. A. Lawson. "Pulsations and declines of RCB stars." International Astronomical Union Colloquium 139 (1993): 212–13. http://dx.doi.org/10.1017/s0252921100117397.

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AbstractWe have continued to observe many of the R Coronae Borealis (RCB) stars and other related hydrogen-deficient carbon stars. We wish to more fully investigate the photometric and spectroscopic properties of these peculiar stars.The UBVRI photometric data (acquired at Mount John University Observatory, MJUO) are being used to investigate whether the periods determined by Lawson et al. (1990), based on time intervals of up to 1100 d, are still evident in the larger datasets which now cover time intervals of up to 2200 d.The long time baseline of photometric observations that we have been able to acquire has enabled us to accumulate an extensive database of decline photometry. These are used to investigate links with the pulsations at maximum light in order to get a better understanding of this remarkable phenomenon.
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Gebhardt, P., A. Schrimpf, C. Dersch, M. Spasovic, L. Bringmann, H. P. Singh, R. Gupta, and S. M. Kanbur. "U–SMART : SMALL APERTURE ROBOTIC TELESCOPES FOR UNIVERSITIES." Revista Mexicana de Astronomía y Astrofísica Serie de Conferencias 51 (April 13, 2019): 44–46. http://dx.doi.org/10.22201/ia.14052059p.2019.51.08.

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A group of universities have come together with the aim of designing and developing small aperture robotic telescopes (SmART) for use by students to observe variable stars and transient follow-ups. The group is deliberating on the components of the robotic system e.g. the telescope, the mount, the back-end camera, control software etc and their integration keeping in mind the scientific objectives. The Marburg group is studying variable stars using photometric and spectroscopic observations in a small local observatory and via analysis of photo plate archival data mainly from Sonneberg observatory (Thuringa, Germany). Our goal is to setup a small, affordable observatory at Marburg University with full remote access to all components, including a spectrometer. Among others, the future measurements can be follow-ups, of variable stars, exoplanet search and spectroscopic measurements, e.g. in cooperation with the BRITE-constellation. We would like to invite other universities to join the project and cooperate in setting up a University network of small aperture robotic telescopes (U-SmART) around the globe.
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Woollands, R. M., P. L. Cottrell, and A. Udalski. "Photometric Analysis of Magellanic Cloud R Coronae Borealis Stars in the Recovery Phases of Their Declines." Publications of the Astronomical Society of Australia 26, no. 1 (2009): 85–91. http://dx.doi.org/10.1071/as08028.

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AbstractThis paper presents the initial results of a multi-site photometric programme to examine the extraordinary behaviour displayed by 18 R Coronae Borealis (RCB) stars in the Magellanic Clouds (MCs). RCB stars exhibit a unique variability whereby they undergo rapid declines of up to several magnitudes. These are thought to be caused by the formation of dust in the stellar environment which reduces the brightness. The monitoring programme comprised the collection of UBVRI photometric data using five telescopes located at three different southern hemisphere longitudes (Las Campanas Observatory in Chile, Mount John University Observatory in New Zealand, and the Southern African Large Telescope, SALT, in South Africa). Examination of the data acquired in the V and I filters resulted in the identification of a total of 18 RCB declines occurring in four stars. Construction of colour–magnitude diagrams (V versus V – I), during the recovery to maximum light were undertaken in order to study the unique colour behaviour associated with the RCB declines. The combined recovery slope for the four stars was determined to be 3.37 ± 0.24, which is similar to the value of 3.1 ± 0.1 calculated for galactic RCB stars (Skuljan et al. 2003). These results may imply that the nature of the dust (i.e. the particle size) is similar in both our Galaxy and the MCs.
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Pollard, Karen, P. M. Kilmartin, A. C. Gilmore, and P. L. Cottrell. "A Photometric and Spectroscopic Study of Southern RV Tauri Stars." International Astronomical Union Colloquium 139 (1993): 216. http://dx.doi.org/10.1017/s0252921100117427.

