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1
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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Innis, J. L., K. Thompson, and D. W. Coates. "The Monash University Observatory: equipment and research." Symposium - International Astronomical Union 118 (1986): 293–94. http://dx.doi.org/10.1017/s0074180900151563.
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The Monash Observatory, located at Mount Burnett, Victoria, seventy kilometres east of the city of Melbourne, at a latitude of 38° S has a 0.45-m Cassegrainian and a 0.25-m Newtonian telescope. Both are equipped for photoelectric photometry, with microcomputer-based data logging systems. The 0.45-m has recently replaced the observatory's original 0.4-m Newtonian. Our site is near the coast, and has less than 20% photometric weather. Access to the telescopes and facilities of Mount Stromlo and Siding Spring Observatories (MSSSO) increases our observing time and the scope of our research. For a description of the Monash Observatory at mid-1984 see Coates et al, (1984).
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Gantz, Joan. "Observatory Publications." International Astronomical Union Colloquium 110 (1989): 134–35. http://dx.doi.org/10.1017/s0252921100003195.
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My library dates back to 1904, shortly after Dr. George Ellery Hale came west from Yerkes Observatory to the sleepy little town of Pasadena, California to start the Mount Wilson Solar Observatory. The classification system used in this new library was published for the International Council by the Royal Society of London. Over time the librarians managed to acquire many complete runs of observatory publications from all over the world, and they were arranged alphabetically according to the place where they were published. University publications have been included in this collection as well.
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Smyrnov, I., and N. Levinskova. ""WHITE ELEPHANT" IN UKRAINIAN CARPATHIANS MOUNTAINS: ON RESTORATION OF A FORMER MILITARY ASTRONOMICAL-METEOROLOGICAL OBSERVATORY." Visnyk Taras Shevchenko National University of Kyiv. Military-Special Sciences, no. 2 (39) (2018): 55–58. http://dx.doi.org/10.17721/1728-2217.2018.39.55-58.
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The article deals with the fate of the astronomical-meteorological observatory, which was built in the Eastern Carpathеs on the Hill of Pip-Ivan (height 2028 m) in 1938, when the Carpathian region was part of Poland. Another name of the observatory is "White Elephant", because in the winter under the snow the observatory's house resembles the shape of the elephant. Mount Pip Ivan has a pyramidal shape with the presence of ancient forms of glacial relief, composed of sandstone. The observatory was equipped with the most up-to-date scientific equipment, in particular, a telescope, astrograph and refractor of British production. The Observatory was destroyed during the Second World War. Currently, with joint efforts of Ukraine and Poland, in particular with the participation of the University of Warsaw and the Precarpathian University named after V. Stefanyk of Ivano-Frankivsk the restoration of the observatory is under way, as well as the construction of an International Center for Ukrainian and Polish Students Youth Meetings focusing on research in geography, meteorology, geology, seismology, astronomy and biology. Keywords: astronomical-meteorological observatory, Mount Pіp Ivan, restoration, Obserwatorium fund, research in the fields of geography, meteorology, geology, seismology, astronomy and biology.
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Hearnshaw, J. B., D. M. Ward, and L. C. Watson. "LUCIFERS: a photoelectric radial-velocity spectrometer at Mt John University Observatory." Experimental Astronomy 5, no. 1-2 (March 1994): 141–46. http://dx.doi.org/10.1007/bf01583825.
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Hyland, A. R., and D. J. Faulkner. "From the Sun to the Universe—The Woolley and Bok Directorships at Mount Stromlo." Publications of the Astronomical Society of Australia 8, no. 2 (1989): 216–28. http://dx.doi.org/10.1017/s1323358000023353.
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AbstractThe twenty years following the Second World War saw great changes in the research interests of the Observatory at Mount Stromlo, with the early emphasis on solar and geophysical phenomena giving way to stellar and galactic astrophysics. This paper traces the development of the astrophysical research work during the directorships of Woolley, who initiated the change of direction, and of Bok, who continued it. Apart from the shift in the Observatory’s research interests, these years were distinguished by (i) an outstanding period of telescope acquisition, which saw the commissioning of the 74 inch reflector, the 50 inch (formerly the Great Melbourne Telescope), the Yale/Columbia refractor (relocated from South Africa), and the Uppsala Schmidt; (ii) an Australia-wide site-testing programme and the consequent establishment of Siding Spring Observatory with the 40 inch, 24 inch and 16 inch reflectors (the site has subsequently, of course, also become the home of the Anglo-Australian Telescope, the U.K. Schmidt, and the ANU 2.3 m Advanced Technology Telescope); (iii) the incorporation of several major technological developments into the instrument complement of the Observatory, including photo-electric photometry, coudé spectroscopy, spectrum scanners, polarization instruments, and digital computers; (iv) the establishment of the link with the Australian National University and the consequent transformation of the Commonwealth Observatory into the Mount Stromlo Observatory; and (v) the setting up of a large and vigorous graduate school, comprising, at Bok’s departure, about fifteen PhD students on course.
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Rawson, Helen C. "James Gregory, the University observatory and the early acquisition of scientific instruments at the University of St Andrews." Notes and Records: the Royal Society Journal of the History of Science 69, no. 2 (February 25, 2015): 109–33. http://dx.doi.org/10.1098/rsnr.2014.0026.
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James Gregory, inventor of the reflecting telescope and Fellow of the Royal Society, was the first Regius Professor of Mathematics of the University of St Andrews, 1668–74. He attempted to establish in St Andrews what would, if completed, have been the first purpose-built observatory in the British Isles. He travelled to London in 1673 to purchase instruments for equipping the observatory and improving the teaching and study of natural philosophy and mathematics in the university, seeking the advice of John Flamsteed, later the first Astronomer Royal. This paper considers the observatory initiative and the early acquisition of instruments at the University of St Andrews, with reference to Gregory's correspondence, inventories made ca. 1699– ca. 1718 and extant instruments themselves, some of which predate Gregory's time. It examines the structure and fate of the university observatory, the legacy of Gregory's teaching and endeavours, and the meridian line laid down in 1748 in the University Library.
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Lozitska, N. "Sunspot magnetic fields in 24 cycle of solar activity." Bulletin of Taras Shevchenko National University of Kyiv. Astronomy, no. 58 (2018): 11–17. http://dx.doi.org/10.17721/btsnua.2018.58.11-17.
