Preliminary Results from the Automated Patrol Telescope CCD Camera

1990 ◽  
Vol 8 (04) ◽  
pp. 377-380 ◽  
Author(s):  
P. W. Brooks
Keyword(s):  
Dark Current ◽  
Ccd Camera ◽  
Low Noise ◽  
Wide Field ◽  
Unique Combination ◽  
Schmidt Telescope ◽  
Charge Coupled Device ◽  
Analog To Digital ◽  
Correlated Double Sampling ◽  
The University

Abstract The University of NSW Automated Patrol Telescope (APT), a modified 0.5 m Baker-Nunn Schmidt telescope situated at Siding Spring Observatory, Coonabarabran, Australia, was opened in June 1989. It features the unique combination of an extremely fast (f/1) optical system with a CCD (Charge-Coupled Device) camera at the prime focus, capable of both fast (50 Hz TV-rate) imaging and slow-scan integrated readout via a low noise Correlated Double Sampling amplifier. This combination of optics and detector gives a wide field (0.9° × 1.4°) suited to observing extended objects including the LMC, SMC and galaxies in the Sculptor group. First images from the APT are presented along with the results of noise, linearity and dark current measurements made to date with a 12-bit analog-to-digital converter. Results were (ADU = Analog-Digital Unit):

A Peltier-cooled CCD Camera

1991 ◽  
Vol 9 (1) ◽  
pp. 158-159 ◽  
Author(s):  
B. D. Carter ◽  
M. C. B. Ashley
Keyword(s):  
Dark Current ◽  
Cooling System ◽  
Ccd Camera ◽  
Radiative Heating ◽  
Peltier Effect ◽  
Charge Coupled Device ◽  
Automated Imaging ◽  
Cooled Ccd ◽  
Ccd Detectors ◽  
Careful Design

AbstractWe describe the application of Peltier effect cooling to charge coupled device (CCD) detectors. We are developing this technique to produce a CCD camera which requires low maintenance, yet has sufficiently small dark-current for long exposure imaging. This camera will be used in an automated imaging telescope at Siding Spring Observatory. The design principles used to maximise cooling of the detector, and hence minimise dark-current, are discussed. A small dark-current can be obtained only if great care is taken to reduce or eliminate convective, conductive and radiative heating of the chip. In addition, a path of high thermal conductivity must be provided for the heat removed from the CCD. A recent laboratory test of our cooling system demonstrates that careful design can lead to sufficiently low CCD dark-current for many astronomical applications.

scholarly journals MOCAM: A 4k × 4k CCD Mosaic for the Canada-France-Hawaii Telescope Prime Focus

1995 ◽  
Vol 167 ◽  
pp. 213-220
Author(s):  
J. C. Cuillandre ◽  
Y. Melliers ◽  
R. Murowinski ◽  
D. Crampton ◽  
G. Luppino ◽  
...  
Keyword(s):  
Focal Plane ◽  
San Diego ◽  
Ccd Camera ◽  
Astronomical Observatory ◽  
Wide Field ◽  
On Line ◽  
Readout Noise ◽  
The University ◽  
Filter Wheel ◽  
Better Than

MOCAM is a wide field CCD camera, currently nearing completion, which will be offered to the Canada-France-Hawaii Telescope (CFHT) user community in 1995. The project is a collaboration between the CFHT, the Dominion Astronomical Observatory (DAO, Canada), the Institut des Sciences de l'Univers (INSU, France), Laboratoire d'Astrophysique de Toulouse (LAT, France) and the University of Hawaii (UH). In the interests of producing a reliable and effective camera in the shortest time, it was decided to use existing technologies rather than innovative ones. Two-edge buttable 2048 × 2048 15 μm pixel CCDs were obtained from the LORAL aerospace foundry, based on a mask designed by J. Geary at Smithsonian Astrophysical Observatory (SAO). They are mounted in a dewar designed by G. Luppino (UH); the focal plane mounting keeps the mosaic flat to within two pixels and the CCDs are aligned to within two pixels. A mechanical interface designed and fabricated by the DAO holds a 150 mm shutter and a filter wheel which has a positioning repeatability better than five μm.The four CCDs are operated in parallel by a San Diego GenIII controller adapted by LAT. The mosaic is read out in seven minutes and a single 33 Mb FITS file is generated to enable convenient on-line preprocessing. The user will control the system through a single CFHT Pegasus environment session. The camera field is 14′ × 14′ with a 0.″2 pixel sampling and the readout noise is less than seven electrons. The scientific goals of the initiators of the project are studies of distant clusters, deep galaxy counts and quasars surveys.

scholarly journals The Edinburgh Astronomy Teaching and Educational Packages

1990 ◽  
Vol 105 ◽  
pp. 124-138
Author(s):  
M.T. Brück ◽  
S.B. Tritton
Keyword(s):  
Teaching Material ◽  
Wide Field ◽  
The Sun ◽  
Visual Aids ◽  
Schmidt Telescope ◽  
Sky Survey ◽  
The Galaxy ◽  
University Of Edinburgh ◽  
The University ◽  
Low Dispersion