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AbstractA program to obtain photometric and spectroscopic (high and medium resolution) observations of a number of southern RV Tauri stars has been undertaken over the past two years at the Mount John University Observatory (MJUO). Eleven RV Tauri stars of both RVa (constant mean magnitude) and RVb (varying mean magnitude) photometric type have been chosen as well as normal and weak metal lined RV Tauri stars.Most program stars display the alternating deep and shallow semi-regular light variations as well as the light curve - colour curve phase lag characteristic of RV Tauri stars. Fourier analyses of the light curves have revealed the dominant periodicities (see figure 1) and allowed phasing of the spectroscopic observations.High resolution échelle spectra obtained of these stars around the Hα region display the complex emission and absorption structure of the Hα line at various phases. Metallic lines show emission and line doubling or ‘splitting’ - profiles characteristic of the shock wave that propagates through the line-formation regions of these stars during a pulsational cycle. Spectra at specific phases will be used in an abundance analysis of selected RV Tauri stars.
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Shutt, T. R., E. Brunsden, and K. R. Pollard. "Spectroscopic frequency and mode identification of γ Doradus stars HD 109799 and HD 103257." Monthly Notices of the Royal Astronomical Society 507, no. 1 (June 16, 2021): 1149–56. http://dx.doi.org/10.1093/mnras/stab1972.

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ABSTRACT Following frequency and mode identification of two candidate γ Doradus stars, HD 103257 and HD 109799, both can be categorized as bona-fide members of the class. Over 250 high-resolution spectra of the two stars were collected at University of Canterbury Mount John Observatory (UCMJO) using the High Efficiency and Resolution Canterbury University Large Echelle Spectrograph (HERCULES) spectrograph. The spectra were cross-correlated with a synthetic δ-function template to produce line-profiles and further augmented with high-quality photometry from the Transiting Exoplanet Survey Satellite (TESS) mission, the Wide Angle Search for Planets (WASP) archive, and HIPPARCOS catalogue for frequency and mode analysis. Frequency analysis was carried out using FAMIAS and SigSpec. Two pulsation frequencies were identified in the spectra for HD 103257: 1.22496 ± 0.00001 and 1.14569 ± 0.00002 d−1, explaining 58.9 ${{\ \rm per\ cent}}$ of the variation across the line profiles. Both frequencies were characterized with best-fitting modes of (ℓ, m) = (1, 1). Two pulsation frequencies were identified in the spectra for HD 109799: 1.48679 ± 0.00002 and 1.25213 ± 0.00002 d−1, explaining 32.6 ${{\ \rm per\ cent}}$ of the variation across the line profiles. Both frequencies also yielded individual mode fits of modes (ℓ, m) = (1, 1). The excellent quality photometry from TESS observations has proven complementary to the work herein, and will provide a meaningful opportunity for deeper analysis of additional stars in the HERCULES catalogue. This will be a key component in the continued development of models relating to the processes within γ Doradus stars.
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Books on the topic "Mount John University Observatory"

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Hearnshaw, J. B. Mt John, the first 50 years: A celebration of half a century of optical astronomy at the University of Canterbury. Christchurch, New Zealand: Canterbury University Press, 2015.

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J, Tobin William, Evans Gill M, Tirikatene-Sullivan Whetu, Bateson Frank M, Cottrell Peter L, Hearnshaw John B, Kilmartin Pamela M, et al., eds. Stars in a cluster: Mt John University Observatory : tenth anniversary of the McLellan Telescope : hundredth anniversary of the Townsend Telescope : publications 1979-1995. Christchurch, New Zealand: Department of Physics & Astronomy, University of Canterbury, 1996.

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Book chapters on the topic "Mount John University Observatory"

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Tobin, William, A. C. Gilmore, Alan Wadsworth, and S. R. D. West. "First CCD Observations of Magellanic Cloud Variable Stars from the Mt John University Observatory, New Zealand." In The Magellanic Clouds, 381. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_100.

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Yoshimura, Hirokazu. "The Detection of Global Convection on the Sun by an Analysis of Line Shift Data of the John M. Wilcox Solar Observatory at Stanford University." In The Internal Solar Angular Velocity, 89–95. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3903-5_13.

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Burt, Stephen, and Tim Burt. "Weather observations in Oxford." In Oxford Weather and Climate since 1767, 6–27. Oxford University Press, 2019. http://dx.doi.org/10.1093/oso/9780198834632.003.0002.

