This article [J. Astron. Telesc. Instrum. Syst. 6(3), 035005 (Sep 24, 2020) DOI: 10.1117/1.JATIS.6.3.035005] as originally published omitted three authors as well as three references. The omitted... Show moreThis article [J. Astron. Telesc. Instrum. Syst. 6(3), 035005 (Sep 24, 2020) DOI: 10.1117/1.JATIS.6.3.035005] as originally published omitted three authors as well as three references. The omitted authors produced the Apodizing Phase Plate design used in the paper’s end-to-end simulations. This contribution was provided by David Doelman, Emiel Por, and Frans Snik, all of Leiden University. They have been added as authors on the paper, as listed above.The following acknowledgment also has been added to the published paper:“The research of DD and FS leading to these results has received funding from the European Research Council under ERC Starting Grant agreement 678194 (FALCONER).”Additionally, three references were omitted from the paper when it was published. They are listed below:61. G. Otten et al., “Performance characterization of a broadband vector Apodizing Phase Plate coronagraph,” Opt. Express 22(24), 30287 (2014).62. G. Otten et al., “The vector apodizing phase plate coronagraph: prototyping, characterization and outlook,” Proc. SPIE 9151, 91511R (2014).63. E. Por, “Optimal design of apodizing phase plate coronagraphs,” Proc. SPIE 10400, 104000V (2017).All versions of the article were corrected on 15 October 2020. The article appears correctly in print. Show less
Keppler, M.; Penzlin, A.; Benisty, M.; Boekel, R. van; Henning, T.; Holstein, R.G. van; ... ; Wildi, F. 2020
Context. A large portion of stars is found to be part of binary or higher-order multiple systems. The ubiquity of planets found around single stars raises the question of whether and how planets in... Show moreContext. A large portion of stars is found to be part of binary or higher-order multiple systems. The ubiquity of planets found around single stars raises the question of whether and how planets in binary systems form. Protoplanetary disks are the birthplaces of planets, and characterizing them is crucial in order to understand the planet formation process.Aims. Our goal is to characterize the morphology of the GG Tau A disk, one of the largest and most massive circumbinary disks. We also aim to trace evidence for binary-disk interactions.Methods. We obtained observations in polarized scattered light of GG Tau A using the SPHERE/IRDIS instrument in the H-band filter. We analyzed the observed disk morphology and substructures. We ran 2D hydrodynamical models to simulate the evolution of the circumbinary ring over the lifetime of the disk.Results. The disk and also the cavity and the inner region are highly structured, with several shadowed regions, spiral structures, and streamer-like filaments. Some of these are detected here for the first time. The streamer-like filaments appear to connect the outer ring with the northern arc. Their azimuthal spacing suggests that they may be generated through periodic perturbations by the binary, which tear off material from the inner edge of the outer disk once during each orbit. By comparing observations to hydrodynamical simulations, we find that the main features, in particular, the gap size, but also the spiral and streamer filaments, can be qualitatively explained by the gravitational interactions of a binary with a semimajor axis of similar to 35 au on an orbit coplanar with the circumbinary ring. Show less
Context. Young stars with debris disks are the most promising targets for an exoplanet search because debris indicate a successful formation of planetary bodies. Debris disks can be shaped by... Show moreContext. Young stars with debris disks are the most promising targets for an exoplanet search because debris indicate a successful formation of planetary bodies. Debris disks can be shaped by planets into ring structures that give valuable indications on the presence and location of planets in the disk.Aims. We performed observations of the Sco-Cen F star HD 117214 to search for planetary companions and to characterize the debris disk structure.Methods. HD 117214 was observed with the SPHERE subsystems IRDIS, IFS, and ZIMPOL at optical and near-IR wavelengths using angular and polarimetric differential imaging techniques. This provided the first images of scattered light from the debris disk with the highest spatial resolution of 25 mas and an inner working angle <0.1 ''. With the observations with IRDIS and IFS we derived detection limits for substellar companions. The geometrical parameters of the detected disk were constrained by fitting 3D models for the scattering of an optically thin dust disk. Investigating the possible origin of the disk gap, we introduced putative planets therein and modeled the planet-disk and planet-planet dynamical interactions. The obtained planetary architectures were compared with the detection limit curves.Results. The debris disk has an axisymmetric ring structure with a radius of 0.42(0.01)'' or similar to 45 au and an inclination of 71(+/- 2.5)degrees and exhibits a 0.4 '' (similar to 40 au) wide inner cavity. From the polarimetric data, we derive a polarized flux contrast for the disk of (F-pol)(disk)/F=(3.1 +/- 1.2)x10(-4) in the RI band.Conclusions. The fractional scattered polarized flux of the disk is eight times lower than the fractional IR flux excess. This ratio is similar to the one obtained for the debris disk HIP 79977, indicating that dust radiation properties are similar for these two disks. Inside the disk cavity we achieve high-sensitivity limits on planetary companions with a mass down to similar to 4 M-J at projected radial separations between 0.2 '' and 0.4 ''. We can exclude stellar companions at a radial separation larger than 75 mas from the star. Show less