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The data of visual measurements of the magnetic field in sunspots umbra, obtained in four observatories during 24 cycles of solar activity, are compared. Magnetic field strength modules with averaging over each observatory are analyzed. The measurements taken in the Astronomical Observatory of the University of Kyiv (KAO) were used as base, where 170 spots were measured on average 4 times each at intervals of one to two daysduring the group passing through the solar disk. Measurements of the Ural, Crimean and Mount Wilson Observatory, performed within 24 hours of observation in the KAO, are used in the study. It was found that the average value of the magnetic field per cycle, obtained from the data of three observatories UrAO, CrAO and KAO, was 26.0 ± 0.3, 25.0 ± 0.2 and 25.2 ± 0.2 cT, respectively. They differ by no more than 3 standard errors, while the Mount Wilson Observatory gives a significantly lower magnetic field – 23.8 ± 0.1 cT. This result is confirmed by the work of R. Rezaei et al., 2015, which compares the visual measurements in Mount Wilson with Tenerife Infrared Polarimeter (TIP) and Facility InfRared Spectropolarimeter (FIRS) for the 23rd and 24th cycle of solar activity. The average magnetic field value for observations of TIP and FIRS in 24 cycles is 26.0 cT, which is slightly higher than we obtained from the visual observations of three observatories, while MtW shows a few centitesla less. The mean square error of the average per cycle of the magnetic field, based on the data of TIP and FIRS is 0.2 cT, so the difference with the MtW is reliable. An understatement of the measured intensity of the magnetic field of the spots requires a revision of the measurement calibration in Mount Wilson. The data of the Crimean Astrophysical Observatory can be considered reference for subsequent comparisons with the results of observations of other observatories. For the calculation of the annual index Bsp of magnetic fields of sunspot size 22-44 Mm, the data of visual measurements of all 4 observatories are traditionally used. We have found that variations in the magnetic field of sunspots are the same as in previous cycles: the peak occurs in the second-third years after the maximum number of spots. The average for the 24 cycle Bsp index is 24.9 ± 0.3 сT, which allows us to consider this magnetic cycle as moderately strong. Reduction of the sunspots magnetic field in 2018 to 23 cT allows it to expect in 2019 the highest near-ground level of galactic cosmic rays in the last half century.
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Budding, E., S. C. Marsden, and O. B. Slee. "The Active Algol Binary KZ Pavonis." Publications of the Astronomical Society of Australia 18, no. 2 (2001): 140–47. http://dx.doi.org/10.1071/as01028.
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AbstractThe Algol type eclipsing binary KZ Pav has been observed over one complete orbit (0.95 days) with theAustraliaTelescope CompactArray. Contemporaneous optical photometric data from the University of Southern Queensland’s Observatory at Mount Kent were also collected and have been included in this multi-wavelength study.Preliminary indications are that the low levels of emission observed share similarities to those of some RS CVn binaries. The optical data show phase-linked effects which can be related to the mass transfer process of Algols. The possibility that the radio emission may be related to this process is considered.
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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." Symposium - International Astronomical Union 148 (1991): 381. http://dx.doi.org/10.1017/s0074180900200934.
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Late in 1988 the Mt John University Observatory acquired a cryogenic CCD system from Photometrics Ltd (Tucson). The chip is a Thomson CSF TH7882 CDA comprising 384 × 576 pixels. As part of the evaluation process, we have begun two differential photometry programs of the Magellanic Clouds using the Mt John 0.6m Boller & Chivens telescope. On this telescope each CCD pixel corresponds to 0.6 arcsec. Mt John's southerly latitude (44°S) permits year-round observations of the Clouds.The first program concerns B, V and I photometry of five blue eclipsing binaries selected, on the basis of Gaposchkin's (1970, 1977) photographic light curves, to have roughly equal components with minimal interaction. HV 12634 has also been observed for comparison with the CCD light curves published by Jensen et al. (1988). Fig. 1 shows the B observations so far obtained for HV 1761, but the reduction is preliminary, being based on aperture-integrated magnitudes. The field is populous, and a final reduction will require use of a crowded-field reduction package such as ROMAFOT.
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Wolf, George W., and Janet T. Kern. "Spectral classification of eclipsing binaries." Symposium - International Astronomical Union 118 (1986): 463–64. http://dx.doi.org/10.1017/s0074180900151940.
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Approximately 375 classification spectra of 130 Southern Hemisphere eclipsing binary stars were obtained between 1978 and 1982 at Mt. John University Observatory, New Zealand using the 0.6 meter reflector, and at Cerro Tololo Inter-American Observatory, Chile using the 0.4, 0.6, 0.9, and 1.0 meter telescopes. The spectra have been classified by one of us (GWW) using a grid of standards obtained on the various spectrographs at each of the observatories. Since many of the spectra were taken during primary and secondary minima, it has been possible in many cases to classify separately each component in the binaries.
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Carignan, Claude. "TWINNING between Institutions in developed and less developed countries: an ideal way to set-up an astrophysics program." Proceedings of the International Astronomical Union 10, H16 (August 2012): 542. http://dx.doi.org/10.1017/s1743921314012009.
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AbstractIt is very difficult to start from scratch a new Astrophysics program in a country with very little or no researchers in the field. In 2007, we began to set-up an Astrophysics program by TWINNING the Université de Ouagadougou with the Université de Montréal in Canada, the Université de Provence in France and the University of Cape Town in South Africa. Already, courses are given at the undergraduate and Master levels and a teaching Observatory has been built. A 1m research telescope was also moved from the La Silla Observatory in Chile to Burkina Faso and the infrastructure is being built at the moment on mount Djaogari in the north-eastern part of the country. In the meantime, 6 students are doing their PhD in Astrophysics overseas (Canada, France and South Africa) and will become the core of the research group at the Université de Ouagadougou. An engineer is also doing his PhD in Astronomical Instrumentation to help with the maintenance of the equipment on the Research Telescope.
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Endl, Michael, Christoph Bergmann, John Hearnshaw, Stuart I. Barnes, Robert A. Wittenmyer, David Ramm, Pam Kilmartin, Fraser Gunn, and Erik Brogt. "The Mt John University Observatory search for Earth-mass planets in the habitable zone of α Centauri." International Journal of Astrobiology 14, no. 2 (May 6, 2014): 305–12. http://dx.doi.org/10.1017/s1473550414000081.
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AbstractThe ‘holy grail’ in planet hunting is the detection of an Earth-analogue: a planet with similar mass as the Earth and an orbit inside the habitable zone. If we can find such an Earth-analogue around one of the stars in the immediate solar neighbourhood, we could potentially even study it in such great detail to address the question of its potential habitability. Several groups have focused their planet detection efforts on the nearest stars. Our team is currently performing an intensive observing campaign on the α Centauri system using the High Efficiency and Resolution Canterbury University Large Échelle Spectrograph (Hercules) at the 1 m McLellan telescope at Mt John University Observatory in New Zealand. The goal of our project is to obtain such a large number of radial velocity (RV) measurements with sufficiently high temporal sampling to become sensitive to signals of Earth-mass planets in the habitable zones of the two stars in this binary system. Over the past few years, we have collected more than 45 000 spectra for both stars combined. These data are currently processed by an advanced version of our RV reduction pipeline, which eliminates the effect of spectral cross-contamination. Here we present simulations of the expected detection sensitivity to low-mass planets in the habitable zone by the Hercules programme for various noise levels. We also discuss our expected sensitivity to the purported Earth-mass planet in a 3.24-day orbit announced by Dumusque et al. (2012).
