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Table 1

Details of the observations used for this work.

Program Date Mode N NDIT DIT CAM Strehl

H1 073.B-0084(A) 2004–06–12 H, W 30 1 30 S13 0.17
K1 083.B-0031(A) 2009–05–18 Ks, W 143 4 10 S13 0.27
K2 179.B-0261(A) 2007–04–03 Ks, Wr 70 2 15 S13 0.22
K3 086.C-0049(A) 2011–03–19 Ks, W 37 2 15 S13
L1 086.C-0049(A) 2011–03–17 Lp, W 26 150 0.2 L27

Notes.Mode denotes the wavelength filter (H/Ks/Lp band, with central wavelength in μm) and the type of observations (Wollaston polarimetry (W or Wr), the latter with a rotated FOV). N is the number of exposures that were taken with a given detector integration time (DIT). NDIT (in s) denotes the number of integrations that were averaged online by the read-out electronics during the observation. CAM indicates the camera optics used (S13 or L27). The Strehl ratio (if given) was measured using the strehl algorithm of the ESO eclipse package (Devillard 1997, publicly available at http://www.eso.org/projects/aot/eclipse/distrib/index.html), given here is the average value over all images in each dataset.

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