All Figures

	Figure 1: Output difference image of Eri. The orthogonal line-shaped artifacts toward the edges of the image are due to the jittering, which shifts the field of view by a few arcseconds for each individual integration. In an unsaturated, undifferenced image, the PSF peak of Eri would here correspond to counts at a Strehl ratio of 85%. North is up and East is to the left in the image.
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In the text

	Figure 2: Image contrast achieved in the NB4.05 filter with the ADI technique. Solid line: the full combined data set. Dashed and dotted lines: the two individual observing runs before co-addition.
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In the text

	Figure 3: Six artificial companions at 3 significance, two each at separations of 1'', 2'', and 3''. The center of the image has been artificially set to zero to enhance visibility. North is up and East is to the left in the image.
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In the text

	Figure 4: Difference in performance between when ADI is used and when it is not. A positive number means that the contrast has increased when using ADI, for a single object signature.
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In the text

	Figure 5: Comparison of different high-contrast methods in terms of detectable mass of companions (in the simulated range of 1-10  ) to stars of ages 100 Myr ( upper panel), 320 Myr ( middle panel), and 1 Gyr ( lower panel), and of similar brightness to Eri. Solid line: 4.05 m with ADI. Dashed line: NACO-SDI with ADI. Dotted line: L'-band (assumed, see text) with ADI.
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In the text

	Figure 6: Detection limits for ages of (from top to bottom) 800 Myr, 600 Myr, 400 Myr, and 200 Myr. Also plotted is the mass corresponding to the linear RV trend (solid line increasing with separation) given the Eri x hypothesis as described in Sect. 5.5, and a vertical dotted line corresponding to the measured baseline of the trend. The dashed line is the minimum projected separation at .
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In the text

Figure 7: Detection probability as a function of semi-major axis, at an age of 200 Myr. Thick lines: for q=1 (solid line) and q=2 (dashed line). Thin lines: fraction of occurrences for a given semi-major axis that yield acceptable orbits, in the sense that the hypothetical planet could be consistent with the basic features of the RV trend (such as minimum baseline), for q=1 (solid line) and q=2 (dashed line).

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In the text

	Figure 8: Same as Fig. 7, but at an age of 800 Myr.
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In the text