By Brian Warner
Tools for beginner astronomers who desire to transcend CCD imaging and step into ‘serious’ technological know-how. The textual content deals recommendations for amassing, studying, and publishing facts, and describes joint initiatives within which amateurs and scholars can participate. Readers learn how to realize and steer clear of universal blunders in accumulating photometry facts, with distinct examples for research. contains studies of obtainable software program, with reveal photographs and worthy tips.
Read or Download A Practical Guide to Lightcurve Photometry and Analysis (Patrick Moore's Practical Astronomy Series) PDF
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Additional resources for A Practical Guide to Lightcurve Photometry and Analysis (Patrick Moore's Practical Astronomy Series)
4 Transforms and Nightly Zero-Points To convert raw instrumental magnitudes to a standard system requires that you determine the values, or transforms (also transformation values). These are applied to the raw instrumental magnitude for a given star (corrected for first and second-order extinction, if necessary) so that the derived standard magnitude for the star matches its catalog value. You must determine these values even if you’re using filters that supposedly match your system to the standard band.
Remember that any noise in the master flat becomes part of the final image. If you are shooting flats with filters and using the twilight sky for illumination, shoot the darker filters first so that you have the most light. Since most CCDs have a shutter of some sort, you must be careful not to take flats with too short of an exposure. Otherwise, the CCD chip will not be evenly illuminated over its entire surface. For example, if you have a camera with a four- The Photometry Primer 39 vane shutter that opens from the middle, expands out, and the collapses shut, the regions nearest the edge of the chip receive less exposure than the center of the chip.
The first involves carefully monitoring the position of the star and noting any “wobble” in the star’s position. The slight back and forth change in position is caused by one or more planets having sufficient mass so that the center of mass of the extra-solar system is measurably different from the physical center of the star. As the planets and sun move about the common center of mass, the star’s position shifts slightly. The amount of the wobble and any periodicity in that wobble help determine the number and masses of any planets.
A Practical Guide to Lightcurve Photometry and Analysis (Patrick Moore's Practical Astronomy Series) by Brian Warner