Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/8515
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dc.contributor.authorWahhaj, Z-
dc.contributor.authorBenisty, M-
dc.contributor.authorGinski, C-
dc.contributor.authorSwastik, C-
dc.contributor.authorArora, S-
dc.contributor.authorvan Holstein, R. G-
dc.contributor.authorDe Rosa, R-
dc.contributor.authorYang, B-
dc.contributor.authorBae, J-
dc.contributor.authorRen, B-
dc.date.accessioned2024-08-22T05:16:59Z-
dc.date.available2024-08-22T05:16:59Z-
dc.date.issued2024-07-
dc.identifier.citationAstronomy & Astrophysics, Vol. 687, A257en_US
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/2248/8515-
dc.descriptionOpen Accessen_US
dc.descriptionOpen Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.-
dc.description.abstractContext. Most ground-based direct-imaging planet search campaigns use angular differential imaging that distorts the signal from extended sources, such as protoplanetary disks. In the case of the young system PDS 70, for which two planets were detected within the cavity of a protoplanetary disk, obtaining a reliable image of both planets and the disk is essential to understanding planet-disk interactions. Aims. Our goals are to reveal the true intensity of the planets and disk without self-subtraction effects for the first time, search for new giant planets beyond separations of 0.1″, and to study the morphology of the disk shaped by two massive planets. Methods. We present YJHK-band imaging, polarimetry, and spatially resolved spectroscopy of PDS 70 using near-simultaneous reference star differential imaging, also known as star-hopping. We created a radiative transfer model of the system to try to match the near-infrared imaging and polarimetric data within measurement errors. Sub-millimeter imaging data from ALMA were also modeled. Furthermore, we extracted the spectra of the planets and the disk and compared them Results. With strong constraints, we find that the disk is quite flared, with a scale height of ∼15 at the outer edge of the disk at ∼90 au, similar to some disks in the literature. The gap inside ∼50 au is estimated to have ∼1 of the dust density of the outer disk. The northeast outer disk arc seen in previous observations is likely the outer lip of the flared disk. Abundance ratios of sub-micron, micron, and grains estimated by the modeling indicate a shallow grain-size index greater than −2.7, instead of the canonical –3.5. There is both vertical and radial segregation of grains. Planet c is well separated from the disk and has a spectrum similar to planet b, and it is clearly redder than the disk spectra. Planet c is possibly associated with the sudden flaring of the disk starting at ∼50 au. We found no new planets in the system. If we assume DUSTY models and an age of 5 Myr, this indicates no new planets more massive than 5 outside a 12 au separation.en_US
dc.language.isoenen_US
dc.publisherEDP Sciencesen_US
dc.relation.urihttps://doi.org/10.1051/0004-6361/202349018-
dc.rights© The Authors 2024-
dc.subjectProtoplanetary disksen_US
dc.subjectCircumstellar matteren_US
dc.subjectPlanetary systemsen_US
dc.subjectStars: individual: PDS 70en_US
dc.subjectStars: pre-main sequenceen_US
dc.subjectStars: variables: T Tauri, Herbig Ae/Been_US
dc.titlePDS 70 unveiled by star-hopping: Total intensity, polarimetry, and millimeter imaging modeled in concerten_US
dc.typeArticleen_US
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