In this paper we describe our experiences with film copies of original astronomical photographs taken with the 1.2-meter U.K. Schmidt Telescope (UKST) in Australia, and used as teaching material in the Department of Astronomy of the University of Edinburgh. Two packages are intended for undergraduate use; the Education Packages are designed as visual aids for colleges, schools, and amateur groups.The original purpose of the telescope (which was commissioned in 1973) was to carry out a Southern Sky Survey to match the Northern Survey done by the Palomar 48” Schmidt Telescope. The telescope has a very wide field — 6.5 × 6.5 degrees, or equivalent to over a hundred and fifty full moons, and the photographs reach objects of 23rd magnitude: they record stars like the Sun to the very edges of the Galaxy and galaxies to a thousand million light years. Each photograph has an area of 356 × 356 mm and records between 100,000 and 1 million stars and galaxies. The survey photographs are the deepest available maps of the sky and are indispensable tools for astronomers in searches for unusual objects, for investigation of the distribution of galaxies and many other tasks. The UKST is equipped with objective prisms that are capable of producing low dispersion spectra of stars and galaxies. A prism of very small angle is placed in front of the aperture of the telescope so that each individual image is drawn out into a tiny spectrum on the photograph. The dispersion is very small, only a few millimeters from the red to the ultraviolet, but the dominant features in the spectra are recognizable and have many applications.

scholarly journals Asteroid Surveys and other CCD Projects Using the Observatoire de la Cote D’Azur (OCA) Schmidt Telescope

1995 ◽  
Vol 148 ◽  
pp. 38-43
Author(s):  
Alain Maury
Keyword(s):  
Ccd Camera ◽  
Wide Field ◽  
Schmidt Telescope ◽  
The Way

AbstractA wide field CCD camera has been developed for asteroid searches and has been used at our Schmidt telescope since September 1993. This paper describes this camera and its software as well as the changes it introduced in the type of programs that were requested on the telescope, and changes introduced in the way the telescope is operated.

scholarly journals Wide-field photothermal reflectance spectroscopy for single nanoparticle absorption spectrum analysis

Nanophotonics ◽  
2021 ◽  
Vol 10 (13) ◽  
pp. 3433-3440
Author(s):  
Jung-Dae Kim ◽  
Dong Uk Kim ◽  
Chan Bae Jeong ◽  
Ilkyu Han ◽  
Ji Yong Bae ◽  
...  
Keyword(s):  
Ccd Camera ◽  
Reflectance Spectroscopy ◽  
Wide Field ◽  
Spectroscopy Technique ◽  
Charge Coupled Device ◽  
Imaging Processing ◽  
Wide Field Of View ◽  
A Charge ◽  
20 Nm ◽  
Individual Nanoparticles

Abstract Photothermal imaging is useful for detecting individual nanoparticles and obtaining the absorption spectra. This study presents a wide-field photothermal reflectance spectroscopy technique achieved by incorporating a pump beam, a probe beam, and a charge-coupled device (CCD) camera into a commercial microscopic setup. The presented design does not require precise alignment between the pump and the probe beams and enables the observation of numerous individual nanoparticles during image acquisition. Despite the use of a simple imaging processing method, i.e., a four-bucket method using a CCD camera, sufficient sensitivity for the spectral imaging of a single gold nanorod (20 nm diameter and 84 nm length) is demonstrated. Numerous individual nanoparticles within a wide field of view (240 μm × 180 μm) are detected in an image captures at an imaging measurement speed of 0.02 mm2 min−1. Furthermore, the proposed photothermal reflectance spectroscopy technique can detect the variation in the absorption peak of the measured spectra depending on the aspect ratio of individual nanoparticles within a spectral resolution of 1 nm.

scholarly journals Spectroscopic flat-fields can be used for precision CCD gain and noise tests

2021 ◽  
Vol 38 ◽  
Author(s):  
J. Gordon Robertson
Keyword(s):  
Ccd Camera ◽  
Matched Pair ◽  
Optical Fibres ◽  
Charge Coupled Device ◽  
Small Areas ◽  
Flat Field ◽  
Basic Parameters ◽  
The Mean ◽  
A Charge ◽  
Analogue To Digital

Abstract One of the basic parameters of a charge coupled device (CCD) camera is its gain, that is, the number of detected electrons per output Analogue to Digital Unit (ADU). This is normally determined by finding the statistical variances from a series of flat-field exposures with nearly constant levels over substantial areas, and making use of the fact that photon (Poisson) noise has variance equal to the mean. However, when a CCD has been installed in a spectroscopic instrument fed by numerous optical fibres, or with an echelle format, it is no longer possible to obtain illumination that is constant over large areas. Instead of making do with selected small areas, it is shown here that the wide variation of signal level in a spectroscopic ‘flat-field’ can be used to obtain accurate values of the CCD gain, needing only a matched pair of exposures (that differ in their realisation of the noise). Once the gain is known, the CCD readout noise (in electrons) is easily found from a pair of bias frames. Spatial stability of the image in the two flat-fields is important, although correction of minor shifts is shown to be possible, at the expense of further analysis.