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Pollard, K. R., E. Brunsden, P. L. Cottrell, M. Davie, A. Greenwood, D. J. Wright, and P. De Cat. "Mode identification from spectroscopy of gravity-mode pulsators." Proceedings of the International Astronomical Union 9, S301 (August 2013): 477–78. http://dx.doi.org/10.1017/s1743921313015135.
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AbstractThe gravity modes present in γ Doradus stars probe the deep stellar interiors and are thus of particular interest in asteroseismology. For the MUSICIAN programme at the University of Canterbury, we obtain extensive high-resolution echelle spectra of γ Dor stars from the Mt John University Observatory in New Zealand. We analyze these to obtain the pulsational frequencies and identify these with the multiple pulsational modes excited in the star. A summary of recent results from our spectroscopic mode-identification programme is given.
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Hearnshaw, John. "A new Starlight Reserve for the central South Island of New Zealand." Proceedings of the International Astronomical Union 10, H16 (August 2012): 736. http://dx.doi.org/10.1017/s1743921314013192.
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AbstractThe Aoraki Mackenzie International Dark Sky Reserve is a new reserve created in 2012 by the International Dark-Sky Association in the central South Island of New Zealand, and covers over 4300 square kilometres around Mt John University Observatory. It is the first such reserve to be recognized at gold tier level and is the largest dark sky reserve in the world. Astro-tourism in the new reserve will be a prominent activity in the coming years.
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Gies, Douglas R. "Taking the Measure of Massive Stars and their Environments with the CHARA Array Long-baseline Interferometer." Proceedings of the International Astronomical Union 12, S329 (November 2016): 156–60. http://dx.doi.org/10.1017/s1743921317002393.
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AbstractMost massive stars are so distant that their angular diameters are too small for direct resolution. However, the observational situation is now much more favorable, thanks to new opportunities available with optical/IR long-baseline interferometry. The Georgia State University Center for High Angular Resolution Astronomy Array at Mount Wilson Observatory is a six-telescope instrument with a maximum baseline of 330 meters, which is capable of resolving stellar disks with diameters as small as 0.2 milliarcsec. The distant stars are no longer out of range, and many kinds of investigations are possible. Here we summarize a number of studies involving angular diameter measurements and effective temperature estimates for OB stars, binary and multiple stars (including the σ Orionis system), and outflows in Luminous Blue Variables. An enlarged visitors program will begin in 2017 that will open many opportunities for new programs in high angular resolution astronomy.
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Özkardeş, Burcu, Derya Sürgit, Ahmet Erdem, Edwin Budding, Faruk Soydugan, and Osman Demircan. "Spectroscopic Study of the Early-Type Binary HX Vel A." Proceedings of the International Astronomical Union 7, S282 (July 2011): 67–68. http://dx.doi.org/10.1017/s1743921311026925.
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AbstractThis paper presents high resolution spectroscopy of the HX Vel (IDS 08390-4744 AB) multiple system. New spectroscopic observations of the system were made at Mt. John University Observatory in 2007 and 2008. Radial velocities of both components of HX Vel A were measured using gaussian fitting. The spectroscopic mass ratio of the close binary was determined as 0.599±0.052, according to a Keplerian orbital solution. The resulting orbital elements are a1sini=0.0098±0.0003 AU, a2sini=0.0164±0.0003 AU, M1sin3i=1.19±0.07 M⊙ and M2sin3i=0.71±0.04 M⊙.
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Airhart, Phyllis D. "Mount Allison University: A History, to 1963. 2 volumes. By John G. Reid. Toronto: University of Toronto Press, 1984. xi + 391 and 500 pp. $37.50 each." Church History 54, no. 3 (September 1985): 445. http://dx.doi.org/10.2307/3165738.
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Cottrell, P. L. "New Zealand Astronomy in the 1990s." Publications of the Astronomical Society of Australia 9, no. 1 (1991): 64–68. http://dx.doi.org/10.1017/s1323358000024917.
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AbstractThere has been a dramatic increase in astronomical research output in New Zealand over the last decade. This is set to increase with the advent of a number of new pieces of astronomical hardware over the last five years. These include the 1m telescope and associated instrumentation at Mount John and the JANZOS collaboration, with its instrumentation on Black Birch. Black Birch is also the site of the US Naval Observatory’s southern hemisphere astrometric station, where, using a transit circle instrument, they are collecting data which will form part of the International Reference Star Catalogue. As well as these ‘professional’ programs there is also a large network of amateur astronomers, who can provide extremely useful input into certain astronomical programs at the various observatories around the country and the world.A brief overview of the existing New Zealand astronomical scene will be followed by discussion of a number of new initiatives being proposed, which includes an automatic patrol telescope being developed by Carter Observatory, an expansion of the JANZOS collaboration and initial discussion about the possibility of an eastern arm for the Australia Telescope some where in New Zealand. In addition, for programs which require a long timebase of observations, extreme southerly latitudes or longitudinal coverage, New Zealand could provide a unique opportunity.
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Orchiston, Wayne. "From Amateur Astronomer to Observatory Director: The Curious Case of R. T. A. Innes." Publications of the Astronomical Society of Australia 18, no. 3 (2001): 317–27. http://dx.doi.org/10.1071/as01036.
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AbstractRobert Innes was one of a select band of amateur astronomers who made the transition to professional ranks towards the end of the nineteenth century. Initially he had a passion for mathematical astronomy, but after settling in Sydney he developed a taste for observational astronomy, specialising in the search for new double stars. He quickly became known for his success in this field and for his publications on solar system perturbations, and with John Tebbutt's patronage managed to secure a clerical position at the Royal Observatory, Cape of Good Hope. Once there he continued to observe in his spare time and to publish, and, with strong support from Sir David Gill, was appointed founding Director of the Transvaal Observatory. By the time he died in 1933, Innes had received an honorary D.Sc. from Leiden University, and had established an international reputation as a positional astronomer.This paper provides an interesting case study of a well-known ‘amateur-turned-professional’, and an example of the ways in which patronage played a key role in nineteenth and early twentieth century Australian and South African astronomy.
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Hearnshaw, John, Norman Rumsey, and Garry Nankivell. "Some comments on the design of échelle spectrographs using R2 or R4 gratings for precise radial-velocity measurements." International Astronomical Union Colloquium 170 (1999): 29–35. http://dx.doi.org/10.1017/s0252921100048302.
