scholarly journals BVRI photometric calibration of the Nedeljkovic telescope

2021 ◽  
pp. 3-3
Author(s):  
A. Vudragovic ◽  
M. Jurkovic
Keyword(s):  
Ccd Camera ◽  
Color Correction ◽  
Photometric Calibration ◽  
Astronomical Station

We have done photometric calibration of the 60 cm Nedeljkovic telescope equipped with the FLI PL 230 CCD camera, mounted at the Astronomical Station Vidojevica (Serbia), using standard stars from the Landolt catalog. We have imaged 31 fields of standard stars using Johnson's BVRI filters during three nights in August 2019. We have measured both extinction and color correction. Relating our calibrated magnitudes to the magnitudes of standard stars from the Landolt catalog, we have achieved accuracy of 2%-5% for the BVRI magnitudes.

scholarly journals Focal length determination for the 60cm telescope at Astronomical station Vidojevica

2012 ◽  
pp. 97-104 ◽  
Author(s):  
Z. Cvetkovic ◽  
G. Damljanovic ◽  
R. Pavlovic ◽  
O. Vince ◽  
I.S. Milic ◽  
...  
Keyword(s):  
Focal Length ◽  
Ccd Camera ◽  
Angular Separation ◽  
Multiple Stars ◽  
Relative Coordinates ◽  
Double And Multiple Stars ◽  
Positional Angle ◽  
Length Determination ◽  
Optical Wavelengths ◽  
Astronomical Station

The focal length of a telescope is an important parameter in determining the angular pixel size. This parameter is used for the purpose of determining the relative coordinates (angular separation and positional angle) of double and multiple stars, and the precise coordinates of extragalactic radio sources (ERS) that are visible at optical wavelengths. At the Astronomical Station Vidojevica we have collected observations of these objects using two CCD cameras, Apogee Alta U42 and SBIG ST-10ME, attached to the 60 cm telescope. Its nominal focal length is 600 cm as given by the manufacturer. To determine the telescope focal length more precisely for both attached detectors, we used angular-separation measurements from CCD images taken at Astronomical Station Vidojevica. The obtained focal lengths are: F42 = (5989 ? 7) mm using the CCD camera Apogee Alta U42 attached to the telescope, and F10 = (5972 ? 4) mm with the CCD camera SBIG ST-10ME attached to the telescope.

Ground-Based Photometric Calibration of the Space Telescope CCD Camera

1989 ◽  
pp. 631-634
Author(s):  
D. A. Hunter ◽  
H. C. Harris ◽  
W. A. Baum ◽  
J. H. Jones ◽  
T. J. Kreidl
Keyword(s):  
Ccd Camera ◽  
Space Telescope ◽  
Photometric Calibration

Color correction against changes of light source in image acquisition by CCD camera

1999 ◽  
Author(s):  
Montserrat Corbalan-Fuertes ◽  
Maria S. Millan Garcia-Verela ◽  
Maria J. Yzuel
Keyword(s):  
Light Source ◽  
Image Acquisition ◽  
Ccd Camera ◽  
Color Correction

scholarly journals Astronomical station Vidojevica: In situ test of the ALTA Apogee U42 CCD camera

2012 ◽  
pp. 65-74
Author(s):  
O. Vince
Keyword(s):  
Ccd Camera ◽  
Astronomical Observatory ◽  
In Situ Test ◽  
Readout Noise ◽  
Astronomical Station

Currently, the CCD camera most used by observers of the Astronomical Observatory of Belgrade is the ALTA Apogee U42. It is used for both photometric and astrometric observations. Therefore, it is very important to know different measurable parameters which describe the condition of the camera - linearity, gain, readout noise etc. In this paper, we present a thorough test of this camera.

A Brightness and Color Correction Method of LED Display Based on CCD Camera

2012 ◽  
Vol 198-199 ◽  
pp. 1190-1195
Author(s):  
Zi Quan Zhao ◽  
Rui Guang Wang
Keyword(s):  
Linear System ◽  
Pulse Width ◽  
Ccd Camera ◽  
Correction Method ◽  
Color Correction ◽  
Gray Level ◽  
Correction Algorithm ◽  
Main Color ◽  
Color Components

The correction methods of LED displays are aiming to address the uniform issues which includes brightness aspect and color aspect. The correction method use a 3×3 correction coefficients matrix to reshape the pulse width of each LED.To calculate the correction coefficients, a linear system is established, which includes a color CCD and a LED display. And a correction algorithm is introduced based on the color CCD. This algorithm describes the relationships of the main color components of a LED, when the gray level of a LED is increasing or decreasing, the three main color components would change according to the correction coefficients. The results shows that the correction based on this algorithm improved the performance of LED displays.

scholarly journals Ground-Based Photometric Calibration of the Space Telescope CCD Camera

