Research Article

A terrestrial planet in a ~1-AU orbit around one member of a ∼15-AU binary

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Science  04 Jul 2014:
Vol. 345, Issue 6192, pp. 46-49
DOI: 10.1126/science.1251527

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  1. Fig. 1 OGLE-2013-BLG-0341 light curve.

    (Top) Light-curve features (C to F), induced by main caustic due to binary, are seen as source passes close to planet host. The entrance has a sharp break (C) indicating a caustic crossing, whereas the exit does not (E and F), indicating a cusp exit. (Bottom left) Low-amplitude “bump” (A) due to source’s passage relatively far from binary companion to host, ∼300 days earlier. (Bottom right) “Dip” (B) due to planet “annihilating” one of the two main images of the source.

  2. Fig. 2 Geometry of OGLE-2013-BLG-0341 “wide minus” solution.

    (Bottom) Locations of the host (M*), planet (Mp) and companion (Mc), and of the caustics (closed curves of formally infinite magnification) that induce strong perturbations in the light curve. Source position is shown at six key times (A to F) corresponding to light-curve features in Fig. 1. (Middle) Zoom of planetary caustic (left) and central caustic (right), giving rise to “dip” and main peak seen in Fig. 1. Central caustic and lens positions are shown at two different epochs (“A” and “E”) separated by ∼300 days, during which it changed its shape and orientation due to binary orbital motion as described in the supplementary materials. (Top) Further zoom showing source (yellow) to scale. Blue and red caustics and circles indicate lens geometries at times of “bump” (A) and main peak (D), respectively. One unit on the x axis corresponds to tE = 33 days in time.

  3. Fig. 3 Full OGLE-2013-BLG-0341 light curve (top) and residuals from “wide minus” model with (middle) and without (bottom), including the parallax effect.

    Parallax is strongly detected, Δχ2 = 730. Silhouetted black and red curves indicate zero and difference between parallax and no-parallax models, respectively. In contrast to all other crucial light-curve parameters, the parallax effect is not directly visible in the light curve, but only in the residuals. However, as explained in the supplementary materials, an experienced modeler can “read off” from these residuals that πE >∼ 0.7.

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