Full textAbstract:
AbstractA new fiber-fed échelle spectrograph (Hercules) is being designed for the 1-m telescope at Mt John University Observatory. The goals are to have a wavelength capability of 380 to 880 nm, covered in a single exposure on a 50-mm square CCD, to have a choice of resolving powers of 35000 or 70000 and to have no moving parts. High precision radialvelocity observations are a major but not the only goal. Designs with both R2 (blaze angle 63.4 deg) and R4 (blaze angle 76 deg) échelle gratings are being considered, in either case with a dimension of 408 mm perpendicular to the grooves.
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Bishop, Roy L. "The R.A.S.C. Observer’s Handbook." International Astronomical Union Colloquium 105 (1990): 225–26. http://dx.doi.org/10.1017/s0252921100086826.
Full textAbstract:
Except for two years, 1909 and 1910, the Observer’s Handbook of The Royal Astronomical Society of Canada has been published every year since 1907. It was founded by Clarence Augustus Chant, who also was responsible for the founding at the University of Toronto, of Canada’s first and largest department of astronomy, and who established the David Dunlap Observatory, which contains the largest optical telescope in Canada. In addition, Chant served as Editor of the Observer’s Handbook for 50 years, which is the main reason I am only the fourth editor since 1907. I should mention that John Percy, Chairman of the Scientific Organizing Committee of this Colloquium, was the third editor.
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Buxton, Michelle, Michael Bessell, and Bob Watson. "The MSSSO Wide Field CCD Hα Imaging Survey." Publications of the Astronomical Society of Australia 15, no. 1 (1998): 24–27. http://dx.doi.org/10.1071/as98024.
Full textAbstract:
AbstractA wide-field Hα survey of the Galactic Plane has been initiated by Mount Stromlo & Siding Spring Observatories in collaboration with the University of Sydney. The primary aim of the survey is to obtain images of the Galactic Plane in Hα and red continuum filters which will be compared with radio continuum images at 843 MHz from the Molonglo Observatory Synthesis Telescope (MOST). The secondary aim is to obtain images in [OIII] and [SII] to provide additional information on the nature of excitation in HII regions. Thirdly, additional images will be taken in B, V and I of interesting areas suitable for general publications as coloured reproductions. The images are taken with a 400 mm f/4·5 Nikkor-Q lens in conjunction with a 2K×2K SITe thinned CCD. The resolution is 12″ per pixel and the pixel size is 24 μm giving a 7°×7° field of view. Hα and red continuum observations are expected to be completed by the end of 1997. It is planned to make the results from the survey available on CD ROM and possibly video.
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West, John. "Climbing With Dr John West in the Rarefied Air of Pulmonary Research: From Mount Everest to the University of California, San Diego." Advances in Pulmonary Hypertension 4, no. 2 (May 1, 2005): 4–11. http://dx.doi.org/10.21693/1933-088x-4.2.4.
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Albrow, Michael, and P. L. Cottrel. "Asymmetry of metallic spectral lines in Cepheids." International Astronomical Union Colloquium 139 (1993): 375. http://dx.doi.org/10.1017/s0252921100117920.
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AbstractA program of high resolution spectroscopic observations of Cepheids has been carried out at Mt John University Observatory for several years. Radial velocities and asymmetries have been measured for selected metallic lines using the method of Wallerstein et al (1992).The line profiles show the largest asymmetry at phases of maximum inward velocity. The asymmetry at phases of maximum outward velocity is smaller and sometimes in the same direction as for the inward velocity maxima. Enhanced asymmetry is also noticed at phases where the bump appears on the radial velocity curve.To date our models are unable to predict such behaviour. It is important that a satisfactory explaination for these observations be found so that the accuracy of Baade-Wesselink radius solutions for such stars can be assessed.
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Flannery, Maura. "Naming a genus for William Darlington: a case study in botanical eponymy." Archives of Natural History 46, no. 1 (April 2019): 75–87. http://dx.doi.org/10.3366/anh.2019.0555.
Full textAbstract:
In 1853, the American botanist John Torrey described a new genus of pitcher plant, naming it Darlingtonia (Sarraceniaceae). The plant had been collected near Mount Shasta in California in 1841 by William Brackenridge, a member of the Wilkes Expedition. The name honoured William Darlington (1782–1863), a Pennsylvania physician and botanist who had traded information and specimens with Torrey for many years. Darlington considered a genus eponym as a distinct honour. The genus name Darlingtonia, however, had been used twice before, but the plants were shown to belong to Desmanthus (Leguminosae) and Styrax (Styracaceae). A letter in the William Darlington Herbarium at West Chester University, Pennsylvania, reveals Torrey's efforts to ease Darlington's fears that the same fate would befall the name of the Californian pitcher plant.
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Pollard, Karen R., E. Brunsden, M. Davie, A. Greenwood, and P. L. Cottrell. "Spectroscopic mode identification of γ Doradus stars: frequencies, modes, rotation and wave leakage." Proceedings of the International Astronomical Union 11, A29B (August 2015): 509–13. http://dx.doi.org/10.1017/s1743921316006001.
Full textAbstract:
AbstractThe gravity modes present in γ Doradus stars probe the deep stellar interiors and are thus of particular interest in asteroseismology. The MUSICIAN programme at the University of Canterbury has been successfully identifying frequencies and pulsation modes in many γ Doradus stars using hundreds of precise, high resolution spectroscopic observations obtained with the 1.0 m telescope and HERCULES spectrograph at the Mt John Observatory in New Zealand. In this paper we present a summary of our spectroscopic frequency and mode identifications. Of particular interest from our spectroscopic analyses are: the prevalence of (ℓ, m) = 1, 1 modes in many γ Dor stars; the importance of stellar rotation in the interpretation of the frequency and mode identification; and finally, possible evidence of wave leakage in one of these stars.
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Kneeshaw, Stephen, Richard Harvey, D'Ann Campbell, Robert W. Dubay, John T. Reilly, James F. Marran, Ann W. Ellis, et al. "Book Reviews." Teaching History: A Journal of Methods 10, no. 2 (May 4, 2020): 82–96. http://dx.doi.org/10.33043/th.10.2.82-96.
