9. Instruments and Techniques

1985 ◽  
Vol 19 (1) ◽  
pp. 41-56
Author(s):  
W. C. Livingston ◽  
C. M. Humphries ◽  
J. C. Bhattacharyya ◽  
J. Davis ◽  
J. L. Heudier ◽  
...  
Keyword(s):  
Imperial College ◽  
Advanced Technology ◽  
New Delhi ◽  
List Type ◽  
Academic Press ◽  
Royal Observatory ◽  
Instruments And Techniques ◽  
Large Telescopes ◽  
Optical Telescopes

Between the Patras and New Delhi General Assemblies no meetings were directly sponsored by Commission 9 because the discipline was amply covered by the following: - “Eighth Symposium on Photoelectronic Image Devices,” Imperial College (London) 5-7 September 1983 (B. L. Morgan, Ed., Academic Press, London, 1984).- “Advanced Technology Optical Telescopes II” Imperial College, 5-7 September 1983.- “Instrumentation in Astronomy V” 7-9 September 1983 (A. Boksenberg and D. Crawford, Eds., Proc. SPIE 415).- IAU Symposium No. 109: “Astrometric Techniques,” 9-12 January 1984, Gainsville (Florida).- “Astronomical Photography 1984,” Edinburgh, 4-6 April 1984 (E. Sim and K. Ishida, Eds., Number 14 of Occasional Reports of the Royal Observatory, Edinburgh).- “IAU Colloquium No. 79: “Very Large Telescopes, Their Instrumentation and Programs,” Garching bei München, 9-12 April 1984 (M. H. Ulrich and K. Kjär, Eds.)

Measuring cosmic magnetic fields with very large telescopes

2008 ◽  
Vol 4 (S259) ◽  
pp. 653-662 ◽  
Author(s):  
Oleg Kochukhov ◽  
Nicolai Piskunov
Keyword(s):  
High Resolution ◽  
Magnetic Fields ◽  
Medium Size ◽  
General Properties ◽  
The Future ◽  
Large Telescopes ◽  
New Generation ◽  
Optical Telescopes

AbstractWe review general properties and capabilities of the instrumentation employed to diagnose cosmic magnetic fields using medium-size and large optical telescopes. During the last decade these spectropolarimeters and high-resolution spectrographs have been successfully used to detect and characterize magnetic fields in stars across the H-R diagram. A new generation of high-resolution spectropolarimeters will benefit from the large collecting area of the future E-ELT and currently operating 8-m class telescopes. We review plans to develop spectropolarimeters for these very large telescopes and outline a number of science cases where new spectropolarimetric instrumentation is expected to play a key role.

scholarly journals Paper Productivity of Ground-based Large Optical Telescopes from 2000 to 2009

2011 ◽  
Vol 28 (3) ◽  
pp. 249-260 ◽  
Author(s):  
Sang Chul Kim
Keyword(s):  
Scientific Publication ◽  
Publication Trends ◽  
Publication Data ◽  
Large Telescopes ◽  
Optical Telescopes ◽  
Infrared Telescopes

AbstractWe present an analysis of the scientific (refereed) paper productivity of the current largest (diameter > 8m) ground-based optical (and infrared) telescopes during the ten-year period from 2000 to 2009. The telescopes for which we have gathered and analysed the scientific publication data are the two 10-m Keck telescopes, the four 8.2-m Very Large Telescopes (VLT), the two 8.1-m Gemini telescopes, the 8.2-m Subaru telescope, and the 9.2-m Hobby–Eberly Telescope (HET). We have analysed the numbers of papers published in various astronomical journals produced by using these telescopes. While the total numbers of papers from these observatories are largest for the VLT, followed by Keck, Gemini, Subaru, and HET, the number of papers produced by each component of the telescopes is largest for Keck, followed by VLT, Subaru, Gemini, and HET. In 2009, each telescope of the Keck, VLT, Gemini, Subaru, and HET observatories produced 135, 109, 93, 107, and 5 refereed papers, respectively. We have shown that each telescope of the Keck, VLT, Gemini, and Subaru observatories is producing 2.1 ± 0.9 Nature and Science papers annually and these papers make up 1.7 ± 0.8% of all refereed papers produced by using each of those telescopes. Extending this relation, we propose that this ratio of the number of Nature and Science papers to the total number of refereed papers that will be produced by future extremely large telescopes (ELTs) will remain similar. From a comparison of the publication trends of the above telescopes, we suggest that (i) having more than one telescope of the same kind at the same location and (ii) increasing the number of instruments available at the telescope are good ways to maximize the paper productivity.

scholarly journals Astronomy from Antarctica

2005 ◽  
Vol 17 (4) ◽  
pp. 555-560 ◽  
Author(s):  
J.W.V. STOREY
Keyword(s):  
Absolute Humidity ◽  
Far Infrared ◽  
Antarctic Plateau ◽  
Earth Like Planets ◽  
Remote Sites ◽  
Large Telescopes ◽  
New Generation ◽  
The Antarctic ◽  
City Centres ◽  
Optical Telescopes

