EDP Sciences
Free Access
Issue
A&A
Volume 578, June 2015
Article Number L9
Number of page(s) 5
Section Letters
DOI https://doi.org/10.1051/0004-6361/201526201
Published online 11 June 2015

Online material

thumbnail Fig. 3

Left: epochs of T Tau S around T Tau N. The coordinates are relative to T Tau N. Observations in which the Sa/Sb pair is not resolved are shown in either light grey or blue. The coloured markers show the resolved observations, in which the centre of mass was calculated from the position of Sa and Sb. The red line shows the orbit calculated by Köhler et al. (2008). The dark blue and green lines shows two possible orbital fits with the extreme periods of 2.7 × 104 and 475 years, respectively. Right: epochs of T Tau Sb around T Tau Sa. The coordinates are relative to T Tau Sa. The red line shows the orbit calculated by Schaefer et al. (2014).

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thumbnail Fig. 4

Detection limits of 3σ for point-like sources near T Tau N in the classical imaging IRDIS mode of VLT/SPHERE and Keck/NIRC2. The bumps in the SPHERE data at 250 and 600 mas are the wings of the PSF from T Tau N. The Keck/NIRC2 data is obtained from the Keck Observatory Archive, from projects identified as N26N2 for the H-band and 2010B for the K-band data.

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thumbnail Fig. 5

Extended emission south of T Tau Sa. Both T Tau Sa and Sb were subtracted using T Tau N as a PSF reference scaled to the peak of T Tau Sa and Sb, respectively. The leftover artefacts are due to the Airy rings apparent around all three components, which cannot be totally eliminated because of the closeness of T Tau Sa and Sb. The leftover residuals have an amplitude of 2.4% and 6.6% of the peak fluxes of T Tau Sa and Sb, respectively.

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© ESO, 2015

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