Application of Objective Prism Techniques in the Magellanic Clouds

1971 ◽  
pp. 181-183
Author(s):  
Jürgen Stock
Keyword(s):  
Magellanic Clouds ◽  
Objective Prism

Novae in the Magellanic Clouds

1979 ◽  
Vol 46 ◽  
pp. 96-101
Author(s):  
J.A. Graham
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
University Of Michigan ◽  
The Past ◽  
Spectroscopic Information ◽  
Objective Prism ◽  
The University ◽  
Small Cloud ◽  
Low Dispersion

During the past several years, a systematic search for novae in the Magellanic Clouds has been carried out at Cerro Tololo Inter-American Observatory. The Curtis Schmidt telescope, on loan to CTIO from the University of Michigan is used to obtain plates every two weeks during the observing season. An objective prism is used on the telescope. This provides additional low-dispersion spectroscopic information when a nova is discovered. The plates cover an area of 5°x5°. One plate is sufficient to cover the Small Magellanic Cloud and four are taken of the Large Magellanic Cloud with an overlap so that the central bar is included on each plate. The methods used in the search have been described by Graham and Araya (1971). In the CTIO survey, 8 novae have been discovered in the Large Cloud but none in the Small Cloud. The survey was not carried out in 1974 or 1976. During 1974, one nova was discovered in the Small Cloud by MacConnell and Sanduleak (1974).

Coravel Radial Velocities of Supergiants in the Small Magellanic Cloud

1984 ◽  
Vol 88 ◽  
pp. 265-268
Author(s):  
E. Maurice ◽  
N. Martin ◽  
L. Prévot ◽  
E. Rebeirot
Keyword(s):  
South Africa ◽  
Velocity Field ◽  
Planetary Nebulae ◽  
Hii Regions ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
Radial Velocities ◽  
Small Magellanic Cloud ◽  
Objective Prism

Kinematical studies of the Magellanic Clouds began more than half a century ago, when Wilson, in 1918, first interpreted the gradient of the 17 radial velocities of gazeous nebulae in the Large Cloud in terms of rotation. In the case of the Small Magellanic Cloud, the first real attempt to understand the velocity field of this galaxy was performed by the Radcliffe astronomers (Feast et al., 1960, 1961). Their study was based on radial velocities of 40 stars and 13 HII regions.With the installation by ESO of an objective-prisme astrograph in South Africa, in 1961, and then of several larger telescopes in Chile in 1968, the number of measurements significantly increased for Magellanic objects, in particular in the SMC. In this galaxy, the objective-prism observations resulted in about 100 stellar radial velocities (Florsch, 1972a) of probable members. A compilation by Maurice (1979) of all then known slit-spectrograph radial velocities gave velocities for 80 supergiants, 35 HII regions and 12 planetary nebulae.

scholarly journals Lists of Confirmed Planetary Nebulae in the Magellanic Clouds

1978 ◽  
Vol 76 ◽  
pp. 64-64
Author(s):  
N. Sanduleak ◽  
D.J. MacConnell ◽  
A.G. Davis Philip
Keyword(s):  
Emission Line ◽  
Total Mass ◽  
Planetary Nebulae ◽  
High Sensitivity ◽  
Hii Regions ◽  
Magellanic Clouds ◽  
Schmidt Telescope ◽  
Deep Blue ◽  
Two Systems ◽  
Objective Prism

Very deep, blue and red-sensitive objective-prism plates, taken with the Curtis Schmidt telescope at the Cerro Tololo Inter-American Observatory, were used to survey both Magellanic Clouds for unresolved objects which could be classified as highly probable planetary nebulae. The high sensitivity of the baked Kodak IIIa-J emulsion at 5000 Å made it possible to detect the N1 and N2 lines of [OIII] in fainter objects than previously observed. A number of emission-line stars, compact HII regions, and very-low-excitation objects, formerly considered to be probable or possible planetaries, were recognized and excluded. The final lists contain 27 confirmed planetaries in the SMC and 100 in the LMC, a ratio equivalent to the estimated ratio of total mass in the two systems. As would be expected, most of these objects had been detected in previous objective-prism surveys but some apparently new planetaries were found.

