A Realistic Model for Point-sources Imaged on Array Detectors: The Model and Initial Results

Details A Realistic Model for Point-sources Imaged on Array Detectors: The Model and Initial Results A Realistic Model for Point-sources Imaged on Array Detectors: The Model and Initial Results

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995exa.....6..163m&link_type=abstract

Experimental Astronomy, Volume 6, Issue 1-2, pp. 163-210

Astronomy and Astrophysics

Astronomy

15

Ccds, Data Analysis, Instrumentation, Photometry, Software, Array Detectors

Scientific paper

We have constructed a computer model for simulation of point-sources imaged on two-dimensional detectors. An attempt has been made to ensure that the model produces “data” that mimic real data taken with 2-D detectors. To be realistic, such simulations must include randomly generated noise of the appropriate type from all sources (e.g. source, background, and detector). The model is generic and accepts input values for parameters such as pixel size, read noise, source magnitude, and sky brightness. Point-source profiles are then generated with noise and detector characteristics added via our model. The synthetic data are output as simple integrations (onedimensional), as radial slices (two-dimensional), and as intensity-contour plots (three-dimensional). Each noise source can be turned on or off so that they can be studied separately as well as in combination to yield a realistic view of an image. This paper presents the basic properties of the model and some examples of how it can be used to simulate the effects of changing image position, image scale, signal strength, noise characteristics, and data reduction procedures. Use of the model has allowed us to confirm and quantify three points: 1) The use of traditionalsize apertures for photometry of faint point-sources adds substantial noise to the measurement which can significantly degrade the quality of the observation; 2) The number of pixels used to estimate the background is important and must be considered when estimating errors; and 3) The “CCD equation” normally used by the astronomical community consistently overestimates the signal-to-noise obtainable by a measurement while a revised equation, discussed here, provides a better estimator.

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