A photometric and spectrophotometric investigation of the central parts of the Norma Cloud

1966 ◽  
Vol 24 ◽  
pp. 338-339
Author(s):  
J. M. Ramberg
Keyword(s):  
Spectrophotometric Investigation ◽  
Photometric System ◽  
Plate Material ◽  
Objective Prism ◽  
Colour Indices

The author has for some time at the Stockholm Observatory been occupied in a photometric and spectrophotometric investigation of the central parts of the Norma Cloud of stars (α = 16h19m5, δ = −52°). The plate material has been collected at the Boyden Observatory: the spectral plates have been secured with the ADH telescope combined with objective prism, the photometric plates with the ADH and the 10-inch Metcalf telescopes. The photographic magnitudes and the colour indices are referred to the photometric system of the E-regions, as established by the Cape Observatory.

scholarly journals A More Complete Listing of LMC Planetary Nebulae

1984 ◽  
Vol 108 ◽  
pp. 231-232
Author(s):  
N. Sanduleak
Keyword(s):  
Planetary Nebula ◽  
Planetary Nebulae ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Plate Material ◽  
Schmidt Telescope ◽  
Complete Listing ◽  
Objective Prism

In an earlier paper by Sanduleak et al. (1978) a listing was given of 102 confirmed and probable planetary nebulae in the Large Magellanic Cloud detected on objective-prism plates taken with the Curtis Schmidt telescope at Cerro Tololo. Subsequently, deeper coverage was obtained on nitrogen-baked Kodak IIIa-J plates plus GG 455 filter exposed for 90 minutes. The thin prism was again used to provide a dispersion of about 1500 Å mm−1 at Hβ and the spectra were unwidened. An additional 25 planetary nebula candidates were found on this new plate material to show the requisite characteristics, i.e. they display (a) a stellar appearance, (b) [OIII] λλ5007, 4959 strongly in emission, and (c) no evidence of a continuum.

scholarly journals Astrometric and photometric observations of six brightest trans-Neptunian objects at the Kyiv comet station

2020 ◽  
Vol 10 (2) ◽  
pp. 48-54
Author(s):  
A. Baransky ◽  
O. Lukina ◽  
S. Borysenko
Keyword(s):  
Ccd Camera ◽  
Photometric System ◽  
Photometric Observations ◽  
Absolute Magnitudes ◽  
Colour Indices

In this work we focused on observations of six trans-Neptunian objects (TNOs) whose apparent magnitudes are brighter than 20m. We present the results of astrometric and photometric observations of (134340) Pluto, (136108) Haumea, (136472) Makemake, (136199) Eris, (90482) Orcus, and (20000) Varuna obtained at the Kyiv comet station (Code MPC 585) in 2017-2019. For observations we used the 0.7-m (f/4) reflector AZT-8 with FLI PL4710 CCD camera and filters of Johnson-Cousins photometric system. From our images we measured the objects' astrometric positions, calculated apparent magnitudes in the BVRI (mostly R) bands using aperture photometry method, and found absolute magnitudes together with the colour indices in several bands. Analysing our results, we investigate the limitation on the astrometry and photometry of faint objects with the 0.7-m telescope.

45. Spectral Classifications and Multi-Band Colour Indices

1973 ◽  
Vol 15 (1) ◽  
pp. 697-716 ◽  
Author(s):  
B. E. Westerlund
Keyword(s):  
Spectral Lines ◽  
General Tendency ◽  
Spectral Classification ◽  
Visual Classification ◽  
The Past ◽  
Objective Prism ◽  
Colour Indices ◽  
Multi Band

During the past three years there has been much activity in the field of spectral classification by photographic and photoelectric techniques. The general tendency of the spectral classification has been one of refinement of the criteria applied in visual classification, the more frequent appearance of criteria based on equivalent widths measured in higher-dispersion spectra and the use of narrowband photometry on individual often rather weak spectral lines. In the area of objective prism classification important extensive programmes are under way at many observatories. Here, the increased interest in and importance of automation of data available on spectral plates is perhaps most obvious.

Objective-prism techniques in use by the Vatican Schmidt

1966 ◽  
Vol 24 ◽  
pp. 59-66
Author(s):  
M. F. McCarthy ◽  
P. J. Treanor ◽  
F. C. Bertiau
Keyword(s):  
Main Sequence ◽  
Variable Stars ◽  
Plate Material ◽  
Main Sequence Stars ◽  
The Past ◽  
Objective Prism

For the past 2 years during which the Vatican Schmidt camera (1) has been in regular operation a large proportion of the plate material has been obtained with one of three large objective prisms (2°5, 4°0 and 8°0); more recently the combination 12° (4° + 8°) prism has been found to be a most effective tool for classification studies (2) for the detection and measurement of the 4430Å interstellar band (3), for investigations of variable stars and for examining differences noted in the 3890Å region in spectra or G8 main-sequence stars.

scholarly journals Passbands and Photometric Systems

1986 ◽  
Vol 7 ◽  
pp. 813-817
Author(s):  
F. Rufener
Keyword(s):  
The Other ◽  
Systematic Evaluation ◽  
Evaluation Procedure ◽  
Photometric System ◽  
Other Hand ◽  
The One ◽  
Colour Indices

AbstractSynthetic photometry must be used to accurately define the passbands which characterize a photometric system. On the one hand, the colour indices of the stars must be coherent with their absolute spectrophotometry; on the other hand, direct comparisons of model atmospheres with observations must be carried out without resorting to arbitrary transformations. A systematic evaluation procedure could be applied to various photometric systems.

scholarly journals Seyfert 1 Galaxies in Calan–Tololo Survey

1989 ◽  
Vol 134 ◽  
pp. 35-36
Author(s):  
José Maza ◽  
María Teresa Ruiz
Keyword(s):  
Emission Line ◽  
Plate Material ◽  
Objective Prism ◽  
Original Survey ◽  
Plate Collection

Four years ago we started at Cerro Calán an extension of the objective prism survey carried out at Cerro Tololo Inter-American Observatory (CTIO) by Malcolm Smith a decade ago (Smith 1975, Smith, Aguirre and Zemelman 1976). Thanks to the kindness of Dr. P.S. Osmer, then Director of CTIO, we got on loan Smith's original plate collection. Searching his plate material we learned to recognize the most prominent emission line objects. We decided then to extend Tololo's original survey to an area of the southern sky large enough to be of statistical interest but small enough so it could be carried through with our very limited facilities at Cerro Calán.

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.

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).

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