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A Technique to Derive Improved Proper Motions for Kepler Objects of Interest

  • Authors: G. Fritz Benedict, Angelle M. Tanner, Phillip A. Cargile, and David R. Ciardi

Benedict et al. 2014 The Astronomical Journal 148 108.

  • Provider: AAS Journals

Caption: Figure 11.

x and y residuals in millipixels as a function of time from the full Schmidt 14 parameter modeling from Section 4.3. The residual clumps on the left-hand side (Channel 21) from left to right are "plates" 3–7. Stars are labeled with a running number from 1 to 97. Note the scale change along the y-axis, a range five times larger than that in Figure 9. The residuals exhibit extreme time dependence. Star 27 continues to show unmodeled behavior in both channels. Virtually all stars in Channel 37 (right) exhibit unmodeled behavior.

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