Astronomers have always sought the very best locations for their telescopes. From observatories in city centres, astronomers moved first to nearby mountain tops, then to remote sites in distant countries, to aircraft, and into space. In the past decade we have come to realize that the best astronomical observing conditions on the surface of the earth are to be found on the Antarctic plateau. The combination of high altitude, low temperature, low absolute humidity, low wind and extremely stable atmosphere offers astronomers gains in sensitivity and measurement precision that can exceed two orders of magnitude over even the best temperate sites. In addition, spectral windows are opened up – particularly in the far-infrared and terahertz regions – that are otherwise only accessible from high-flying aircraft or from space. Established and highly successful telescopes at the South Pole are soon to be joined by a new generation of facilities at Concordia Station, including large telescopes and interferometers. It has even been suggested that the largest optical telescopes currently proposed, with diameters of up to 100 m, might achieve their science goals at a lower overall cost if they are built on the Antarctic plateau rather than at a temperate site. Such telescopes offer the possibility of not only detecting earth-like planets in other star systems, but also of analysing their atmospheres spectroscopically.

Three-dimensional confocal microscopy in living cells: historical development, practical application and limitations

1992 ◽  
Vol 50 (2) ◽  
pp. 1120-1121
Author(s):  
Barry R. Masters
Keyword(s):  
New York ◽  
Confocal Microscopy ◽  
Optical Microscopy ◽  
Cell Biology ◽  
Living Cells ◽  
Theory And Practice ◽  
List Type ◽  
Academic Press

Confocal microscopy is a rapidly evolving technique which is solving problems in the biological and material sciences. This tutorial focuses on the confocal microscopy of living cells. Both in vivo and in vitro applications of confocal microscopy will be reviewed. Applications of confocal microscopy of the eye will illustrate the concepts. Fluorescence and back scattered confocal microscopy are critically reviewed. A bibliography on confocal microscopy is given to aid the users of this technique.Books (Optical Theory, Image Formation, Fluorescence Techniques) •Theory and Practice of Scanning Optical Microscopy, (eds. T. Wilson, C. Sheppard), Academic Press, London, 1984.•Confocal Microscopy, (ed. by T. Wilson), Academic Press, London, 1990.•Handbook of Biological Confocal Microscopy, (ed. J.B. Pawley), Plenum Press, New York, 1989.•New Techniques of Optical Microscopy and Microspectroscopy (ed. R.J. Cherry), CRC Press, Inc., Boca Raton, Florida, 1991.•Noninvasive Techniques in Cell Biology, (eds. J.K. Foskett, S. Grinstein), Wiley-Liss, New York, 1990.

scholarly journals Optical pulsars and polarimetry

2017 ◽  
Vol 13 (S337) ◽  
pp. 191-194 ◽  
Author(s):  
Andrew Shearer ◽  
Eoin O’ Connor
Keyword(s):  
Gamma Ray ◽  
Optical Observations ◽  
Crab Pulsar ◽  
Optical Detectors ◽  
X Ray ◽  
First Order ◽  
Near Ir ◽  
Large Telescopes ◽  
Optical Telescopes ◽  
Polarisation Measurements

AbstractDespite the early optical detection of the Crab pulsar in 1969, optical pulsars have become the poor cousin of the neutron star family. Only five normal pulsars have been observed to pulse in the optical waveband. A further three magnetars/SGRs have been detected in the optical/near IR. Optical pulsars are intrinsically faint with a first order luminosity, predicted by Pacini, to be proportional to P−10, where P is the pulsar’s period. Consequently they require both large telescopes, generally over-subscribed, and long exposure times, generally difficult to get. However optical observations have the benefit that polarisation and spectral observations are possible compared to X-ray and gamma-ray observations where polarisation measurements are limited. Over the next decade the number of optical pulsars should increase as optical detectors approach 100% quantum efficiency and as we move into the era of extremely large telescopes where limiting fluxes will be 30 to 100 times fainter compared to existing optical telescopes.

Survey for Duplicity Frequencies: Status and Prospects

1992 ◽  
Vol 135 ◽  
pp. 266-272
Author(s):  
Paul Couteau
Keyword(s):  
Stellar Evolution ◽  
List Type ◽  
Type Number ◽  
Complete Set ◽  
The Mean ◽  
Large Telescopes

I.We recall the main surveys: J. Herschel (1826), W. Struve (1825), A.W. Burnham and G.W. Hough (1880), R.G. Aitken and W.J. Hussey (1910), R. Jonckeere and T.E. Espin (1910), W.H. van den Bos (1925), R.A. Rossiter (1950). Presently the classical surveys are continuing with P. Muller, W.D. Heintz, and P. Couteau. The interferometric survey with large telescopes is carried out at CHARA.II.The results of old surveys, up to 1950, amount to 700 known orbits out of more than 35000 found binaries. The new surveys since 1965, both visual and interferometric, had checked 4000 new binaries giving already about 30 orbits. The periods are shorter and shorter: the mean period is 200 years for Struve (1825) binaries, 75 years for Aitken’s (1910), 25 years for Couteau and Muller’s (1970), and 7 years for CHARA’s. The number of known orbits increases exponentially with time.III.The “classical” surveys will have to be performed again within fifty years with refractors.The interferometric and aperture syntheses surveys will be able to observe every binary, even those in contact with each other. With HIPPARCOS’ results, astronomers will dispose of a complete set of data for new theories of stellar evolution.

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