A Practical Guide to Lightcurve Photometry and Analysis by Brian D. Warner

By Brian D. Warner

A sensible advisor to Lightcurve Photometry and research presents, for
those with entry to even a modest telescope and CCD digital camera, all the
information had to participate in the medical research of asteroids and
variable stars.

Using commercially to be had apparatus, beginner astronomers can
determine the rotation price, measurement, and form of asteroids. equally, it
is attainable to find the scale, temperature, and orbits of stars in
binary structures through the use of this robust technique.

A sensible advisor to Lightcurve Photometry and research comprises all the
material wanted for readers to appreciate the idea, and keep away from the
practical pitfalls of lightcurve photometry. special examples are
given for acquiring information, and naturally for the interesting and rewarding
task of interpreting the information to figure out the actual houses of the

Any collage pupil or beginner astronomer who desires to transcend mere
imaging with a CCD digicam and input the demanding international of "real
science" through the lightcurves of asteroids and binary stars will find
everything valuable during this book.

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Extra resources for A Practical Guide to Lightcurve Photometry and Analysis

Example text

The centers for the two bands were 6500 Å and 8000 Å. The R and I magnitudes of the two systems are not the same, with the Cousins system now being the preferred one. You’ll often see Rc and Ic, which means Cousins RI magnitudes. 6 CCDs and Standard Magnitudes What should be apparent at this point is that the detector used to gather photons defines the system as much as the filters. If CCDs and the 1P21 had approximately the same spectral response, then the same filters used for traditional photoelectric photometry could be used on CCDs and the transformation from an instrumental system to a standard system would be fairly easy.

I’ve worked asteroids with SNRs well over 100 that generated lightcurves with data points loosely tied to the average curve while others, with SNRs of only 20–40, generated lightcurves that were smooth and had tightly fitting data points. 6 Seeing and Scintillation Seeing is a measurement of atmospheric turbulence. When there are large temperature differences between layers of air, the seeing is usually very poor, meaning – in simple terms – that the visible disc of a star is enlarged and so covers a greater number of pixels.

4. 1) 21 22 Photometry Fundamentals In the context of this book, B1 and B2 will be the electron counts for each object as derived from pixel values. 5? It accounts for the fact that the magnitude system is “upside down” and so more negative numbers represent brighter stars. 24 less than the fainter star. This is often confusing for the beginner, especially when describing a range of values. For example, when someone says that he observes objects 14th magnitude or less, does he mean brighter or fainter than 14th magnitude?

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