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This chapter gives some brief account of weather observations at Oxford prior to 1767, including John Locke’s observation of smoke from the Great Fire of London in 1666. However, the main purpose of the chapter is to describe the history of the Radcliffe Observatory and the work of Thomas Hornsby in its funding, design and construction. Hornsby, himself a keen meteorologist, included weather observations from the very beginning and these have been continued to the present day, both in the time when the Observatory was operated by the Radcliffe Trust and since 1935, when the Observatory has been in the ownership of Oxford University and run by the School of Geography.
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MacDonald, Alexander. "Piety, Pioneers, and Patriots: The First American Observatories." In The Long Space Age. Yale University Press, 2017. http://dx.doi.org/10.12987/yale/9780300219326.003.0002.

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In the earliest period of American history, astronomy and the exploration of the heavens was considered a hallmark of intellectual development and a noble endeavor for the colonial elite. In the wake of the American Revolution, the desire to signal a robust and independent national presence intensified in all areas, including astronomy. Major efforts in this regard were led by John Quincy Adams. From the mid-1830s, and for the next four decades, the construction of observatories accelerated rapidly as part of what has been referred to as “the American Observatory Movement” starting with university and college observatories and progressing to observatories with broader social contexts. An observatory located on top of a Philadelphia high school was an unlikely inflexion point in the history of American space exploration. The motivations of religious belief also played a significant role in the funding of early American observatories. The Georgetown Observatory was a point of contention between American Jesuits and the Superior General in Rome, and politics and ambition elevated the Navy’s Depot for Charts and Instruments to America’s first National Observatory.
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Headrick, Daniel R. "Displaying Information Maps and Graphs." In When Information Came of Age. Oxford University Press, 2001. http://dx.doi.org/10.1093/oso/9780195135978.003.0006.

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Not all those who contributed to the culture of information were members of the bourgeoisie. In the area of visual representation, two names—Cassini and Harrison—illustrate how widely the culture of information had spread to all classes of society. For over a century, four generations of Cassinis dominated French astronomy and cartography. The founder of this illustrious lineage, Giovanni Domenico Cassini (1625 –1712), was a professor of astronomy at the University of Bologna when he was recruited to head the Paris Observatory in 1669. He became a French citizen, changed his name to Jean-Dominique Cassini, and entered into the privileged elite of the Old Regime. At the observatory, Jean Cassini discovered the rotation of the planets and developed a method of determining longitude by sighting the moons of Jupiter. He also launched the most elaborate cartographic project of his time, the map of France known as “la carte de Cassini.” His son Jacques Cassini (1677–1756), known as Cassini II, succeeded him at the observatory and as a member of the French Academy of Sciences. Jacques carried on his father’s work of measuring the arc of the meridian—a necessary but preliminary step in constructing an accurate map of France. In this effort, which was to take fifty years, Jacques Cassini was seconded by his son César-François Cassini de Thury (1714 –1784), known (of course) as Cassini III, who was also a member of the Academy and director of the observatory. When César-François died in 1784, his son Jacques-Dominique (1748 – 1845), count of Cassini (Cassini IV), carried on as head of the observatory, member of the academy, and director of the map project. The Cassinis’ Carte de France, completed in 1793, was a masterpiece of Old Regime cartography. Jacques­ Dominique’s son Gabriel (1784 –1832) broke with the family tradition and became a botanist. In contrast to this story of distinction and privilege, John Harrison’s life was one of struggle and hardship, rewarded by success only at the very end. Harrison (1693 –1776) was the son of a carpenter who taught himself how to build clocks.
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Reid, Peter H. "A Lovely, Creative Woman and an All-American Boy from the South." In Every Hill a Burial Place, 18–21. University Press of Kentucky, 2020. http://dx.doi.org/10.5810/kentucky/9780813179988.003.0003.

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Peverley (Peppy) Dennett Kinsey came from a prominent New England background. Her grandfather, Tyler Dennett, received the Pulitzer Prize for his biography of John Hay. Her father graduated Phi Beta Kappa from Harvard and was director of the World Peace Foundation and president of the American Scandinavian Foundation. She attended prestigious schools, including Mount Holyoke College, where she became an accomplished dancer. Peppy’s longtime friend Victoria Ferenbach speculates on what might have happened on Impala Hill, where Peppy died. Bill Kinsey grew up in North Carolina, attended Washington and Lee University, where he excelled academically, and participated in a great many activities, such as, the Washington Literary Society, publication of Ariel, track, rifle team, and the International Relations Club.
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deBuys, William. "Mt. Graham: The Biopolitics of Change." In A Great Aridness. Oxford University Press, 2011. http://dx.doi.org/10.1093/oso/9780199778928.003.0015.