1989 ◽  
Vol 8 ◽  
pp. 631-634
Author(s):  
D.A. Hunter ◽  
H.C. Harris ◽  
W.A. Baum ◽  
J.H. Jones ◽  
T.J. Kreidl
Keyword(s):  
Hubble Space Telescope ◽  
Ccd Camera ◽  
Wide Field ◽  
Photometric System ◽  
Standard Star ◽  
Space Telescope ◽  
Ccd Imaging ◽  
Photometric Calibration ◽  
Imaging Instrument

The Wide-Field and Planetary Camera (WF/PC) is a CCD imaging instrument which is part of the Hubble Space Telescope. Ground-based observations have been made with a CCD system similar to those of the WF/PC in order to establish the standard star sequence to be used for in-flight photometric calibration. Because the WF/PC passbands differ from those in previous photometric use, the filters and CCDs will define a new photometric system. We outline here the procedures used to establish the calibration fields to be used in flight (see Harris et al. 1988 for additional details).

Brief summary of Kleť photographic search programme for minor planets

1999 ◽  
Vol 173 ◽  
pp. 189-192
Author(s):  
J. Tichá ◽  
M. Tichý ◽  
Z. Moravec
Keyword(s):  
Ccd Camera ◽  
Minor Planet ◽  
Minor Planets ◽  
Main Belt

AbstractA long-term photographic search programme for minor planets was begun at the Kleť Observatory at the end of seventies using a 0.63-m Maksutov telescope, but with insufficient respect for long-arc follow-up astrometry. More than two thousand provisional designations were given to new Kleť discoveries. Since 1993 targeted follow-up astrometry of Kleť candidates has been performed with a 0.57-m reflector equipped with a CCD camera, and reliable orbits for many previous Kleť discoveries have been determined. The photographic programme results in more than 350 numbered minor planets credited to Kleť, one of the world's most prolific discovery sites. Nearly 50 per cent of them were numbered as a consequence of CCD follow-up observations since 1994.This brief summary describes the results of this Kleť photographic minor planet survey between 1977 and 1996. The majority of the Kleť photographic discoveries are main belt asteroids, but two Amor type asteroids and one Trojan have been found.

Zero-loss omega-filtered REM and RHEED on the new Zeiss 912

1991 ◽  
Vol 49 ◽  
pp. 616-617
Author(s):  
J.C.H. Spence ◽  
J. Mayer
Keyword(s):  
Electron Microscopy ◽  
Materials Science ◽  
Surface States ◽  
Ccd Camera ◽  
Dark Field ◽  
Ion Pump ◽  
Magnetic Imaging ◽  
Reflection Electron Microscopy ◽  
Diffraction Patterns ◽  
Large Background

The Zeiss 912 is a new fully digital, side-entry, 120 Kv TEM/STEM instrument for materials science, fitted with an omega magnetic imaging energy filter. Pumping is by turbopump and ion pump. The magnetic imaging filter allows energy-filtered images or diffraction patterns to be recorded without scanning using efficient parallel (area) detection. The energy loss intensity distribution may also be displayed on the screen, and recorded by scanning it over the PMT supplied. If a CCD camera is fitted and suitable new software developed, “parallel ELS” recording results. For large fields of view, filtered images can be recorded much more efficiently than by Scanning Reflection Electron Microscopy, and the large background of inelastic scattering removed. We have therefore evaluated the 912 for REM and RHEED applications. Causes of streaking and resonance in RHEED patterns are being studied, and a more quantitative analysis of CBRED patterns may be possible. Dark field band-gap REM imaging of surface states may also be possible.

Automated electron tomography: from data collection to image processing

1995 ◽  
Vol 53 ◽  
pp. 26-27
Author(s):  
Weiping Liu ◽  
Jennifer Fung ◽  
W.J. de Ruijter ◽  
Hans Chen ◽  
John W. Sedat ◽  
...  
Keyword(s):  
Image Processing ◽  
Data Collection ◽  
Structural Information ◽  
Imaging Technique ◽  
Electron Tomography ◽  
Ccd Camera ◽  
Automated Data Collection ◽  
Full Control ◽  
Transmission Electron ◽  
Amorphous Structures

Electron tomography is a technique where many projections of an object are collected from the transmission electron microscope (TEM), and are then used to reconstruct the object in its entirety, allowing internal structure to be viewed. As vital as is the 3-D structural information and with no other 3-D imaging technique to compete in its resolution range, electron tomography of amorphous structures has been exercised only sporadically over the last ten years. Its general lack of popularity can be attributed to the tediousness of the entire process starting from the data collection, image processing for reconstruction, and extending to the 3-D image analysis. We have been investing effort to automate all aspects of electron tomography. Our systems of data collection and tomographic image processing will be briefly described.To date, we have developed a second generation automated data collection system based on an SGI workstation (Fig. 1) (The previous version used a micro VAX). The computer takes full control of the microscope operations with its graphical menu driven environment. This is made possible by the direct digital recording of images using the CCD camera.

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