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Robert William Fogel and G. R. Elton. Which Road to the Past? Two Views of History. New Haven and London: Yale University Press, 1983. Pp. vii, 136. Cloth, $14.95. Review by Stephen Kneeshaw of The School of the Ozarks. Emmanuel LeRoy Ladurie. The Mind and Method of the Historian. Translated by Sian Reynolds and Ben Reynolds. Chicago: University of Chicago Press, 1981. Pp. v, 310. Paper, $9.95. Review by Richard Harvey of Ohio University. John E. O'Connor, ed. American History/ American Television: Interpreting the Video Past. New York: Frederick Ungar Publishing Company, 1983. Pp. 463. Cloth, $17.50; Paper, $8.95. Review by D' Ann Campbell of Indiana University. Foster Rhea Dulles & Melvyn Dubofsky. Labor in America: A History. Arlington Heights, Illinois: Harlan Davidson, Inc., 1984. 4th edition. Pp. ix, 425. Cloth, $25.95. Paper, $15.95. Review by Robert W. Dubay of Bainbridge Junior College. Karen Ordahl Kupperman. Roanoke: The Abandoned Colony. Totowa, New Jersey: Rowman & Allanheld, 1984. Pp. viii, 182. Cloth, $24.95; Paper, $12.50. Review by John T. Reilly of Mount Saint Mary College. Kevin O'Reilly. Critical Thinking in American History: Exploration to Constitution. South Hamilton, Massachusetts: Hamilton-Wenham Regional High School, 1983. Pp. 86. Paper, $2.95. Teacher's Guides: Pp. 180. Paper, $12.95; Kevin O'Reilly. Critical Thinking in American History: New Republic to Civil War. South Hamilton, Massachusetts: Hamilton-Wenham Regional High School, 1984. Pp. 106. Paper, $2.95. Teacher's Guide: Pp. 190. Paper, $12.95. Review by James F. Marran of New Trier Township High School, Winnetka, Illinois. Michael J. Cassity, ed. Chains of Fear: American Race Relations Since Reconstruction. Westport, Connecticut: Greenwood Press, 1984. Pp. xxxv, 253. Cloth, $35.00. Review by Ann W. Ellis of Kennesaw College. L. P. Morris. Eastern Europe Since 1945. London and Exeter, New Hampshire: Heinemann Educational Books, 1984. Pp. 211. Paper, $10.00. Review by Thomas T. Lewis, Mount Senario College. John Marks. Science and the Making of the Modern World. Portsmouth, New Hampshire: Heinemann Educational Books, Inc., 1983. Pp. xii, 507. Paper, $25.00. Review by Howard A. Barnes of Winston-Salem State University. Kenneth G. Alfers, Cecil Larry Pool, William F. Mugleston, eds. American's Second Century: Topical Readings, 1865-Present. Dubuque, Iowa: Kendall/ Hunt Publishing Co., 1984. Pp. viii, 381. Paper, $8.95. Review by Richard D. Schubart of Phillips Exeter Academy. Sam C. Sarkesian. America's Forgotten Wars: The Counterrevoltuionary Past and Lessons for the Future. Westport, Connecticut: Greenwood Press, 1984. Pp. xiv, 265. Cloth, $29.95. Review by Richard Selcer of Mountain View College. Edward Wagenknecht. Daughters of the Covenant: Portraits of Six Jewish Women. Amherst: University of Massachusetts, 1983. Pp. viii, 192. Cloth, $17.50. Review by Abraham D. Kriegel of Memphis State University. Morton Borden. Jews, Turks, and Infidels. Chapel Hill and London: University of North Carolina Press, 1984. Pp. x, 163. Cloth, $17.95. Review by Raymond J. Jirran of Thomas Nelson Community College. Richard Schlatter, ed. Recent Views on British History: Essays on Historical Writing Since 1966. New Brunswick: Rutgers University Press, 1984. Pp. xiii, 524. Cloth, $50.00. Review by Fred R. van Hartesveldt of Fort Valley State College. Simon Hornblower. The Greek World, 479-323 B.C. London and New York: Methuen, 1983. Pp. xi, 354. Cloth, $24.00; Paper, $11.95. Review by Dan Levinson of Thayer Academy, Braintree, Massachusetts. H. R. Kedward. Resistance in Vichy France. New York: Oxford University Press, 1978. Paper edition 1983. Pp. ix, 311. Paper, $13.95. Review by Sanford J. Gutman of the State University of New York at Cortland.
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Skuljan, J., J. B. Hearnshaw, and P. L. Cottrell. "Absolute Radial Velocities by Cross-Correlation with Synthetic Spectra." International Astronomical Union Colloquium 170 (1999): 91–97. http://dx.doi.org/10.1017/s0252921100048417.
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AbstractPrecise absolute radial velocities have been measured for several hundred late-type stars at Mt John University Observatory with the 1-m telescope, fiber-fed échelle spectrograph, and Thomson CCD. Six échelle orders in the green (5000−5600 Å) are used. Many delicate steps have been undertaken in order to maintain exactly the same conditions, both in recording and reducing the spectra, over a period of 18 months. A cross-correlation technique with theoretical spectra computed by R. L. Kurucz has been chosen to determine the absolute radial velocities. Blue sky spectra have been used to monitor systematic zero-point fluctuations from one observing run to another. An additional correlation between the measured velocities and average number of A/D units in the continuum has been discovered and used for fine adjustments, significantly improving the results. A random uncertainty of 10–20 ms−1 has been achieved for stellar spectra having intrinsically constant radial velocities.
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Pollard, Karen R., and P. L. Cottrell. "The Long-term Variation in the RV Tauri Star U Mon." International Astronomical Union Colloquium 155 (1995): 409–10. http://dx.doi.org/10.1017/s025292110003774x.
Full textAbstract:
The RV Tauri stars are semiregular pulsating variables located in the brightest part of the Cepheid II instability strip. They have a characteristic light curve of alternating deep and shallow minima. A subset of the RV Tauri stars (the RVb subclass) exhibit long-term (500 to 2600 day) light and radial velocity variations. Although it is well established that the short-term variations are due to pulsations, the long-term behaviour is not well understood.BVRI photometry and high-resolution spectra of U Mon (the brightest member of the RVb subclass) were obtained at the Mt John University Observatory (MJUO) between 1990 Aug and 1994 May. The light and colour curves obtained clearly show the long-term variation in U Mon (Fig. 1(a) and (b)). The reddest colours occur slightly later than the long-term minimum in the light curve. The short-term light and colour variations are ‘damped’ at the long-term minimum.
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Skuljan, Lj, P. L. Cottrell, A. C. Gilmore, and P. M. Kilmartin. "Photometry of R Coronae Borealis Stars during the Recovery Phase of their Declines." Publications of the Astronomical Society of Australia 20, no. 2 (2003): 159–64. http://dx.doi.org/10.1071/as02024.
Full textAbstract:
AbstractThe photometric observations (UBVRI) of nine cool R Coronae Borealis (RCB) stars have been collected at Mt John University Observatory, New Zealand, over a period of twelve years. The analysis of the magnitude–colour and colour–colour diagrams for the recovery phase demonstrates that all declines exhibit a similar asymptotic approach to their normal brightness. Declines return to maximum brightness along a line with essentially the same slope that does not depend on the star or the depth of the decline. Assuming a uniform obscuration of the photosphere by the dust cloud during the recovery phase, the extinction properties of the material were determined. The ratio of total to selective extinction (RV) for the RCB stars in our sample is in the range 2.5 to 4.6, indicating that the obscuring dust has extinction properties similar to that of the interstellar dust. Observations have been compared with the theoretical extinction curves for different sorts of grains.
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Skuljan, Jovan. "HRSP — A dedicated echelle reduction software package for Hercules." International Astronomical Union Colloquium 193 (2004): 575–78. http://dx.doi.org/10.1017/s0252921100011362.