scholarly journals Experimental study of nonlinear characterization of hybrid SWCNTs/Ag-NPs fluids, using nonlinear diffraction technique

2018 ◽  
Vol 16 (36) ◽  
pp. 199-205
Author(s):  
Eman A A. Aboob
Keyword(s):  
Volume Fraction ◽  
Ccd Camera ◽  
Single Wall Carbon Nanotubes ◽  
Ag Nps ◽  
Charge Coupled Device ◽  
Nano Fluid ◽  
Nonlinear Characterization ◽  
Nonlinear Diffraction ◽  
Result Show

Based on nonlinear self- diffraction technique, the nonlinear optical properties of thin slice of matter can be obtained. Here, nonlinear characterization of nano-fluids consist of hybrid Single Wall Carbon Nanotubes and Silver Nanoparticles (SWCNTs/Ag-NPs) dispersed in acetone at volume fraction of 6x10-6, 9x10-6, 18x10-6 have been investigated experimentally. Therefore, CW DPSS laser at 473 nm focused into a quartz cuvette contains the previous nano-fluid was utilized. The number of diffraction ring patterns (N) has been counted using Charge - Coupled- Device (CCD) camera and Pc with a certain software, in order to find the maximum change of refractive index ( of fluids. Our result show that the fraction volume of 18x10-6 is more nonlinearity than others.

scholarly journals Observations of galaxies at z>6. The properties of large, spectroscopic samples

2006 ◽  
Vol 2 (14) ◽  
pp. 252-252
Author(s):  
Esther M. Hu ◽  
Lennox L. Cowie ◽  
Yuko Kakazu
Keyword(s):  
High Redshift ◽  
Broad Band ◽  
Ccd Camera ◽  
Far Infrared ◽  
Current Status ◽  
Wide Field ◽  
High Redshift Galaxies ◽  
Field Samples ◽  
Multi Wavelength ◽  
Redshift Galaxies

AbstractObserved properties of spectroscopically confirmed galaxies at z≫5 and z≫6 based on selection from deep, multi-wavelength wide-field samples provide a picture of the current status of the properties of high-redshift galaxies and their evolution to yet higher redshifts.In the current presentation, we use results of deep, wide-field spectroscopy with the multi-object Deimos spectrograph on Keck in combination with deep, wide-field multi-color imaging studies using the SuprimeCam CCD camera of Subaru for a number of fields, to evaluate the luminosity function of high-redshift galaxies and its evolution at z>6. High-redshift candidates are selected using both narrow-band Lyman alpha emission and broad-band colors with a high success-rate from a number of SuprimeCam (0.5 degree FOV) fields.Luminosity functions and Lymanα emission line profiles and equivalent widths appear similar between samples at z≃5.7 and z≃6.5, and the galaxy distribution is structured both spatially and in redshift. A large amount of cosmic variance is seen in the distribution of z≫6 galaxies from field to field.The observed properties are discussed in relationship to their impact on strategies for complementary optical surveys of high-redshift galaxies, and in relationship to surveys at very different wavelengths (X-ray, far-infrared, and submillimeter) that cover the same regions.

Observational Data and Orbits of the Asteroids Discovered at the Baldone Observatory in 2008–2013

2015 ◽  
Vol 24 (3) ◽  
Author(s):  
K. Černis ◽  
I. Wlodarczyk ◽  
I. Eglitis
Keyword(s):  
Observational Data ◽  
Ccd Camera ◽  
Minor Planet ◽  
Orbital Elements ◽  
Main Belt ◽  
Schmidt Telescope ◽  
Ccd Observations ◽  
Near Earth Objects ◽  
Asteroids And Comets

AbstractThe paper presents statistics of the asteroids observed and discovered at the Baldone Observatory, Latvia, in 2008–2013 within the project for astrometric observations of the near-Earth objects (NEOs), the main belt asteroids and comets. CCD observations of the asteroids were obtained with the 0.80/1.20 m, f/3 Schmidt telescope and a ST-10XME 15 × 10 mm CCD camera. In the Minor Planet Circulars and the Minor Planet Electronic Circulars (2008–2013) we published 3511 astrometric positions of 826 asteroids. Among them, 43 asteroids were newly discovered at Baldone. For 36 of these asteroids the precise orbits are calculated. Because of short observational arc and small number of observations, a few asteroids have low-precision orbits and their tracks have been lost. For seven objects with poorly known orbits we present their ephemerides for 2015–2016. The orbits and the evolution of orbital elements of two asteroids, (428694) 2008 OS9 from the Apollo group and the Centaur (330836) Orius (2009 HW77), are recalculated including new observations obtained after 2011.

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