The European Ultra-High Precision Stellar Photometry Road Map for Asteroseismology and Planet Finding

2006 ◽  
pp. 479-480
Author(s):  
Ian Roxburgh ◽  
Fabio Favata ◽  
Annie Baglin ◽  
Jørgen Christensen-Dalsgaard
Keyword(s):  
High Precision ◽  
Stellar Photometry ◽  
Road Map

scholarly journals High Precision Stellar Photometry by CCDs. II

1995 ◽  
Vol 167 ◽  
pp. 175-185
Author(s):  
Michael S. Bessell
Keyword(s):  
High Precision ◽  
Ccd Photometry ◽  
Stellar Photometry ◽  
Set Up ◽  
Good Range

CCD photometry is capable of high internal precision, however there are several important requirements necessary to attain high precision in standardized photometry. Firstly, the CCD passbands must match as closely as possible the standard passbands; secondly, new faint standards must be set up in several declination zones and thirdly, for convenience a sufficient number of standards covering a good range in color should be obtained on a single CCD frame so that several different frames should suffice for standardization. Landolt has taken the first steps in defining several such fields. The small systematic differences between different UBVRI systems have been examined and transformations can be applied to the photometry of Landolt and Bessell to place it on the Cape — SAAO system.

scholarly journals The Large-Field Bright-Star High-Precision CCD Photometer of BAO

1995 ◽  
Vol 167 ◽  
pp. 325-326
Author(s):  
Shiyang Jiang
Keyword(s):  
High Precision ◽  
Single Channel ◽  
High Accuracy ◽  
Bright Star ◽  
Large Field ◽  
Comparison Star ◽  
General Description ◽  
High Quantum Efficiency ◽  
Stellar Photometry ◽  
Long Time

Time-series high-accuracy photometry is very important for research in stellar variability. For a long time photometry made by a photomultiplier was the only instrument for high precision stellar photometry. To overcome the atmospheric variation and instrumental problems, we must choose at least one stable star as a comparison star and move the telescope quickly between the targets. So the real efficiency is very low and one only can do it on photometric nights. To overcome this limitation, since 1989 we began to cooperate with the team of the STEPHI network. We used the Chevreton four-channel photometer which can observe the variable, two comparison stars and a chosen sky background simultaneously. The multi-channel photometer is much better than normal single channel photometer as we can see from the several STEPHI results. Now the very high quantum efficiency CCD becomes more and more popular, so we are trying to change to use CCDs. Here we give some general description of a large field high accuracy bright star CCD photometer being prepared for the Beijing Astronomical Observatory (BAO).

COROT-high-precision stellar photometry on a low Earth orbit: solutions to minimize environmental perturbations

2003 ◽  
Author(s):  
Michel Auvergne ◽  
Laurent Boisnard ◽  
Jean-Tristan M. Buey ◽  
Gerard Epstein ◽  
Herve Hustaix ◽  
...  
Keyword(s):  
High Precision ◽  
Low Earth Orbit ◽  
Earth Orbit ◽  
Stellar Photometry ◽  
Environmental Perturbations

scholarly journals High Precision Stellar Photometry by CCDs. I

1995 ◽  
Vol 167 ◽  
pp. 173-173
Author(s):  
A. J. Penny
Keyword(s):  
High Precision ◽  
Percent Level ◽  
Systematic Errors ◽  
Uniform Illumination ◽  
Point Spread Functions ◽  
Stellar Photometry ◽  
The Third ◽  
Point Spread ◽  
Infra Red

This talk is about the limits to the precision of stellar photometry in comparing one star with another in a single CCD frame. This is concerned with bright stars, and concentrates on three problems at the 0.1 percent level of accuracy: how to flatfield; how to deal with varying point-spread-functions that vary across an image; how to deal with the fact that the response inside a pixel is not uniform. The first is the well-known difficulty of getting a uniform illumination across the CCD to use as a flatfield; the use of a rotatable CCD mounting and of drift-scanning is discussed. The second depends on the ability to detect and define small, but significant, changes in the PSF. The third is the fact that the pixels of optical CCDs can have non-uniformities inside them of ten percent, and these when folded with the PSF produce systematic errors significant at the 0.1 percent level; with infra-red arrays these problems can be much worse. The use of software to model these variations and reduce these errors is described.

scholarly journals A Neural Network for Monitoring and Characterization of Buildings with Environmental Quality Management, Part 1: Verification under Steady State Conditions

Energies ◽  
2020 ◽  
Vol 13 (13) ◽  
pp. 3469 ◽  
Author(s):  
Marek Dudzik ◽  
Anna Romanska-Zapala ◽  
Mark Bomberg
Keyword(s):  
Quality Management ◽  
High Precision ◽  
Environmental Quality ◽  
Initial Conditions ◽  
Integrated Control ◽  
Climatic Conditions ◽  
Transient Effects ◽  
Road Map ◽  
Precise Representation ◽  
Relative Errors

Introducing integrated, automatic control to buildings operating with the environmental quality management (EQM) system, we found that existing energy models are not suitable for use in integrated control systems as they poorly represent the real time, interacting, and transient effects that occur under field conditions. We needed another high-precision estimator for energy efficiency and indoor environment and to this end we examined artificial neural networks (ANNs). This paper presents a road map for design and evaluation of ANN-based estimators of the given performance aspect in a complex interacting environment. It demonstrates that in creating a precise representation of a mathematical relationship one must evaluate the stability and fitness under randomly changing initial conditions. It also shows that ANN systems designed in this manner may have a high precision in characterizing the response of the building exposed to the variable outdoor climatic conditions. The absolute value of the relative errors ( M a x A R E ) being less than 1.4% for each stage of the ANN development proves that our objective of monitoring and EQM characterization can be reached.

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