Observational Window Functions in Planet Transit Searches
arXiv:0711.4256 · doi:10.1017/S1743921308016451
Abstract
Window functions describe, as a function of orbital period, the probability that an existing planetary transit is detectable in one's data for a given observing strategy. We show the dependence of this probability upon several strategy and astrophysical parameters, such as length of observing run, observing cadence, length of night, and transit duration. The ability to detect a transit is directly related to the intrinsic noise of the observations. In our simulations of the window function, we explicitly address non-correlated (gaussian or white) noise and correlated (red) noise and discuss how these two different noise components affect window functions in different manners.
arXiv comment8 pages, 6 figures; to appear in the Proceedings of the 249th IAU Meeting: "Exoplanets: Detection, Formation and Dynamics" (Suzhou, China); added referee's comments
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