Full textAbstract:
AbstractA collection of computer programs called the Hercules Reduction Software Package (HRSP) has been developed in the Department of Physics and Astronomy, University of Canterbury, for the data reduction of échelle spectra obtained with the Hercules spectrograph. The main goal in writing a dedicated software package for Hercules was to achieve a highly-optimized reduction process that would provide the basis of a pipeline reduction performed at the Mt John University Observatory. Since the spectrograph has no moving parts, the spectrum produced in the focal plane does not move or change, so that the same reduction procedure can be applied to all CCD images. An optimized routine written especially for Hercules is always much more efficient and reliable than any general-purpose software available. HRSP is written in C and the whole reduction procedure is performed on standard FITS files. A standard échelle reduction is applied, including the background and cosmic ray subtraction, order extraction, flat-fielding, normalization and wavelength rebinning. A special feature is the radial velocity determination by cross-correlation, which has been tested extensively over the past two years proving that Hercules is capable of delivering the high-precision radial velocities needed for detailed studying of binary stars, stellar pulsations, extra-solar planets and other related fields.
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Wittenmyer, Robert A., Michael Endl, Christoph Bergmann, John Hearnshaw, Stuart I. Barnes, and Duncan Wright. "A Campaign for the Detection of Earth-Mass Planets in the Habitable Zone of Alpha Centauri." Proceedings of the International Astronomical Union 8, S293 (August 2012): 58–64. http://dx.doi.org/10.1017/s1743921313012532.
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AbstractWe review the possible formation and orbital stability of Earth-mass or super Earth-mass planets around either of the stars Alpha Centauri A or B and describe a program at Mt John University Observatory using the Doppler method that aims to detect such planets. From New Zealand, we are able to observe the Alpha Centauri system year-round. This is critical in order to acquire data of sufficient quantity and phase coverage to detect the orbit of a terrestrial-mass planet in the habitable zone. Our observations are being made at high resolution (R = 70,000) and high signal-to-noise with the Hercules vacuum echelle spectrograph attached to the 1-m McLellan telescope by a 25-m long optical fibre and using an iodine cell. We discuss the velocity precision and instrumental stability required for success and outline the progress of the observations so far. At present we are collecting about 10,000 observations of each star, A and B, per year with a typical precision of 2.5 m/s per observation.
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Windover, Michael. "John Leroux and Thaddeus Holownia, A Vision in Wood & Stone: The Architecture of Mount Allison University, Kentville, NS: Gaspereau Press Ltd, 2016, 234 pp. $ 65.95 (hardcover) ISBN 9781554471409." RACAR : Revue d'art canadienne 44, no. 1 (2019): 121. http://dx.doi.org/10.7202/1062165ar.
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Hearnshaw, J. B., I. A. Bond, N. J. Rattenbury, S. Noda, M. Takeuti, F. Abe, B. S. Carter, et al. "Photometry of Pulsating Stars in the Magellanic Clouds as Observed in the MOA Project." International Astronomical Union Colloquium 176 (2000): 31–37. http://dx.doi.org/10.1017/s0252921100057018.
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AbstractA review of the MOA (Microlensing Observations in Astrophysics) project is presented. MOA is a collaboration of approximately 30 astronomers from New Zealand and Japan established with the aim of finding and detecting microlensing events towards the Magellanic Clouds and the Galactic bulge, which may be indicative of either dark matter or of planetary companions. The observing program commenced in 1995, using very wide band blue and red filters and a nine-chip mosaic CCD camera.As a by-product of these observations a large database of CCD photometry for 1.4 million stars towards both LMC and SMC has been established. In one preliminary analysis 576 bright variable stars were confirmed, nearly half of them being Cepheids. Another analysis has identified large numbers of blue variables, and 205 eclipsing binaries are included in this sample. In addition 351 red variables (AGB stars) have been found. Light curves have been obtained for all these stars. The observations are carried out on a 61-cm f/6.25 telescope at Mt John University Observatory where a new larger CCD camera was installed in 1998 July. From this latitude (44° S) the Magellanic Clouds can be monitored throughout the year.
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Webb, George E. "Allan Sandage. The Mount Wilson Observatory: Breaking the Code of Cosmic Evolution. (Centennial History of the Carnegie Institution of Washington, 1.) xiii + 647 pp., figs., apps., bibl., index. Cambridge: Cambridge University Press, 2004. $107.95 (cloth)." Isis 98, no. 1 (March 2007): 204–5. http://dx.doi.org/10.1086/519124.
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Georgievna, Popova. "The Serbian manuscripts of the lader of divine ascent of St. John Sinaites (14th c.)." Prilozi za knjizevnost, jezik, istoriju i folklor, no. 82 (2016): 19–36. http://dx.doi.org/10.2298/pkjif1682019g.
Full textAbstract:
The Ladder of Divine Ascent of St. John Sinaites has been very popular among the Slaves in the Middle Ages. From the 14th century 66 manuscripts were kept, 29 of them are Serbian. Not less than seven ancient manuscripts are kept in the National Library of Serbia (in the collections of the monasteries of Decani and Pec and in the New collection). Two manuscripts are kept in the library of the University of Belgrade, in the collection of manuscripts Lesnovo monastery. Five Serbian manuscripts of the Ladder are kept in the Russian National Library (St. Petersburg). Three ancient Serbian books of the Ladder are kept in Moscow, in the Russian State Library. Six ancient Serbian manuscripts of the Ladder are kept in the libraries of Mount Athos: four in the Hilandar monastery and two in the Zograf monastery. Four manuscripts of the Serbian Ladder are kept in Bucharest, in the Library of the Romanian Academy of Sciences. One ancient manuscript is kept in Macedonia, in the Ohrid National Museum. One Serbian book of the Ladder is kept in Paris, in the Slavic Fund of the French National Library. Of course, the former number of ancient Serbian manuscripts of the Ladder was much more than 29. The Serbian manuscripts preserved all ancient Slavonic translations of the Ladder: Preslav (in two versions), Tarnovo, Serbian (in two versions) and Athos. The author gives a description of each manuscript, names its location, dating and the related manuscripts. The Ladder as a book has many components. The basics of this book are the Life of St. John Sinaites and his message to John of Raif and 30 homilies. In the Slavic tradition we added a lot of new texts to this, not Greek but Slavic. One of these texts is the dictionary ?Tolkovanie recem?. According to our observations, this dictionary appeared in the Serbian book culture not later than the second half of the 14th century. The text of this dictionary began to appear separately from the Ladder very early as a part of the ascetic Sammelbands. An example is a Sammelband of the library of the Hilandar Monastery, number 455. The text of this dictionary is in the appendix of the article.
