By Brian Warner
Tools for newbie astronomers who desire to transcend CCD imaging and step into ‘serious’ technology. The textual content bargains suggestions for amassing, studying, and publishing info, and describes joint initiatives within which amateurs and scholars can participate. Readers learn how to realize and stay away from universal mistakes in amassing photometry facts, with specified examples for research. comprises experiences of accessible software program, with monitor photographs and invaluable tips.
Read or Download A Practical Guide to Lightcurve Photometry and Analysis (Patrick Moore's Practical Astronomy Series) PDF
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Extra info for A Practical Guide to Lightcurve Photometry and Analysis (Patrick Moore's Practical Astronomy Series)
The theory, creation, and use of bias frames are explained very thoroughly in some of the books listed in the Bibliography. , “thermal noise”. Cooling the chip reduces thermal noise by making the atoms move slower and so fewer collisions result in free electrons. Dark frames are usually taken at the same temperature and duration as the target image. For example, if you take a 1-minute image at –30°, then you would use a dark frame that was also 1-minute long at –30°. e. both images must have the same binning.
As the light from the star is spread over more pixels, the star’s profile becomes asymmetrical and dark current noise increases. The net result of all this is decreased precision and accuracy. When the seeing turns stars into “fuzzballs,” it’s best to find something else to do. Of course, that point is relative. Some observers give up on nights that others would consider superior. Scintillation is a slightly different phenomenon, caused by a star’s light arriving not as a single packet of light but several, each “imaged” by small cells in the Earth’s atmosphere.
This reduces errors caused by changing conditions. As you’ll see later, you don’t need to worry about using stars of similar color, though it’s good general practice to avoid stars that are extremely red or blue. The former are particularly troublesome throughout the reduction process, partly because they are often variable. Richard Miles has developed a variation of this method using blue–red star pairs culled from the Hipparcos catalog. org). It will not be discussed in detail here, but it is worth investigating.
A Practical Guide to Lightcurve Photometry and Analysis (Patrick Moore's Practical Astronomy Series) by Brian Warner