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dc.contributor.authorWillson, M
dc.contributor.authorKraus, S
dc.contributor.authorKluska, J
dc.contributor.authorMonnier, JD
dc.contributor.authorCure, M
dc.contributor.authorSitko, M
dc.contributor.authorAarnio, A
dc.contributor.authorIreland, MJ
dc.contributor.authorRizzuto, A
dc.contributor.authorHone, E
dc.contributor.authorKreplin, A
dc.contributor.authorAndrews, S
dc.contributor.authorCalvet, N
dc.contributor.authorEspaillat, C
dc.contributor.authorFukagawa, M
dc.contributor.authorHarries, TJ
dc.contributor.authorHinkley, S
dc.contributor.authorKanaan, S
dc.contributor.authorMuto, T
dc.contributor.authorWilner, DJ
dc.date.accessioned2018-11-05T14:37:16Z
dc.date.issued2018-11-08
dc.description.abstractContext. V1247 Orionis harbours a pre-transitional disc with a partially cleared gap. Earlier interferometric and polarimetric observations revealed strong asymmetries both in the gap region and in the outer disc. The presence of a companion was inferred to explain these asymmetric structures and the ongoing disc clearing. Aims. Using an extensive set of multi-wavelength and multi-epoch observations we aimed to identify the origin of the previously detected asymmetries. Methods. We observed V1247 Ori at three epochs spanning ∼ 678 days using sparse aperture masking interferometry with Keck/NIRC2 and VLT/NACO. In addition, we search for signs of accretion through VLT/SPHERE-ZIMPOL spectral differential imaging in Hα and R-band continuum. Our SMA sub-millimetre interferometry in 880 µm continuum and in the CO(3-2) line allows us to constrain the orientation and direction of rotation of the outer disc. Results. We find the L’-band emission to be dominated by static features which trace forward-scattered dust emission from the inner edge of the outer disc located to the north-east. In H- and K-band, we see evidence for a companion candidate that moved systematically by 45◦ within the first ∼345 days. The separation of the companion candidate is not well constrained, but the observed position angle change is consistent with Keplerian motion of a body located on a 6 au orbit. From the SMA CO moment map, the location of the disc rim, and the detected orbital motion, we deduced the 3-dimensional orientation of the disc. We see no indication of accretion in Hα and set upper limits for an accreting companion. Conclusions. The measured contrast of the companion candidate in H and K is consistent with an actively accreting protoplanet. Hence, we identify V1247 Ori as a unique laboratory for studying companion-disc interactions and disc clearing.en_GB
dc.description.sponsorshipWe acknowledge support from an ERC Starting Grant (Grant Agreement No. 639889), STFC Rutherford Fellowship Article number, page 14 of 17 M. Willson et al.: Imaging the disc rim and companion candidate in V1247 Ori (ST/J004030/1), STFC Rutherford Grant (ST/K003445/1), Marie SklodowskaCurie CIG grant (Ref. 618910), and Philip Leverhulme Prize (PLP-2013-110). We additionally acknowledge support from NASA KPDA grants (JPL-1452321, 1474717, 1485953, 1496788). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. J. Kluska acknowledges support from the research council of the KU Leuven under grant number C14/17/082. M. Curé and S. Kanaan acknowledge financial support from Centro de Astrofísica de Valparaiso. S. Kanaan thank the support of Fondecyt iniciacíon grant No. 11130702. T. Muto is partially supported by JSPS KAKENHI grant No. 26800106.en_GB
dc.identifier.citationPublished online 08 November 2018.en_GB
dc.identifier.doi10.1051/0004-6361/201630215
dc.identifier.urihttp://hdl.handle.net/10871/34645
dc.language.isoenen_GB
dc.publisherEDP Sciencesen_GB
dc.rights© ESO 2018.
dc.subjectPlanetary systemsen_GB
dc.subjectPlanets and satellites: formationen_GB
dc.subjectPlanets and satellites: detectionen_GB
dc.subjectProtoplanetary discsen_GB
dc.subjectStars: pre-main sequenceen_GB
dc.subjectStars: individual (V1247 Orionis)en_GB
dc.subjectInfrared: planetary systemsen_GB
dc.titleImaging the disc rim and a moving close-in companion candidate in the pre-transitional disc of V1247 Orionisen_GB
dc.typeArticleen_GB
dc.identifier.issn0004-6361
dc.descriptionThis is the author accepted manuscript. The final version is available from EDP Sciences via the DOI in this record.en_GB
dc.identifier.journalAstronomy and Astrophysicsen_GB


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