Photoelectric spectrophotometry of emission nebulosities in the Magellanic Clouds

1964 ◽  
Vol 20 ◽  
pp. 294-310 ◽  
Author(s):  
H. R. Dickel ◽  
L. H. Aller ◽  
D. J. Faulkner
Keyword(s):  
Wavelength Range ◽  
Magellanic Clouds ◽  
Cross Sectional ◽  
Objective Prism ◽  
Photometric Measurements

Photometric measurements of the emission nebulosities in the LMC are not numerous. Doherty, Henize, and Aller (1956) microphotometered both widened and unwidened objective-prism photographs covering a narrow wavelength range near Hα to obtain cross-sectional “intensity profiles” for certain nebulosities in the Large Cloud. These intensities were converted to surface brightnesses by tracing the widened spectra of stars of known magnitude and colour and using the method of Ambartsumian (1933). Peak intensities for each scan across a nebulosity are given in erg cm–2 sec–1 steradian–1.

scholarly journals Wolf-Rayet stars in the Magellanic Clouds

1979 ◽  
Vol 83 ◽  
pp. 51-54
Author(s):  
J. Breysacher ◽  
M. Azzopardi
Keyword(s):  
Magellanic Clouds ◽  
Systematic Search ◽  
Objective Prism

Up to now 4 WR stars were known in the SMC (Breysacher and Westerlund, 1978) and 76 in the LMC (Fehrenbach et al., 1976). Because no systematic search for WR stars in the SMC had ever been made, a survey was carried out with the ESO Objective Prism Astrograph which resulted in the identification of 4 new WR stars of the WN type, afterwards confirmed by slit spectroscopy. In the LMC, two fields were also observed and 13 new faint WR stars detected. The results presented here mainly concern the SMC WR stars.

scholarly journals A New Objective Prism Catalogue of OB and Supergiant B, A, F and G Stars in the Magellanic Clouds

1979 ◽  
Vol 47 ◽  
pp. 155-157
Author(s):  
A. G. Davis Philip ◽  
N. Sanduleak
Keyword(s):  
Magellanic Clouds ◽  
Schmidt Telescope ◽  
Ob Stars ◽  
Objective Prism ◽  
Hydrogen Lines

The Michigan Curtis Schmidt telescope at Cerro Tololo Inter-American Observatory has been used with the “thin” prism (Blanco 1974) to survey the Large and Small Magellanic Clouds. Four plates, covering approximately 90 square degrees, and three plates, covering approximately 70 square degrees, were taken of the Large and Small Magellanic Clouds respectively. One hour exposures on nitrogen baked, IIIa-J plates were obtained. The limiting magnitude of the plates is V = 16 mag. At the dispersion of 1360 Å/mm OB stars can be recognized by their long uv extension, in which no sign of a Balmer discontinuity can be seen. The supergiants can be recognized by the appearance of a Balmer discontinuity and classified into temperature types by the strength of the hydrogen lines.

Spectrophotometric measurements of objective-prism spectra

1966 ◽  
Vol 24 ◽  
pp. 118-119
Author(s):  
Th. Schmidt-Kaler
Keyword(s):  
Progress Report ◽  
Two Dimensional ◽  
Objective Prism ◽  
Made In

I should like to give you a very condensed progress report on some spectrophotometric measurements of objective-prism spectra made in collaboration with H. Leicher at Bonn. The procedure used is almost completely automatic. The measurements are made with the help of a semi-automatic fully digitized registering microphotometer constructed by Hög-Hamburg. The reductions are carried out with the aid of a number of interconnected programmes written for the computer IBM 7090, beginning with the output of the photometer in the form of punched cards and ending with the printing-out of the final two-dimensional classifications.

Some problems of objective-prism spectra classification

1966 ◽  
Vol 24 ◽  
pp. 51-52
Author(s):  
E. K. Kharadze ◽  
R. A. Bartaya
Keyword(s):  
Short Wave ◽  
High Quality ◽  
Stellar Spectra ◽  
Objective Prism

The unique 70-cm meniscus-type telescope of the Abastumani Astrophysical Observatory supplied with two objective prisms and the seeing conditions characteristic at Mount Kanobili (Abastumani) permit us to obtain stellar spectra of a high quality. No additional design to improve the “climate” immediately around the telescope itself is being applied. The dispersions and photographic magnitude limits are 160 and 660Å/mm, and 12–13, respectively. The short-wave end of spectra reaches 3500–3400Å.

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