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Observational window functions in planet transit searches

Published online by Cambridge University Press:  01 October 2007

Kaspar von Braun  and
David R. Ciardi
Kaspar von Braun
Affiliation:
Michelson Science CenterCalifornia Institute of Technology770 South Wilson Ave. Pasadena, CA 91125, USA email: [email protected]; [email protected]
David R. Ciardi
Affiliation:
Michelson Science CenterCalifornia Institute of Technology770 South Wilson Ave. Pasadena, CA 91125, USA email: [email protected]; [email protected]
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Abstract

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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 (white) noise and correlated (red) noise and discuss how these two different noise components affect window functions in different manners.

Keywords

methods: statisticalplanetary systemstime
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 93 - 100
Copyright
Copyright © International Astronomical Union 2008

References

Aigrain, S. & Pont, F. 2007, MNRAS, 378, 741CrossRefGoogle Scholar
Kane, S. R., et al. 2007, ArXiv e-prints, 711, arXiv:0711.2581Google Scholar
Kovács, G., Bakos, G., & Noyes, R. W. 2005, MNRAS, 356, 557CrossRefGoogle Scholar
Mandel, K., & Agol, E. 2002, ApJL, 580, L171CrossRefGoogle Scholar
Mallén-Ornelas, G., Seager, S., Yee, H. K. C., Minniti, D., Gladders, M. D., Mallén-Fullerton, G. M., & Brown, T. M. 2003, ApJ, 582, 1123CrossRefGoogle Scholar
Pepper, J., & Gaudi, B. S. 2005, ApJ, 631, 581CrossRefGoogle Scholar
Pont, F. 2006, in “Tenth Anniversary of 51 Peg-b: Status of and prospects for hot Jupiter studies” (eds. Arnold, L., Bouchy, F., & Moutou, C.), p.153 (astro-ph/0612540)Google Scholar
Pont, F., Zucker, S., & Queloz, D. 2006, MNRAS, 373, 231CrossRefGoogle Scholar
Seager, S., & Mallén-Ornelas, G. 2003, ApJ, 585, 1038CrossRefGoogle Scholar
Tamuz, O., Mazeh, T., & Zucker, S. 2005, MNRAS, 356, 1466CrossRefGoogle Scholar
von Braun, K., Lee, B. L., Seager, S., Yee, H. K. C., Mallén-Ornelas, G., & Gladders, M. D. 2005, PASP, 117, 141CrossRefGoogle Scholar