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Pooley, D. J., P. L. Cottrell, K. R. Pollard, and M. D. Albrow. "Spectroscopic and photometric monitoring of southern post-AGB stars." International Astronomical Union Colloquium 193 (2004): 353–56. http://dx.doi.org/10.1017/s0252921100010939.
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AbstractWe present the results of contemporaneous photometric and spectroscopic monitoring of 20 post-AGB stars from Mt John University Observatory. Photometric measures were carried out using Johnson BV and Cousins RI filters, and the radial velocity measurements were acquired using spectra from an echelle spectrograph. Our programme spanned five years and the stars covered a range of spectral types from B to K in order to investigate the behaviour of post-AGB stars as they evolve away from the AGB. A number of stars proved to be variable in ways incompatible with post-AGB models and are reclassified. Periodicities are presented for a number of stars. Photometrically, HD 70379 was found to be pulsating in two modes with periods of 85 and 97 d. The radial velocities also varied, with the peak amplitude occurring when the photometry was also changing most. AI CMi presented three different types of spectra associated with photometric brightness, with varying strengths of narrow emission lines and molecular bandheads. The Hα profiles in almost all of the stars show evidence of emission which varies on time scales of days to months. The Na D line profiles are generally complex showing between 4 and 7 components due to both circumstellar and interstellar material.
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Jones, Norman L., and Paul M. O’Byrne. "Respiratory Medicine at McMaster University, Hamilton, Ontario: 1968 to 2013." Canadian Respiratory Journal 21, no. 6 (2014): 325. http://dx.doi.org/10.1155/2014/860834.
Full textAbstract:
The medical school at McMaster University (Hamilton, Ontario) was conceived in 1965, and admitted the first class in 1969. John Evans became the founding Dean and he invited EJ Moran Campbell to be the first Chairman of the Department of Medicine. Moran Campbell, already a world figure in respiratory medicine and physiology, arrived at McMaster in September 1968, and he invited Norman Jones to be Coordinator of the Respiratory Programme.At that time, Hamilton had a population of 300,000, with two full-time respirologists, Robert Cornett at the Hamilton General Hospital and Michael Newhouse at St Joseph’s Hospital. From the clinical perspective, the aim of the Respiratory Programme was to develop a network approach to clinical problems among the five hospitals in the Hamilton region, with St Joseph’s Hospital serving as a regional referral centre, and each hospital developing its own focus: intensive care and burns units at the Hamilton General Hospital; cancer at the Henderson (later Juravinski) Hospital; tuberculosis and rehabilitation at the Chedoke Hospital; pediatrics and neonatal intensive care at the McMaster University Medical Centre; and community care at the Joseph Brant Hospital in Burlington. The network provided an ideal base for a specialty residency program. There was also the need to establish viable research.These objectives were achieved through collaboration, support of hospital administration, and recruitment of clinicians and faculty, mainly from our own trainees and research fellows. By the mid-1970s, the respiratory group numbered more than 25; outpatient clinic visits and research had grown beyond our initial expectations. The international impact of the group became reflected in the clinical and basic research endeavours.ASTHMA: Freddy Hargreave and Jerry Dolovich established methods to measure airway responsiveness to histamine and methacholine. Allergen inhalation was shown to increase airway responsiveness for several weeks, and the late response was shown to be an immunoglobulin E-mediated phenomenon. Paul O’Byrne and Gail Gauvreau showed that the prolonged allergen-induced responses were due to eosinophilic and basophilic airway inflammation and, with Judah Denburg, revealed upregulation of eosinophil/basophil progenitor production in bone marrow and airways. The Firestone Institute became the centre of studies identifying the inflammatory phenotype of patients with difficult-to-control asthma. Freddy Hargreave and others developed methods for sputum induction to identify persisting eosinophilic airway inflammation and documented its presence in the absence of asthma, and in patients with persistent cough. Parameswaran Nair has applied these techniques to the management of asthma in routine clinical practice. The Asthma Quality of Life Questionnaire and the Asthma Control Tests were developed by Liz Juniper and Gordon Guyatt. The first Canadian evidence-based clinical guidelines for asthma management in 1989 were coordinated by Freddy Hargreave, Jerry Dolovich and Michael Newhouse.DISTRIBUTION OF INHALED PARTICLES: Michael Newhouse and Myrna Dolovich used inhaled radiolabelled aerosols to study the distribution of inhaled particles and their clearance in normal subjects, smokers and patients with chronic obstructive pulmonary disease. They developed the aerochamber, and were the first to radiolabel therapeutic aerosols to distinguish the effects of peripheral versus central deposition. Particle deposition and clearance were shown to be impaired in ciliary dyskinesia and cystic fibrosis.DYSPNEA: Moran Campbell and Kieran Killian measured psychophysical estimates of the sense of effort in breathing in studies of loaded breathing and exercise to show that dyspnea increased as a power function of both duration and intensity of respiratory muscle contraction, and in relation to reductions in respiratory muscle strength. These principles also applied to dyspnea in cardiorespiratory disorders.EXERCISE CAPACITY: Norman Jones and Moran Campbell developed a system for noninvasive cardiopulmonary exercise testing using an incremental exercise test, and more complex studies with measurement of mixed venousPCO2by rebreathing. The 6 min walk test was validated by Gordon Guyatt. Kieran Killian and Norman Jones introduced routine muscle strength measurements in clinical testing and symptom assessment in exercise testing. Muscle strength training improved exercise capacity in older subjects and patients with chronic obstructive pulmonary disease.METABOLISM AND ACID-BASE CONTROL IN EXERCISE: After showing that imposed acidosis reduced, and alkalosis improved performance, Norman Jones, John Sutton and George Heigenhauser investigated the interactions between acid-base status and metabolism in exercise.HIGH-ALTITUDE MEDICINE: John Sutton and Peter Powles participated in high-altitude research on Mount Logan (Yukon), demonstrating sleep hypoxemia in acute mountain sickness and its reversal by acetazolamide, and participated in Operation Everest II.EPIDEMIOLOGY: David Pengelly and Tony Kerrigan followed children living in areas with differing air quality to show that lung development was adversely affected by pollution and maternal smoking. Malcolm Sears and Neil Johnstone showed that the ‘return to school’ asthma exacerbation epidemic was due mainly to rhinoviruses. David Muir investigated the effects of silica exposure in hard-rock miners, and mortality in the nickel industry.SUMMARY: The Respirology Division has grown to more than 50 physicians and PhD scientists, currently provides the busiest outpatient clinic in Hamilton, and has successful training and research programs.
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Jones, Norman L., and Paul M. O’Byrne. "Respiratory Medicine at McMaster University, Hamilton, Ontario: 1968 To 2013." Canadian Respiratory Journal 21, no. 6 (2014): e68-e74. http://dx.doi.org/10.1155/2014/285162.
