Get A Practical Guide to Lightcurve Photometry and Analysis PDF

By Brian Warner

ISBN-10: 0387293655

ISBN-13: 9780387293653

Tools for beginner astronomers who desire to transcend CCD imaging and step into ‘serious’ technological know-how. The textual content deals concepts for amassing, reading, and publishing information, and describes joint initiatives within which amateurs and scholars can participate. Readers learn how to realize and steer clear of universal mistakes in amassing photometry information, with targeted examples for research. comprises experiences of obtainable software program, with display pictures and worthy tips.

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Read Online or Download A Practical Guide to Lightcurve Photometry and Analysis (Patrick Moore's Practical Astronomy Series) PDF

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Additional info for A Practical Guide to Lightcurve Photometry and Analysis (Patrick Moore's Practical Astronomy Series)

Sample text

Recall also that the number of electrons is found by multiplying the total of the ADU values by the gain, which is the number of electrons per ADU (e–/ADU). 1 Measuring a star. The object’s brightness and position are computed by using the sum of the values within the inner circle – the measuring aperture, less the average sky background times the number of pixels within the measuring aperture. , the sky annulus. Normalization is used so that values from images with different exposures can be compared directly.

The B band is centered on 4400 Å and the V band is centered at about 5500 Å. See Fig. 1. The reasons for selecting the regions for filters were not arbitrary, though some astronomers disagreed, and still do, with those reasons. The V filter approximates the photovisual magnitude system. The 1P21 and not the filter defines the cutoff in the red region. The B filter approximates the original photographic (blue) system. The filter for this band is actually consists of two filters. One is used to block light from shorter wavelengths and the Balmer discontinuity.

I’ve used this method at times when I didn’t have time to get twilight flats at the start of the run. The results have been very good. They are much better than no flats at all and serve well when doing differential photometry where there are no plans to convert to standard magnitudes. 11 Photometry Apertures and Annuluses When you click on a star in many photometry programs, two or more concentric regions appear that are centered on a star (see Fig. 1). The program may use circles, squares, allow one or the other, and even custom shapes.

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A Practical Guide to Lightcurve Photometry and Analysis (Patrick Moore's Practical Astronomy Series) by Brian Warner

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