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The site manager for the Mt. Graham International Observatory (MGIO) met us at the locked gate to the Telescope Road. He was not there to greet us. John Ratje had driven out from Tucson, starting before dawn and traveling not less than two and a half hours, to demand that we surrender to him a key that would have opened the gate. A member of his staff had loaned it to us the afternoon before, but Ratje swept aside that troublesome fact. Ratje also demanded the two-way radio we’d been issued to assure safety on the narrow road to the mountaintop. “That’s University of Arizona property,” he said. “It should not have been given to you.” Our shock at his demands no doubt showed in our faces. Ratje wanted to forestall argument, so he added ominously, “University police are on their way.” I’d been about to unlock the gate when he stepped from the trees. His truck was parked nearby, and he’d no doubt been waiting quite a while. He was a big man, but uncomfortable. His voice had a quaver of anxiety. At first I thought he merely wanted to inspect our one-day permit for entering the Red Squirrel Refugium, the restricted area that surrounds the observatory, at the top of the mountain. I’d obtained the permit from the Forest Service the previous day in Safford; I pulled it now from my shirt pocket, unfolded it, and extended it to him, but he ignored it. We did not have permission to go in, he repeated: “This area is ours.” I stammered a question or two, but the answer did not vary: our entry was barred, and police would soon arrive to ensure our compliance. Then my companion, Peter Warshall, a conservation biologist whose name was recorded on the permit along with mine, asked, “Is this about me? Am I the reason you won’t let us in?” “Your name was part of the discussion,” Ratje said. A discussion? I had thought our visit was routine.
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Smallman-Raynor, Matthew, and Andrew Cliff. "Tracking Epidemics." In War Epidemics. Oxford University Press, 2004. http://dx.doi.org/10.1093/oso/9780198233640.003.0017.

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In studies of past, present, and likely future disease distributions, the ‘added value’ provided by the geographer lies in three main areas: detecting spatial concentrations of disease; isolating the processes (environmental, social, demographic, and pathogenic) which cause these disease hotspots; and in enhancing our understanding of the space–time dynamics of disease spread. This is as true of war-related epidemics as of any others. Within geography, there is a long-standing tradition of mapping disease. In this early history, the incidence maps of yellow fever produced in 1798 are often given pride of place (Robinson, 1982). These were, however, pre-dated by maps of topics as diverse as hospital capacities and the distribution of dressing-stations on a battlefield, through to maps of pestilential swamps and other hostile medical environments. But, so far as most epidemiological reports were concerned, such maps were usually incidental. The breakthrough in disease mapping occurred in the middle of the nineteenth century with the cholera map produced by Dr John Snow to accompany the second edition of his prize-winning essay On the Mode of Communication of Cholera (1855a). What set Snow’s work apart was not the cartography (dot maps, which were a well-established cartographic device, to show the geographical distribution of individual cholera deaths), but his inductive reasoning from the map. By showing what he termed the ‘topography of the outbreak’, Snow was able to draw inferences about the central source of infection. The use of mapping as an important device for suggesting hypotheses of medical interest may be traced through to the present day. For war and disease, the classic example is the Seuchen Atlas. This atlas of epidemic disease (Zeiss, 1942–5; Anderson, 1947) was conceived by the German army as an adjunct to war, enhancing its ability to mount military campaigns. The atlas was produced as separate sheets over the years 1942–5. Its distribution was confined to military institutes and to those German university institutes involved in training medical students. The scope of the atlas was not global but confined largely to those areas where the Army High Command expected to be fighting.
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Conference papers on the topic "Mount John University Observatory"

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Mohr, Judy L., Rachel A. Johnston, C. Clare Worley, and Peter L. Cottrell. "Optical turbulence profiling at Mount John University Observatory." In SPIE Remote Sensing, edited by Anton Kohnle, Karin Stein, and John D. Gonglewski. SPIE, 2008. http://dx.doi.org/10.1117/12.799756.

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Liu, Jiayu, Vishnu Anand Muruganandan, Richard Clare, Maria Cruz Ramirez Trujillo, and Stephen J. Weddell. "A Tip-Tilt Mirror Control System for Partial Image Correction at UC Mount John Observatory." In 2020 35th International Conference on Image and Vision Computing New Zealand (IVCNZ). IEEE, 2020. http://dx.doi.org/10.1109/ivcnz51579.2020.9290543.

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