Full textAbstract:
The medical school at McMaster University (Hamilton, Ontario) was conceived in 1965 and admitted the first class in 1969. John Evans became the founding Dean and he invited Moran Campbell to be the first Chairman of the Department of Medicine. Moran Campbell, already a world figure in respiratory medicine and physiology, arrived at McMaster in September 1968, and he invited Norman Jones to be Coordinator of the Respiratory Programme.At that time, Hamilton had a population of 300,000, with two full-time respirologists, Robert Cornett at the Hamilton General Hospital and Michael Newhouse at St Joseph’s Hospital. From the clinical perspective, the aim of the Respiratory Programme was to develop a network approach to clinical problems among the five hospitals in the Hamilton region, with St Joseph’s Hospital serving as a regional referral centre, and each hospital developing its own focus: intensive care and burns units at the Hamilton General Hospital; cancer at the Henderson (later Juravinski) Hospital; tuberculosis and rehabilitation at the Chedoke Hospital; pediatrics and neonatal intensive care at the McMaster University Medical Centre; and community care at the Joseph Brant Hospital in Burlington (Ontario). The network provided an ideal base for a specialty residency program. There was also the need to establish viable research.These objectives were achieved through collaboration, support of hospital administration, and recruitment of clinicians and faculty, mainly from our own trainees and research fellows. By the mid-1970s the respiratory group numbered more than 25; outpatient clinic visits and research had grown beyond our initial expectations. The international impact of the group became reflected in the clinical and basic research endeavours.ASTHMA: Freddy Hargreave and Jerry Dolovich established methods to measure airway responsiveness to histamine and methacholine. Allergen inhalation was shown to increase airway responsiveness for several weeks, and the late response was shown to be an immunoglobulin E-mediated phenomenon. Paul O’Byrne and Gail Gauvreau showed that the prolonged allergen-induced responses were due to eosinophilic and basophilic airway inflammation and, with Judah Denburg, revealed upregulation of eosinophil/basophil progenitor production in bone marrow and airways. The Firestone Institute became the centre of studies identifying the inflammatory pheno-type of patients with difficult-to-control asthma. Freddy Hargreave and others developed methods for sputum induction to identify persisting eosinophilic airway inflammation and documented its presence in the absence of asthma and in patients with persistent cough. Parameswaran Nair has applied these techniques to the management of asthma in routine clinical practice. The Asthma Quality of Life Questionnaire and the Asthma Control Tests were developed by Drs Liz Juniper and Gordon Guyatt. The first Canadian evidence-based clinical guidelines for asthma management in 1989 were coordinated by Freddy Hargreave, Jerry Dolovich and Michael Newhouse.DISTRIBUTION OF INHALED PARTICLES: Michael Newhouse and Myrna Dolovich used inhaled radiolabelled aerosols to study the distribution of inhaled particles and their clearance in normal subjects, smokers and patients with chronic obstructive pulmonary disease. They developed the aerochamber, and were the first to radiolabel therapeutic aerosols to distinguish the effects of peripheral versus central deposition. Particle deposition and clearance were shown to be impaired in ciliary dyskinesia and cystic fibrosis.DYSPNEA: Moran Campbell and Kieran Killian measured psychophysical estimates of the sense of effort in breathing in studies of loaded breathing and exercise to show that dyspnea increased as a power function of both duration and intensity of respiratory muscle contraction, and in relation to reductions in respiratory muscle strength. These principles also applied to dyspnea in cardiorespiratory disorders.EXERCISE CAPACITY: Norman Jones and Moran Campbell developed a system for noninvasive cardiopulmonary exercise testing using an incremental exercise test, and more complex studies with measurement of mixed venousPCO2by rebreathing. The 6 min walk test was validated by Gordon Guyatt. Kieran Killian and Norman Jones introduced routine muscle strength measurements in clinical testing and symptom assessment in exercise testing. Muscle strength training improved exercise capacity in older subjects and patients with chronic obstructive pulmonary disease.METABOLISM AND ACID-BASE CONTROL IN EXERCISE: After showing that imposed acidosis reduced, and alkalosis improved performance, Norman Jones, John Sutton and George Heigenhauser investigated the interactions between acid-base status and metabolism in exercise.HIGH-ALTITUDE MEDICINE: John Sutton and Peter Powles participated in high-altitude research on Mount Logan (Yukon), demonstrating sleep hypoxemia in acute mountain sickness and its reversal by acetazol-amide, and participated in Operation Everest II.EPIDEMIOLOGY: David Pengelly and Tony Kerrigan followed children living in areas with differing air quality to show that lung development was adversely affected by pollution and maternal smoking. Malcolm Sears and Neil Johnstone showed that the ‘return to school’ asthma exacerbation epidemic was due mainly to rhinoviruses. David Muir investigated the effects of silica exposure in hard-rock miners, and mortality in the nickel industry.SUMMARY: The Respirology Division has grown to more than 50 physicians and PhD scientists, and currently provides the busiest outpatient clinic in Hamilton, and has successful training and research programs.
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Martin, R. N., and J. W. M. Baars. "The Submillimeter Telescope - A Status Report." International Astronomical Union Colloquium 140 (1994): 66–67. http://dx.doi.org/10.1017/s0252921100019151.
Full textAbstract:
SummaryThe Max-Planck-Institut für Radioastronomie, Bonn and the Steward Observatory of the University of Arizona, Tucson are collaborating on the construction and operation of a dedicated submillimeter facility. The Submillimeter Telescope (SMT) is a 10 m diameter reflector surrounded by a corotating enclosure. The instrument is an alt-azimuth mounted f/13.8 Cassegrain homology telescope with two Nasmyth and bent Cassegrain foci. The SMT will have diffraction limited performance at a wavelength of 300 μm. and an operating overall figure accuracy of 15 μm rms. The primary and secondary reflector surfaces are constructed out of aluminum-core, carbon-fiber-reinforced-plastic (CFRP) face sheet sandwich panels. The primary reflector backup structure and secondary support are fabricated from CFRP structural members. This modern technology provides both the means for reaching the required precision of the SMT for both night and day operation (basically because of the low coefficient of thermal expansion and high strength-to-weight ratio of CFRP) and a potential route for the realization of lightweight telescopes of even greater accuracy in the future. The SMT will be the highest accuracy radio telescope ever built.The SMT is located at an altitude of 3180 m on Emerald Peak (Mt. Graham) 120 km northeast of Tucson in southern Arizona. Measurements indicate that atmospheric conditions allow submillimeter observations during about 40% of the time in winter months. The telescope is placed in a co-rotating enclosure of novel design. The enclosure fits tightly around the telescope, with the focus flanges extending from the elevation bearings into the receiver rooms of the enclosure. A flat tertiary mirror is used to direct the beam through either of the two elevation bearings. Thus, we are able to mount receivers directly on the telescope while maintaining laboratory type conditions in the access area surrounding the receivers. On the “facility instrument” side, several receivers can be operated simultaneously.