scholarly journals Measurement of Rose Indices on a Kiso 4-Degree Objective Prism Plate

1995 ◽  
Vol 148 ◽  
pp. 344-346
Author(s):  
S.-G. Lee
Keyword(s):  
Narrow Band ◽  
Structure Study ◽  
Galactic Structure ◽  
Spectral Indices ◽  
Structure Program ◽  
Interference Filters ◽  
Objective Prism ◽  
Low Dispersion

AbstractIn order to check the utilisation of 4-degree objective prism spectra for the deep spectroscopic galactic structure study, Rose’s (1984) seven indices between 3500 Å and 4400 Å for 19 Hyades stars were measured on a Kiso Schmidt prism plate, L3496. By comparison with those of Rose (1984), it is found that his spectral indices, Hδ/FeI, Hγ/P(4325), and P(3912)/P(CN) measured on these low dispersion spectra, are still usable. This result gives good prospects for a deep spectroscopic galactic structure program with the 4-degree objective prism and narrow band interference filters.

scholarly journals Contributions and Prospects for Spectral Classification of Stars with Objective Prism Techniques

1979 ◽  
Vol 47 ◽  
pp. 127-136
Author(s):  
E. K. Kharadze
Keyword(s):  
Galactic Structure ◽  
Spectral Classification ◽  
Missing Mass ◽  
Mass Problem ◽  
Important Stage ◽  
Objective Prism ◽  
Low Dispersion

The following topics will be discussed: a) A few historical comments; b) MK classification - the most important stage of classification work; c) Recently revealed peculiarity features and the problem of further differentiation of the classification scale; d) Classification work in the USSR; e) The role of classification results with respect to galactic structure studies; f) Low dispersion spectra and faint M-type stars and the missing mass problem; g) Extraterrestrial spectral observations: new promising means for research.

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).

scholarly journals A Survey of Planetary Nebulae in the SMC and M31

1989 ◽  
Vol 131 ◽  
pp. 351-351
Author(s):  
N. Meyssonnier ◽  
M. Azzopardi ◽  
J. Lequeux ◽  
R. Gathier
Keyword(s):  
Emission Line ◽  
Planetary Nebulae ◽  
Wide Field ◽  
Objective Prism ◽  
Low Dispersion ◽  
Selection Of ◽  
General Method

Our general method for finding planetary nebulae (PN) is to make wide field objective-prism or objective-grating low-dispersion spectra on photographic plates, PN stand up amongst other emission-line objects either as Hα + [N II] 6548-6583 A emitters or as [O III] 50007 A emitters with faint or no continuum, higher-resolution spectroscopy is used for confirming a selection of candidates.

scholarly journals The Muenster Redshift Project (MRSP)

1994 ◽  
Vol 161 ◽  
pp. 699-704
Author(s):  
P. Schuecker ◽  
W.C. Seitter ◽  
P. Boschan ◽  
R. Budell ◽  
B. Cunow ◽  
...  
Keyword(s):  
Low Resolution ◽  
Preliminary Results ◽  
Objective Prism ◽  
Low Dispersion

The Muenster Redshift Project provides to date 0.9 million low-resolution redshifts obtained from automatic reductions of pairs of direct and low-dispersion objective prism Schmidt plates. Preliminary results obtained from subsamples of the survey are described.

Laser-induced damage of Ta 2 O 5 /SiO 2 narrow-band interference filters under different 1064 nm Nd:YAG laser modes

2005 ◽  
Vol 250 (1-4) ◽  
pp. 195-202 ◽  
Author(s):  
Weidong Gao ◽  
Meiqiong Zhan ◽  
Shuhai Fan ◽  
Janda Shao ◽  
Zheng-Xiu Fan
Keyword(s):  
Nd:Yag Laser ◽  
Narrow Band ◽  
Interference Filters ◽  
Laser Modes ◽  
Laser Induced Damage

scholarly journals Multicolor Contrast Effects by Monochromatic Astronomic Filters – Utilization in Light Microscopy and Photomicrography

2008 ◽  
Vol 16 (5) ◽  
pp. 20-27 ◽  
Author(s):  
Jörg Piper
Keyword(s):  
Image Quality ◽  
Narrow Band ◽  
Light Pollution ◽  
Contrast Effects ◽  
Characteristic Radiation ◽  
Improve Image Quality ◽  
Interference Filters ◽  
Positive Effects ◽  
Spectral Components ◽  
Color Filters

Several color filters have been developed for astronomic use in order to improve image quality in visual observations and astronomic photography. Various positive effects, which can be achieved in astronomic practice, have already been described by several authors, manufacturers and distributors [2, 4, 5, 9, 10, 12]. Monochromatic narrow-band filters are widely used by astronomers. These filters are constructed as interference filters; they select small ranges within the spectrum of the visible light corresponding with characteristic radiation emitted by celestial nebula or the sun and its protuberances. This way, scattered terrestrial radiation caused by “light pollution” and non visible infrared or ultraviolet spectral components are blocked. Fundamental improvements of image quality will result from these filters when refractors or reflector telescopes are fitted with them.

scholarly journals The Frequency of Faint M Giant Stars at High Galactic Latitudes

1977 ◽  
Vol 4 (2) ◽  
pp. 35-36 ◽  
Author(s):  
N. Sanduleak
Keyword(s):  
Main Sequence ◽  
Galactic Plane ◽  
Absolute Magnitude ◽  
Main Sequence Stars ◽  
Giant Stars ◽  
The North ◽  
Objective Prism ◽  
M Stars ◽  
Low Dispersion ◽  
North Galactic

Based on the observations of M giant stars in the north galactic polar objective-prism survey of Upgren (1960) and the data summarized by Blanco (1965) the overall space density of all M-type giants as a function of distance from the galactic plane at the position of the sun can be approximated by,where z is in kpc and ρ(z) is the number of stars per 106 pc3. This relationship is derived from the observed fall-off in space densities up to a distance of about 2 kpc.The question arises as to the validity of extrapolation equation (1) to larger z distances so as to predict the number of faint M giants expected per unit area near the galactic poles. Adopting for the M giants a mean visual absolute magnitude of −1.0 (Blanco 1965), one finds that equation (1) predicts that less than one giant fainter than V~12 should be expected in a region of 200 square degrees. This expectation formed the hypothesis of a thesis study (Sanduleak 1965) in which it was assumed that the very faint M stars detected in a deep, infrared objective-prism survey at the NGP were main-sequence stars, since this could not be ascertained spectroscopically on the very low-dispersion plates used.

scholarly journals Automatic extraction and classification of low-dispersion objective prism stellar spectra

2000 ◽  
Vol 142 (2) ◽  
pp. 339-345 ◽  
Author(s):  
E. Bratsolis ◽  
I. Bellas-Velidis ◽  
A. Dapergolas ◽  
E. Kontizas ◽  
M. Kontizas
Keyword(s):  
Automatic Extraction ◽  
Stellar Spectra ◽  
Objective Prism ◽  
Low Dispersion
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